Author name code: koutchmy ADS astronomy entries on 2022-09-14 author:"Koutchmy, Serge L." ------------------------------------------------------------------------ Title: Refraction and scattering in the atmosphere of the planet Venus: The Lomonossov arc Authors: Koutchmy, Serge Bibcode: 2022arXiv220706760K Altcode: The main observations of 1761 by M. Lomonossov and those that followed are recalled by extending the discussion to other remarkable visual observations of the passages, then with more and more powerful imagers producing images in profusion. The modern treatment of parasitic effects is briefly recalled by focusing on the expert observation of 1761 which has recently been widely commented on and criticized. It included a spurious effect called the "black drop effect". The shell or aureole or atmospheric ring of Venus observed outside the solar disk is considered with reference to the today parameters of the Venus atmosphere. The contacts during the transit are discussed taking into account effects of scattering, absorption and the dominant effects of the refraction at the small angular distances found to be comparable to a fraction of the angular dimension of the planet. Modern observations of the 2004 and the 2012 transit are tentatively discussed to elucidate what is the arc of Lomonossov? Title: Polarimetric Studies of a Fast Coronal Mass Ejection Authors: Mierla, Marilena; Inhester, Bernd; Zhukov, Andrei N.; Shestov, Sergei V.; Bemporad, Alessandro; Lamy, Philippe; Koutchmy, Serge Bibcode: 2022SoPh..297...78M Altcode: 2022arXiv220604411M In this work we performed a polarimetric study of a fast and wide coronal mass ejection (CME) observed on 12 July 2012 by the COR1 and COR2 instruments onboard the Solar TErrestrial RElations Observatory (STEREO) mission. The CME source region was an X1.4 flare located at approximately S15W01 on the solar disk, as observed from the Earth's perspective. The position of the CME as derived from the 3D Graduated Cylindrical Shell (GCS) reconstruction method was at around S18W00 at 2.5 solar radii and S07W00 at 5.7 solar radii, meaning that the CME was deflected towards the Equator while propagating outward in the corona. The projected speed of the leading edge of the CME also evolved from around 200 km s−1 in the lower corona to around 1000 km s−1 in the COR2 field of view. The degree of polarisation of the CME is around 65% but it can go as high as 80% in some CME regions. The CME showed deviation of the polarisation angle from the tangential in the range of 10 - 15∘ (or more). Our analysis showed that this is mostly due to the fact that the sequence of three polarised images from where the polarised parameters are derived is not taken simultaneously, but at a difference of a few seconds in time. In this interval of time, the CME moves by at least two pixels in the FOV of the instruments and this displacement results in uncertainties in the polarisation parameters (degree of polarisation, polarisation angle, etc.). We propose some steps forward to improve the derivation of the polarisation. This study is important for analysing the future data from instruments with polarisation capabilities. Title: Polar regions activity and the prediction of the height of the solar cycle 25 Authors: Koutchmy, S.; Filippov, B.; Tavabi, E.; Noens, J-C.; Wurmser, O. Bibcode: 2022arXiv220509089K Altcode: The forthcoming solar cycle (SC) 25 was beleived to be rather low when using the sunspot number (SN) as a measurement of the level of activity. The most popular prediction was made by the panel of NASA in 2019, including works based on extrapolations of dynamo-type models. We however discovered that using different observations to measure the level of polar regions activity several years before the start of SC25 and also after the start of the SC25 in 2020, the height of the SC25 could be high. The polar regions activity we considered seems related to the polar coronal holes (CH) activity and it is found significantly higher before the SC25 that it was before the SC24 and accordingly, we suggest that the SN cycle could indeed be much higher than during the SC24 that was a low SN height cycle. Title: Predicting the height of the solar cycle 25 through polar regions activity Authors: Koutchmy, S.; Tavabi, E.; Noëns, J. -C.; Wurmser, O.; Filippov, B. Bibcode: 2021sf2a.conf..238K Altcode: We describe and discuss the reasons why we believe the forthcoming solar cycle (SC) 25 will be significantly higher than what was predicted by NASA in 2019. Title: Polarimetric Coronagraphy to record the initiation of CMEs Authors: Koutchmy, S.; Sèvre, F.; Rochain, S.; Noëns, J. -C.; Pitout, F. Bibcode: 2021sf2a.conf..298K Altcode: A new type of polarimetric coronagraph is proposed for permitting citizen Astronomers and Amateurs involved in $H\alpha$ and coronal observations using the Pic du Midi (PdM) Observatory Facilities (so-called CLIMSO) to apprehend and analyze the dynamical processes inside the solar corona. It includes relevant for economic reasons observations of the initiation phase of Coronal Mass Ejections (CMEs) and of recurrent geo-active quasi-polar coronal holes (CHs). Title: Solar Total Eclipse of 21 August 2017: Study of the Inner Corona Dynamical Events Leading to a CME Authors: Filippov, Boris; Koutchmy, Serge; Lefaudeux, Nicolas Bibcode: 2020SoPh..295...24F Altcode: 2020arXiv200110203F Total solar eclipse (TSE) coronal large- and small-scale events were reported in the historical literature but a definite synoptic coverage was missing for studying a relationship with the more general magnetic context of the solar-disk. We here analyze temporal changes in the solar corona before, during, and after the total solar eclipse on 21 August 2017 from a set of ground-based and of space-borne observations. High-quality ground-based white-light (W-L) observations and a deep image processing allow us to reveal these changes for the first time with a fraction of a minute temporal resolution. Displacements of a number of fine coronal features were measured for the first time at these small radial distances, using a diffraction-limited instrument at a single site. The comparison with space-based observations, including observations from the Solar Terrestrial Relations Observatory (STEREO) mission, showed that the features belong to a slow coronal mass ejection (CME) propagating through the corona with the nearly constant speed of 250 km s−1. Our TSE images provide the same typical velocity as measured at a distance of one solar radius from the surface. The event was initiated by coronal dynamics manifested by a prominence eruption that started just before the eclipse observations and an ascent of a U-shaped structure visible in the Atmospheric Imaging Assembly (AIA) 171 Å channel, which we assume as the lower part of a coronal cavity. The prominence material was observed draining down towards the chromosphere along the prominence arch. While the prominence disappears in the STEREO-A field-of-view at the height of about 6' above the limb, the corresponding flux rope seems to continue towards the outer corona and produces the slow CME with turbulent motion. The overall mass of the moving features is evaluated based on absolute photometrical data extracted from our best W-L eclipse image. Title: Total solar eclipse 2017 in USA: deep coronal spectra Authors: Koutchmy, S.; Baudin, F.; Abdi, Sh.; Golub, L.; Sèvre, F. Bibcode: 2019sf2a.conf..363K Altcode: Total eclipses permit a deep analysis of both the inner and the outer parts of the solar corona using the Thomson scattered (inverse Compton effect on free electrons at millions degrees T^{\circ} ) continuum White- Light (W-L) radiations and the spectrum of forbidden emission lines from hot highly ionized ions of iron, nickel, argon, etc. Spectra are largely affected by the superposition of the solar light scattered and diffracted by the interplanetary dust particles orbiting the Sun at large distances but intercepted along the line of sight (los)\citep{1973ApJ...186..671K}. Sometimes the parasitic light due to multiple scattering from the ground and from the Earth atmosphere should be removed using the light observed on the Moon image background. After sufficiently dispersing the W-L corona, the Fraunhofer (F) spectrum of the dust corona appears with its absorption (dark) lines of known equivalent widths and the continuum Thomson radiation can be extracted. The identified emission (bright) lines of ions with different degrees of ionization are studied to permit an evaluation of i/ relative abundances (compared to photospheric abundances), ii/ temperatures, iii/ non-thermal velocities and the resulting from the analysis of the departures from a Gaussian profile of net Doppler shifts after integration along the los. 60 spectra were obtained during the totality using a specially designed slit spectroscopic experiment for providing an accurate analysis of the most typical "broadly averaged" parts of the quasi-minimum of activity type corona. With the scanning +/- 3 solar radii long slit a .072 nm FWHM effective resolution was obtained in the range of 510 to 590 nm. The background sky was exceptionally clear during this US total eclipse of Aug. 21, 2017 as observed from our site in Idaho; spectra are without significant parasitic light on the Moon disk. The K+F continuum corona is well exposed up to at least 1 solar radius (Rs) from the limb and further out with a lower S/N ratio, showing several forbidden coronal emission lines. The F-corona can be measured even at the solar limb where its intensity reached near 6\% of the K-corona intensity. Streamers, active region enhancements and polar coronal holes (CHs) are well measured on each 1 sec exposure time coronal spectra see Fig. \ref{author1:fig1}; the 2^{nd} contact showing the chromospheric and the most inner layers emission lines was observed with a fast sequence and exposure time 10 times shorter. New weak emission lines were also discovered and/or confirmed see Fig. \ref{author1:fig2} ; their identifications are proposed. The rarely observed high FIP ArX \citep{2018ApJ...852...52D} line is recorded almost everywhere and a new nearby FeX line is well identified; the classical low FIP FeXIV and NiXIII lines are well recorded everywhere without over-exposure. For the 1st time hot lines are also measured at low levels inside the CH regions, at both poles. The radial variations of the corrected non-thermal turbulent velocities of the lines do not show a great departure from the average values. No significantly large Doppler shifts are seen nowhere in the inner and the middle corona although the whole corona is almost covered.\citep{Koutchmy} The corona is confirmed to be made of a mixing of hot and less hot components everywhere around the Sun, due to the yet unidentified magnetic origin heating processes reflected in our spectra and in the line profiles. Coronal density variations are well reflected by the K-corona continuum intensity variations the azimuthal and radial direction variations will permit the interpretation of the emission measures to be compared with the simultaneously obtained AIA images from the SDO space mission. The W-L images taken simultaneously shows a much better spatial resolution with images of bright background well known stars that permit to deduce an excellent absolute calibration needed to deduce the electron densities and to check our F-corona model, see \ref{author1:fig3}. Title: Eclipse 2017: new results on the dynamical inner-corona Authors: Koutchmy, S.; Filippov, B.; Lecleire, J. M.; Lefaudeux, N.; Mouette, J.; Sèvre, F.; Tavabi, E.; Viladrich, Ch.; Abdi, Sh. Bibcode: 2019sf2a.conf..361K Altcode: The total solar eclipse of 21 Aug. 2017 was observed by our teams in excellent conditions for almost 1 hour (from Oregon at 17h12, Idaho 17h27, see Fig. 1, Wyoming 17h36 and Missouri, 18h12 U.T.). Excellent images were recorded in white-light (W-L), including a very high spatial-temporal resolution (HR) sequence covering faint dynamical phenomena related to an exceptionally slow CME that evolved over the E-limb. In addition: i) The overall polarized K-corona, from linearly polarized images taken in 12 positions with a green filter, was analyzed, to be compared to the latest quantitative magnetic dynamical coronal modeling of the Mikic team \citep{mikic2018predicting}. The complex fine scale structure reflecting the magnetic field topology is analyzed using specially designed algorithms with suggestion of a more turbulent field in the outer corona above r= 2Rs. ii) The more simple Polar- cap Regions are considered to compare the impressive fine- scale more linear W-L plumes with the EUV plumes simultaneously observed in the lower corona with the AIA filtergrams of the SDO mission; we integrate 60 successive AIA images taken with the 171, 193, 211 Å filters to improve the S/N ratio of EUV frames. The new view of dynamical polar plumes is illustrated at different temperature regimes, including a high temperature regime. Some evidence of fast propagating transverse waves is obtained by comparing deep spatially Fourier- filtered W-L images of plumes and jets separated by typically 1 min of time; amplitudes are larger for larger radial distances, suggesting that they reflect the propagation of alfvenic disturbances and possibly their dissipation. iii) The most notable dynamic phenomenon is analyzed at the E- limb: it is a slow CME that shows a constant 250 km/s velocity from the LASCO (SoHO) observations. It is analyzed here in W-L with HR eclipse images and with images from the SECCHI EUV filtergrams of the STEREO mission and from the AIA of the SDO mission. Very small scale and faint moving and curved W-L features at r= 1.7 Rs, possibly owning to high disrupted loops, are analyzed for the 1st time with a 20 sec temporal resolution movie; falling back remnants of the erupted high latitude polar crown filament- prominence found at the feet of the CME are detected in W-L, well after the eruption. It is suggested that such processes are a component of the slow wind that is more easily demonstrated at time of this minimum corona using eclipse images in the r = 1.5 to 2 Rs region where instabilities grow and outwardly propagate.( \citet{1997Kout} \citet{2018Tavabi}) Title: New deep coronal spectra from the 2017 total solar eclipse Authors: Koutchmy, S.; Baudin, F.; Abdi, Sh.; Golub, L.; Sèvre, F. Bibcode: 2019A&A...632A..86K Altcode: 2019arXiv191001372K Context. The origin of the high temperature of the solar corona, in both the inner bright parts and the more outer parts showing flows toward the solar wind, is not understood well yet. Total eclipses permit a deep analysis of both the inner and the outer parts of the corona using the continuum white-light (W-L) radiations from electrons (K-corona), the superposed spectrum of forbidden emission lines from ions (E-corona), and the dust component with F-lines (F-corona).
Aims: By sufficiently dispersing the W-L spectrum, the Fraunhofer (F) spectrum of the dust component of the corona appears and the continuum Thomson radiation can be evaluated. The superposed emission lines of ions with different degrees of ionization are studied to allow the measurement of temperatures, non-thermal velocities, Doppler shifts, and abundances to constrain the proposed heating mechanisms and understand the origin of flows that lead to solar wind.
Methods: We describe a slit spectroscopic experiment of high spectral resolution to provide an analysis of the most typical parts of the quasi-minimum type corona observed during the total solar eclipse of Aug. 21, 2017 from Idaho, USA. Streamers, active region enhancements, and polar coronal holes (CHs) are measured well using deep spectra.
Results: Sixty spectra are obtained during the totality with a long slit, covering ±3 solar radii in the range of 510 nm to 590 nm. The K+F continuum corona is exposed well up to two solar radii. The F-corona can be measured even at the solar limb. New weak emission lines were discovered or confirmed. The rarely observed Ar X line is detected almost everywhere; the Fe XIV and Ni XIII lines are clearly detected everywhere. For the first time hot lines are also measured inside the CH regions. The radial variations of the non-thermal turbulent velocities of the lines do not show a great departure from the average values. No significantly large Doppler shifts are seen anywhere in the inner or the middle corona. The wings of the Fe XIV line show some non-Gaussianity.
Conclusions: Deep slit coronal spectra offered an opportunity for diagnosing several aspects of coronal physics during a well observed total eclipse without extended investments. The analysis of the ionic emission line profiles offers several powerful diagnostics of the coronal dynamics; the precise measurement of the F-continuum component provides insight into the ubiquitous dust corona at the solar limb. Title: Pointing the NTT at the Sun: Studying the Solar Corona During the Total Eclipse Authors: Dennefeld, M.; Koutchmy, S.; Sèvre, F.; Fathivavsari, H.; Auchère, F.; Baudin, F.; Abdi, S.; Sinclaire, P.; Saviane, I.; Labraña, F.; Schmidtobreick, L. Bibcode: 2019Msngr.177...54D Altcode: No abstract at ADS Title: Chromospheric Peculiar Off-limb Dynamical Events from IRIS Observations Authors: Tavabi, E.; Koutchmy, S. Bibcode: 2019ApJ...883...41T Altcode: 2019arXiv190710960T To study motions and oscillations in the solar chromosphere and at the transition region level we analyze some extreme Doppler shifts observed off-limb with the Interface Region Imaging Spectrograph (IRIS). Raster scans and slit-jaw imaging observations performed in the near-ultraviolet channels were used. Large transverse oscillations are revealed by the far wings profiles after accurately removing the bulk average line profiles of each sequence. Different regions around the Sun are considered. Accordingly, the cool material of spicules is observed in Mg II lines rather dispersed up to coronal heights. In the quiet Sun and especially in a polar coronal hole, we study dynamical properties of the dispersed spicules-material off-limb using high spectral, temporal, and spatial resolutions IRIS observations. We suggest that numerous small-scale jet-like spicules show rapid twisting and swaying motions evidenced by the large distortion and dispersion of the line profiles, including impressive periodic Doppler shifts. Most of these events repeatedly appear in red and blueshifts above the limb throughout the whole interval of the observation data sets, with an average swaying speed of order ±35 km s-1 reaching a maximum value of 50 km s-1 in the polar coronal hole region, well above the 2.2 Mm heights. We identified for the first time waves with a short period of order of 100 s, and less and transverse amplitudes of order of ±20-30 km s-1 with the definite signature of Alfvén waves. No correlation exists between brightness and Doppler shift variations; the phase speed of the wave is very large and cannot definitely be determined from the spectral features seen along the quasi-radial features. Even shorter periods waves are evidenced, although their contrast is greatly attenuated by the overlapping effects along the line of sight. Title: Atmospheric Emission Layers according to Photographic Observations from the International Space Station Authors: Platov, Yu. V.; Koutchmy, S.; Nikolayshvili, S. Sh. Bibcode: 2019Ge&Ae..59..351P Altcode: No abstract at ADS Title: Polar Coronal Plumes as Tornado-like Jets Authors: Tavabi, E.; Koutchmy, S.; Golub, L. Bibcode: 2018ApJ...866...35T Altcode: 2018arXiv180807322T We examine the dynamical behavior of white-light polar-plume structures in the inner corona that are observed from the ground during total solar eclipses, based on their extreme ultraviolet (EUV) hot and cool emission line counterparts observed from space. EUV observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) of a sequence of rapidly varying coronal hole structures are analyzed. Evidence of events showing acceleration in the 1.25 Mk line of Fe XII at 193 Å is given. The structures along the plume show an outward velocity of about 140 km s-1 that can be interpreted as an upward propagating wave in the 304 Å and 171 Å lines; higher speeds are seen in 193 Å (up to 1000 km s-1). The ejection of the cold He II plasma is delayed by about 4 minutes in the lowest layer and is delayed more than 12 minutes in the highest level compared to the hot 193 Å behavior. A study of the dynamics using time-slice diagrams reveals that a large amount of fast ejected material originates from below the plume, at the footpoints. The release of plasma material appears to come from a cylinder with quasi-parallel edge-enhanced walls. After the initial phase of a longitudinal acceleration, the speed substantially reduces, and the ejecta disperse into the environment. Finally, the detailed temporal and spatial relationships between the cool and hot components were studied with simultaneous multiwavelength observations, using more AIA data. The outward-propagating perturbation of the presumably magnetic walls of polar plumes supports the suggestion that Alfvén waves propagate outwardly along these radially extended walls. Title: Evidence of cool prominence material embedded in CMEs from polarization measurements Authors: Lamy, Philippe; Floyd, Olivier; Koutchmy, Serge Bibcode: 2018cosp...42E1930L Altcode: In white-light coronagraph images, cool prominence material is sometimes observed as bright substructures or plasmoids in coronal mass ejections (CMEs). Based on observations of a CME with the SECCHI/STEREO coronagraphs on 31 August 2007, Mierla et al. (2011) have shown that the emission from such bright patches is characterized by very low polarization and was due to H-alpha radiation from cool prominence material. We have examined several polarization images of CMEs obtained with the LASCO-C2 coronagraph with its orange filter. This filter is approximately centered on the HeI D3 line. This low excitation line emission is superior to the H-alpha emission of HI because its FIP is much higher. In several cases, we observe very low-polarization components embedded in CMEs characterized by a much larger polarization resulting from the Thomson scattering. They most likely present evidence of cool prominence material carried by the CMEs. Title: Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO Authors: Koutchmy, S.; Tavabi, E.; Urtado, O. Bibcode: 2018MNRAS.478.1265K Altcode: 2018MNRAS.tmp.1151K; 2018arXiv180504930K A shower of secondary cosmic ray (CR) particles is produced at high altitudes in the Earth's atmosphere, so the primordial galactic cosmic rays (GCRs) are never directly measured outside the Earth magnetosphere and atmosphere. They approach the Earth and other planets in the complex pattern of rigidity's dependence, generally excluded by the magnetosphere. GCRs revealed by images of single nuclear reactions also called spallation events are described here. Such an event was seen on 2015 November 29 using a unique Large Angle and Spectrometric Coronagraphs C3 space coronagraph routine image taken during the Solar and Heliospheric Observatory (SoHO) mission observing uninterruptedly at the Lagrangian L1 point. The spallation signature of a GCR identified well outside the Earth's magnetosphere is obtained for the first time. The resulting image includes different diverging linear `tracks' of varying intensity, leading to a single pixel; this frame identifies the site on the silicon CCD chip of the coronagraph camera. There was no solar flare reported at that time, nor coronal mass ejection and no evidence of optical debris around the spacecraft. More examples of smaller CR events have been discovered through the 20 yr of continuous observations from SoHO. This is the first spallation event from a CR, recorded outside the Earth's magnetosphere. We evaluate the probable energy of these events suggesting a plausible galactic source. Title: Proper Motions of Sunspots’ Umbral Dots at High Temporal and Spatial Resolution Authors: Goodarzi, Hadis; Koutchmy, Serge; Adjabshirizadeh, Ali Bibcode: 2018ApJ...860..168G Altcode: 2018arXiv180705531G To deepen the analysis of the photometric properties of the umbra of a sunspot, we study proper motions of small features such as umbral dots (UDs) inside a single sunspot observed by the Solar Optical Telescope of Hinode close to the disk center. We consider horizontal flows with high precision and details to study the transient motion behavior of UDs in short time intervals. Blue continuum images were first deconvolved with the point-spread function, such that the stray light is precisely removed and the original resolution is improved. Several images were co-added to improve the signal-to-noise ratio, keeping a reasonable temporal resolution and checking that the results are reproducible. The Fourier local correlation tracking technique is applied to the new corrected time sequence of images, and horizontal velocity maps were obtained both for the whole umbra (16″ × 12″) and for a high-resolution small region of the umbra (3.″5 × 3.″5) to study the smallest details of the velocity fields. We used two different Gaussian tracking windows (0.8 and 0.″2 ), which reveals two types of horizontal motions for umbral features. First, a global inner penumbra and peripheral umbra inward motion directed to the central parts is revealed as an overall proper motion of bright peripheral fine structures. Second, motions matching small cells inside the darkest parts of the umbra with apparent sink and source areas are revealed, suggesting possible upflows and downflows appearing in different bright and dark locations without a definite answer regarding their brightness identification with a convective or a buoyant cell. Title: Analysis of a Failed Eclipse Plasma Ejection Using EUV Observations Authors: Tavabi, E.; Koutchmy, S.; Bazin, C. Bibcode: 2018SoPh..293...42T Altcode: 2018arXiv180109222T The photometry of eclipse white-light (W-L) images showing a moving blob is interpreted for the first time together with observations from space with the PRoject for On Board Autonomy (PROBA-2) mission (ESA). An off-limb event seen with great details in W-L was analyzed with the SWAP imager (Sun Watcher using Active pixel system detector and image Processing) working in the EUV near 174 Å. It is an elongated plasma blob structure of 25 Mm diameter moving above the east limb with coronal loops under. Summed and co-aligned SWAP images are evaluated using a 20-h sequence, in addition to the 11 July, 2010 eclipse W-L images taken from several sites. The Atmospheric Imaging Assembly (AIA) instrument on board the Solar Dynamics Observatory (SDO) recorded the event suggesting a magnetic reconnection near a high neutral point; accordingly, we also call it a magnetic plasmoid. The measured proper motion of the blob shows a velocity up to 12 kms−1. Electron densities of the isolated condensation (cloud or blob or plasmoid) are photometrically evaluated. The typical value is 108cm−3 at r =1.7 R⊙, superposed on a background corona of 107cm−3 density. The mass of the cloud near its maximum brightness is found to be 1.6 ×1013 g, which is typically 0.6 ×10−4 of the overall mass of the corona. From the extrapolated magnetic field the cloud evolves inside a rather broad open region but decelerates, after reaching its maximum brightness. The influence of such small events for supplying material to the ubiquitous slow wind is noticed. A precise evaluation of the EUV photometric data, after accurately removing the stray light, suggests an interpretation of the weak 174 Å radiation of the cloud as due to resonance scattering in the Fe IX/X lines. Title: Preliminary optical design of the coronagraph for the ASPIICS formation flying mission Authors: Vivès, S.; Lamy, P.; Saisse, M.; Boit, J. -L.; Koutchmy, S. Bibcode: 2017SPIE10567E..1WV Altcode: Formation flyers open new perspectives and allow to conceive giant, externally-occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft at approximately 100-150 m from the first one. ASPIICS (Association de Satellites Pour l'Imagerie et l'Interfromtrie de la Couronne Solaire) is a mission proposed to ESA in the framework of the PROBA-3 program of formation flying which is presently in phase A to exploit this technique for coronal observations. ASPIICS is composed of a single coronagraph which performs high spatial resolution imaging of the corona as well as 2-dimensional spectroscopy of several emission lines from the coronal base out to 3 R. The selected lines allow to address different coronal regions: the forbidden line of Fe XIV at 530.285 nm (coronal matter), Fe IX/X at 637.4 nm (coronal holes), HeI at 587.6 nm (cold matter). An additional broad spectral channel will image the white light corona so as to derive electron densities. The classical design of an externally occulted coronagraph is adapted to the detection of the very inner corona as close as 1.01 R and the addition of a Fabry-Perot interferometer using a so-called "etalon". This paper is dedicated to the description of the optical design and its critical components: the entrance optics and the FabryPerot interferometer. Title: Stray light rejection in giant externally-occulted solar coronagraphs: experimental developments Authors: Venet, M.; Bazin, C.; Koutchmy, S.; Lamy, P. Bibcode: 2017SPIE10565E..1WV Altcode: The advent of giant, formation-flight, externally-occulted solar coronagraphs such as ASPIICS (Association de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne Solaire [1,2,3,4]) selected by the European Space Agency (ESA) for its third PROBA (Project for On-Board Autonomy) mission of formation flying demonstration (presently in phase B) and Hi-RISE proposed in the framework of ESA Cosmic Vision program, presents formidable challenges for the study and calibration of instrumental stray light. With distances between the external occulter (EO) and the optical pupil (OP) exceeding hundred meters and occulter sizes larger than a meter, it becomes impossible to perform tests at the real scale. The requirement to limit the over-occultation to less than 1.05 Rsun, orders of magnitude to what has been achieved so far in past coronagraphs, further adds to the challenge. We are approaching the problem experimentally using reduced scale simulators and present below a progress report of our work. Title: Improved SOT (Hinode mission) high resolution solar imaging observations: 2—Photometric properties of sunspot umbral dots Authors: Goodarzi, H.; Koutchmy, S.; Adjabshirizadeh, A. Bibcode: 2016Ap&SS.361..366G Altcode: The origin and evolution of solar sunspots in deep photospheric layers are not yet well understood. The case of a quasi-symmetric single mature sunspot near the solar centre is selected for analysis. We use the best available observations of the partial Sun free of turbulent Earth atmospheric effects from the Solar Optical Telescope (SOT) onboard the Hinode spacecraft, after greatly improving the resolution with an optimum Max-likelihood deconvolution with the Point Spread Function (PSF) deduced in a preceding paper. For several different images both the smearing due to the instrumental diffraction effects (PSF core) and the large angle stray light are removed. The selected iterative processing depends on both the signal/noise ratio and on the desired contrast of the ultimate details under examination. The photometric properties of bright umbral dots (BUDs) are deduced from corrected frames. Calibrated isophote maps are provided to show the intensity variations around each UD across the background umbra and the surrounding photospheric field, including the penumbra. We deduce the typical photometrical properties of bright UDs that populate the whole umbral surface down to sub-pixel scales of 0.05448''. The analysis demonstrates the basic heterogeneous nature of the umbra, similar to a network of minute bright and dark round or elongated cells with a spacing of order of 0.35''. For the first time a complete and detailed map of the color index and temperature deduced from the analysis of deeply corrected continuum images is provided, showing that tiny bright UDs can reach photospheric temperatures and even higher for the peripheral BUDs. In the umbra, there are some very dark small regions with temperatures as low as 3100 K. Close links seemingly exist with bright UDs. Central BUDs and peripheral BUDs are found to have similar properties but significantly different contrast values. Photometric analysis shows a large dispersion that reflects the broad range of dynamical phenomena involved in the umbra and its periphery, suggesting that the small scale activity observed in the deepest measured photospheric layers of the umbra determines the more impressive rapid phenomena observed in higher layers. Title: Multiple Null Point Reconnections in a limb faint cool jet ejection event Authors: Tavabi, E.; Koutchmy, S. Bibcode: 2016aiaw.conf..127T Altcode: Giant spicules and macro- spicules are an important extended rather cool structure between the solar surface and the corona, partly filling the space inside the chromosphere and surrounded by a transition thin region. Their formation and dynamical properties are still mysterious. In order to explain solar limb and disc periodic recurrences of these events, a simulation model assuming quasi- random positions of spicules above the solar limb was studied. We allow a set number of spicules with different physical properties (such as height, lifetime and tilt angle as shown by an individual spicule) randomly occurring. It is assumed that after reaching a maximum length, the spicules are less rapidly falling back to the solar surface. This kind of limb event was often reported in the literature (spike; giant spicule; Ha ejection event; spray etc) but no serious quantitative analysis could be done. Indeed from ground-based observations, it is impossible to deduce precised parameters because the earth atmospheric turbulent effects makes impossible to make small scale measurements. SOT space-borne observations we use are unique in providing well reproducible observations permitting very precise measurements. The study of X-ray jets is an important topic to understand the heating of the solar corona and the origin of the fast wind. The recently launched Hinode mission permitted to observe the cool proxies of these jets with an unprecedented high spatial resolution of 120 km on the Sun. We selected a high cadence sequence of SOT (Hinode) observations taken with both the HCaII and the Hα filter to look at the details of the dynamics revealed by a large jet event. Both wavelet and amplitude spectra analysis were used to analyze the observed kink wave and the time variations of intensities during the event. The results are discussed in the frame of different models implying reconnections with the inference of the dynamical phenomena occurring in the vicinity of several null points, including the oscillatory behavior. Title: An airborne infrared spectrometer for solar eclipse observations Authors: Samra, Jenna; Cheimets, Peter; DeLuca, Edward; Galeros, John; Gauron, Thomas; Golub, Leon; Guth, Giora; Hertz, Edward; Judge, Philip; Koutchmy, Serge; Marquez, Vanessa Bibcode: 2016SPIE.9908E..5US Altcode: This paper presents the design of an innovative solar spectrometer that will y on the NSF/NCAR Gulfstream V High-Performance Instrumented Airborne Platform for Environmental Research (GV HIAPER) during the 2017 solar eclipse. The airborne infrared spectrometer (AIR-Spec) is groundbreaking in two aspects: it will image infrared coronal emission lines that have never been measured, and it will bring high resolution imaging to GV HIAPER. The instrument development faces the challenges of achieving adequate resolution and signal-to-noise ratio in a compact package mounted to a noisy moving platform. To ensure that AIR-Spec meets its research goals, the instrument is undergoing pre-flight modeling and testing. The results are presented with reference to the instrument requirements. Title: Prominence material embedded in coronal mass ejections as observed with the LASCO-C2 coronagraph using polarization diagnostic Authors: Lamy, Philippe; Boclet, Brice; Koutchmy, Serge Bibcode: 2016cosp...41E1107L Altcode: Prominences are believed to be caused by the formation of a flux rope low in the magnetic structure that eventually erupts to form the CME. Indeed, many CME onset models (e.g., flux cancellation, mass loading) require the presence or formation of a prominence in order for the CME to erupt. The remnants of the cool prominence material is often seen as recognizable twisted structures inside the CME in the lines of He II at 304 Å, of D3 HeI at 587.5 nm, and of Hα at 656 nm, sometime up to a distance of several solar radii from the surface in the latter lines. The orange filter of the LASCO-C2 coronagraph includes the D3 HeI line and its presence in the core of CMEs can be unambiguously detected on polarized images as polarization allows disentangling the contributions from the hot coronal plasma (the polarized Thomson scattered light by electrons) and from the unpolarised emission of cool prominence material. This has been made possible by an in-depth calibration that removes adverse instrumental effects. We will show several examples of CME with embedded prominence material and we will attempt to estimate the mass of this material to be compared with that of the CME. We will also exploit the polarization measurements to reconstruct the 3D geometry of the observed CMEs. Title: Photometric analysis of the corona during the 20 March 2015 total solar eclipse: density structures, hydrostatic temperatures and magnetic field inference. Authors: Bazin, C.; Vilinga, J.; Wittich, R.; Koutchmy, S.; Mouette, J.; Nitschelm, C. Bibcode: 2015sf2a.conf..259B Altcode: 2015arXiv151006436B We present some new accurate CCD photometry analysis of the white light solar corona at the time of the last 20 March 2015 total eclipse (airborne observations on a Falcon 7X and at ground-based- Svalbard). We measured coronal brightness profiles taken along radial directions from 1.001 to 3 solar radii in the northern, southern and equatorial regions, after removing the F-corona and the sky background. These studies allow to evaluate the density gradients, structures and temperature heterogeneity, by considering the Thomson scattering in white light of the K- corona and also emissions of the EUV Fe XII 193A (1 to 2 MK) and Fe XI 171/174 (lower temperature) simultaneously observed by SDO/AIA and SWAP/Proba2 space missions. Some dispersion between the regions is noticed. The limitation of the hydrostatic equilibrium assumption in the solar atmosphere is discussed as well as the contribution of the magnetic field pressure gradients as illustrated by a comparison with the model stationary magnetic corona from Predictive Sc. Inc. These results are compared with the results of the quieter 2010 total solar eclipse corona analyzed with the same method. This photometric analysis of the inner and intermediate white light corona will contribute to the preparation of the Aspiics/Proba 3 flying formation future coronagraphic mission of ESA for new investigation at time of artificial eclipses produced in Space. Note that Aspiics will also observe in the He I D3 line at 5876 A, and will record intensities of the Fe XIV line 5303A simultaneously with the analysis of the orange white- light continuum, including precise polarimetry analysis. . Title: Limb Event Brightenings and Fast Ejection Using IRIS Mission Observations Authors: Tavabi, E.; Koutchmy, S.; Golub, L. Bibcode: 2015SoPh..290.2871T Altcode: 2015SoPh..tmp..118T; 2015arXiv150706794T The Interface Region Imaging Spectrograph (IRIS) of the recently commissioned NASA small explorer mission provides significantly more complete and higher resolution spectral coverage of the dynamical conditions inside the chromosphere and transition region (TR) than has been available ever before. High temporal, spatial (0.3″) and spectral resolution observations from the ultraviolet IRIS spectra near the solar limb reveal high-energy limb event brightenings (LEBs) at low chromospheric heights at about 1 Mm above the limb. They can be characterized as explosive events producing jets. We selected two events showing spectra of a confined eruption just off or near the quiet-Sun limb, the jet part showing obvious moving material with short-duration large Doppler shifts in three directions that were identified as macrospicules on slit-jaw (SJ) images in Si IV and He II 304 Å. The events were analyzed from a sequence of very close rasters taken near the central meridian and the South Pole limb. We analyzed the processed SJ images and the simultaneously observed fast spectral sequences, which have large Doppler shifts, with a pair of redshifted elements together with a faster blueshifted element from almost the same position. Shifts correspond to velocities of up to 100 kms−1 in projection on the plane of the sky. Erupting spicules and macrospicules from these regions are visible in images taken before and after the spectra. The cool low first ionization potential (FIP) element simultaneous line emissions of the Mg II h and k resonance lines do not clearly show a similar signature because of optical thickness effects, but the Si IV broadband SJ images do. The bidirectional plasma jets ejected from a small reconnection site are interpreted to be the result of coronal loop-loop interactions that lead to reconnection in nearby sites. Title: A Novel Technique for Measuring the Solar Radius from Eclipse Light Curves - Results for 2010, 2012, 2013, and 2015 Authors: Lamy, Philippe; Prado, Jean-Yves; Floyd, Olivier; Rocher, Patrick; Faury, Guillaume; Koutchmy, Serge Bibcode: 2015SoPh..290.2617L Altcode: 2015SoPh..tmp..170L We report on a novel technique for measuring the solar radius during total solar eclipses that exploits light curves recorded just before and after second and third contacts. The measurements are performed by pre-programmed photometers that are deployed over the eclipse paths and are operated without supervision. The recorded light curves are compared to synthetic light curves calculated from high-accuracy ephemerides and lunar-limb profiles constructed from the topographic model of the Moon provided by the Kaguya lunar space mission. A minimization process between the two sets of curves yields the solar radius. Altogether, seventeen determinations have been obtained during the past four total eclipses with the following averages (at a wavelength of 540 nm and scaled to 1 AU): 959.94 ±0.02 arcsec on 11 July 2010, 960.02 ±0.04 arcsec on 13 November 2012, 959.99 ±0.09 arcsec on 3 November 2013, and 960.01 ±0.09 arcsec on 20 March 2015. Part of the differences between these four values may be attributed to weather conditions. Averaging the whole set of measurements yields a radius of 959.99 ±0.06 arcsec (696 ,246 ±45 km), which agrees excellently well with the most recent data and supports an upward revision of the standard IAU value, as previously suggested. Title: Design and modelisation of ASPIICS optics Authors: Galy, C.; Fineschi, S.; Galano, D.; Howard, R. A.; Kintziger, C.; Kirschner, V.; Koutchmy, S.; Lamy, P.; Mazzoli, A.; Melich, R.; Mestreau-Garreau, A.; Renotte, E.; Servaye, J. S.; Stockman, Y.; Thizy, C.; Zhukov, A. Bibcode: 2015SPIE.9604E..0BG Altcode: In the framework of development of ASPIICS (Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun), the Centre Spatial de Liege is responsible of the optical design of the coronagraph and the optics will be manufactured by TOPTEC. The particularity of this coronagraph is to have an external occulter located 150 m ahead of the first imaging lens. This external occulter is re-imaged on an internal occulter which function is - as in a classical externally occulted Lyot coronagraph - to block the sun light diffracted by the external occulter and to reduce the straylight on the detector. The selection of this configuration is driven by the requirement to observe the corona as close as possible to the solar limb (i.e. 1 RSun) without imaging the limb itself. A requirement of 1.08 RSun is specified at optical design level to grant 1.2 Rsun at instrument level. The coronograph instrument is designed to have a field of view of 1.6° x 1.6° with a resolution of less than 6 arcsec. Its performances are limited by diffraction in a 530 - 590 nm wavelength range. This paper presents the optical design and demonstrates that by design the requirements are fulfilled within the misalignment, manufacturing and thermo-elastic error contributions. Title: Design status of ASPIICS, an externally occulted coronagraph for PROBA-3 Authors: Renotte, Etienne; Alia, Andres; Bemporad, Alessandro; Bernier, Joseph; Bramanti, Cristina; Buckley, Steve; Capobianco, Gerardo; Cernica, Ileana; Dániel, Vladimir; Darakchiev, Radoslav; Darmetko, Marcin; Debaize, Arnaud; Denis, François; Desselle, Richard; de Vos, Lieve; Dinescu, Adrian; Fineschi, Silvano; Fleury-Frenette, Karl; Focardi, Mauro; Fumel, Aurélie; Galano, Damien; Galy, Camille; Gillis, Jean-Marie; Górski, Tomasz; Graas, Estelle; Graczyk, Rafał; Grochowski, Konrad; Halain, Jean-Philippe A.; Hermans, Aline; Howard, Russ; Jackson, Carl; Janssen, Emmanuel; Kasprzyk, Hubert; Kosiec, Jacek; Koutchmy, Serge; Kovačičinová, Jana; Kranitis, Nektarios; Kurowski, Michał; Ładno, Michał; Lamy, Philippe; Landini, Federico; Lapáček, Radek; Lédl, Vít.; Liebecq, Sylvie; Loreggia, Davide; McGarvey, Brian; Massone, Giuseppe; Melich, Radek; Mestreau-Garreau, Agnes; Mollet, Dominique; Mosdorf, Łukasz; Mosdorf, Michał; Mroczkowski, Mateusz; Muller, Raluca; Nicolini, Gianalfredo; Nicula, Bogdan; O'Neill, Kevin; Orleański, Piotr; Palau, Marie-Catherine; Pancrazzi, Maurizio; Paschalis, Antonios; Patočka, Karel; Peresty, Radek; Popescu, Irina; Psota, Pavel; Rataj, Miroslaw; Rautakoski, Jan; Romoli, Marco; Rybecký, Roman; Salvador, Lucas; Servaye, Jean-Sébastien; Solomon, Cornel; Stockman, Yvan; Swat, Arkadiusz; Thizy, Cédric; Thomé, Michel; Tsinganos, Kanaris; Van der Meulen, Jim; Van Vooren, Nico; Vit, Tomáš; Walczak, Tomasz; Zarzycka, Alicja; Zender, Joe; Zhukov, Andrei Bibcode: 2015SPIE.9604E..0AR Altcode: The "sonic region" of the Sun corona remains extremely difficult to observe with spatial resolution and sensitivity sufficient to understand the fine scale phenomena that govern the quiescent solar corona, as well as phenomena that lead to coronal mass ejections (CMEs), which influence space weather. Improvement on this front requires eclipse-like conditions over long observation times. The space-borne coronagraphs flown so far provided a continuous coverage of the external parts of the corona but their over-occulting system did not permit to analyse the part of the white-light corona where the main coronal mass is concentrated. The proposed PROBA-3 Coronagraph System, also known as ASPIICS (Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun), with its novel design, will be the first space coronagraph to cover the range of radial distances between ~1.08 and 3 solar radii where the magnetic field plays a crucial role in the coronal dynamics, thus providing continuous observational conditions very close to those during a total solar eclipse. PROBA-3 is first a mission devoted to the in-orbit demonstration of precise formation flying techniques and technologies for future European missions, which will fly ASPIICS as primary payload. The instrument is distributed over two satellites flying in formation (approx. 150m apart) to form a giant coronagraph capable of producing a nearly perfect eclipse allowing observing the sun corona closer to the rim than ever before. The coronagraph instrument is developed by a large European consortium including about 20 partners from 7 countries under the auspices of the European Space Agency. This paper is reviewing the recent improvements and design updates of the ASPIICS instrument as it is stepping into the detailed design phase. Title: Improved SOT (Hinode mission) high resolution solar imaging observations Authors: Goodarzi, H.; Koutchmy, S.; Adjabshirizadeh, A. Bibcode: 2015Ap&SS.358...25G Altcode: 2015arXiv150608265G We consider the best today available observations of the Sun free of turbulent Earth atmospheric effects, taken with the Solar Optical Telescope (SOT) onboard the Hinode spacecraft. Both the instrumental smearing and the observed stray light are analyzed in order to improve the resolution. The Point Spread Function (PSF) corresponding to the blue continuum Broadband Filter Imager (BFI) near 450 nm is deduced by analyzing (i) the limb of the Sun and (ii) images taken during the transit of the planet Venus in 2012. A combination of Gaussian and Lorentzian functions is selected to construct a PSF in order to remove both smearing due to the instrumental diffraction effects (PSF core) and the large-angle stray light due to the spiders and central obscuration (wings of the PSF) that are responsible for the parasitic stray light. A Max-likelihood deconvolution procedure based on an optimum number of iterations is discussed. It is applied to several solar field images, including the granulation near the limb. The normal non-magnetic granulation is compared to the abnormal granulation which we call magnetic. A new feature appearing for the first time at the extreme- limb of the disk (the last 100 km) is discussed in the context of the definition of the solar edge and of the solar diameter. A single sunspot is considered in order to illustrate how effectively the restoration works on the sunspot core. A set of 125 consecutive deconvolved images is assembled in a 45 min long movie illustrating the complexity of the dynamical behavior inside and around the sunspot. Title: Inferring the Structure of the Solar Corona and Inner Heliosphere During the Maunder Minimum Using Global Thermodynamic Magnetohydrodynamic Simulations Authors: Riley, Pete; Lionello, Roberto; Linker, Jon A.; Cliver, Ed; Balogh, Andre; Beer, Jürg; Charbonneau, Paul; Crooker, Nancy; DeRosa, Marc; Lockwood, Mike; Owens, Matt; McCracken, Ken; Usoskin, Ilya; Koutchmy, S. Bibcode: 2015ApJ...802..105R Altcode: Observations of the Sun’s corona during the space era have led to a picture of relatively constant, but cyclically varying solar output and structure. Longer-term, more indirect measurements, such as from 10Be, coupled by other albeit less reliable contemporaneous reports, however, suggest periods of significant departure from this standard. The Maunder Minimum was one such epoch where: (1) sunspots effectively disappeared for long intervals during a 70 yr period; (2) eclipse observations suggested the distinct lack of a visible K-corona but possible appearance of the F-corona; (3) reports of aurora were notably reduced; and (4) cosmic ray intensities at Earth were inferred to be substantially higher. Using a global thermodynamic MHD model, we have constructed a range of possible coronal configurations for the Maunder Minimum period and compared their predictions with these limited observational constraints. We conclude that the most likely state of the corona during—at least—the later portion of the Maunder Minimum was not merely that of the 2008/2009 solar minimum, as has been suggested recently, but rather a state devoid of any large-scale structure, driven by a photospheric field composed of only ephemeral regions, and likely substantially reduced in strength. Moreover, we suggest that the Sun evolved from a 2008/2009-like configuration at the start of the Maunder Minimum toward an ephemeral-only configuration by the end of it, supporting a prediction that we may be on the cusp of a new grand solar minimum. Title: Alfvénic waves in polar spicules Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.; Ahangarzadeh Maralani, A. R.; Zeighami, S. Bibcode: 2015A&A...573A...4T Altcode: 2014arXiv1409.7654T Context. For investigating spicules from the photosphere to coronal heights, the new Hinode/SOT long series of high-resolution observations from space taken in CaII H line emission offers an improved way to look at their remarkable dynamical behavior using images free of seeing effects. They should be put in the context of the huge amount of already accumulated material from ground-based instruments, including high- resolution spectra of off-limb spicules.
Aims: Both the origin of the phenomenon and the significance of dynamical spicules for the heating above the top of the photosphere and the fuelling of the chromospheric and the transition region need more investigation, including of the possible role of the associated magnetic waves for the corona higher up.
Methods: We analyze in great detail the proper transverse motions of mature and tall polar region spicules for different heights, assuming that there might be Helical-Kink waves or Alfvénic waves propagating inside their multicomponent substructure, by interpreting the quasi-coherent behavior of all visible components presumably confined by a surrounding magnetic envelop. We concentrate the analysis on the taller CaII spicules more relevant for coronal heights and easier to measure. Two-dimensional velocity maps of proper motion were computed for the first time using a correlation tracking technique based on FFTs and cross-correlation function with a 2nd-order-accuracy Taylor expansion. Highly processed images with the popular mad-max algorithm were first prepared to perform this analysis. The locations of the peak of the cross-correlation function were obtained with subpixel accuracy.
Results: The surge-like behavior of solar polar region spicules supports the untwisting multicomponent interpretation of spicules exhibiting helical dynamics. Several tall spicules are found with (i) upward and downward flows that are similar at lower and middle levels, the rate of upward motion being slightly higher at high levels; (ii) the left- and righthand velocities are also increasing with height; (iii) a large number of multicomponent spicules show shearing motion of both left- and righthanded senses occurring simultaneously, which might be understood as twisting (or untwisting) threads. The number of turns depends on the overall diameter of the structure made of components and changes from at least one turn for the smallest structure to at most two or three turns for surge-like broad structures. The curvature along the spicule corresponds to a low turn number similar to a transverse kink mode oscillation along the threads.

A movie associated to Fig. 1 is available in electronic form at http://www.aanda.org Title: The photosphere-corona Interface: enrichement of the corona in low FIP elements and helium shells Authors: Bazin, C.; Koutchmy, S.; Lamy, P.; Veselovski, I. Bibcode: 2014sf2a.conf..209B Altcode: Slitless consecutive spectra were obtained during the contacts of the last total solar eclipses (2008, 2009, 2010, 2012, et 2013). They allowed to show that the overabundance of low First Ionisation Potential (FIP) elements (Fe II, Ti II, Ba II) in the corona comes from the low layers of the solar atmosphere, just near and above the temperature minimum region of the high photosphere. All spectra are recorded with a fast CCD/CMOS camera, with an equivalent radial resolution of 60 milliarcseconds, or 45 km in the solar atmosphere, above a solar edge not affected by the parasitic light like it is outside of total eclipse conditions. Many emission lines of low FIP elements appear in regions situated between 200 to 600 km above the solar limb defined by the true continuum measured between the lines. This continuum appears at these altitudes where the beta of the plasma is near 1. The He I 4713 Å and He II 4686 Å (Paschen alpha line) shells appear at the height of 800 km above the solar edge and higher. The light curve I = f(h) of each ion is located at a particuliar altitude in the solar atmosphere. The scale height corresponds to a density variation, which allows to evaluate the temperature thanks to the hydrostatic equilibrium assumption. Moreover, with ionised Titanium lines taken as markers, we show a similarity between the photosphere-corona interface and the prominence-corona interface. We discuss the role of the magnetic field and the ambipolar diffusion for supplying the corona in mass, without taking into account the role of spicules. The photo-ionisation of the helium lines by the EUV coronal lines is illustrated thanks to an extract of SDO/AIA coronal stacked image simultaneously obtained. Title: The June 6 2012 transit of Venus: Imaging and spectroscopic analysis of the upper atmosphere emission Authors: Bazin, C.; Zhi, X.; Valls-Gabaud, D.; Koutchmy, S.; Rocher, P.; Zin, Z. Y.; Fu, Y.; Yang, L.; Liu, G. Q.; Liu, Z.; Ji, K.; Goodarzi, H. Bibcode: 2014sf2a.conf...57B Altcode: In the context of transiting exoplanets, the last June 6, 2012 Venus transit was a unique opportunity to address important questions regarding its atmosphere. The transit of Venus is indeed a particular case of an Earth-like planet transit, and the inference one can make about the upper layers of its atmosphere can be applied to other exoplanets. To this aim, we designed a small spectrograph that we placed at the focus of the New Vacuum Solar Telescope of Yunnan Observatory in China (45 m focus and 1 m of aperture), coupled to a 4K×2K 14 bit CCD detector, to measure low-resolution optical spectra of the refracted, scattered and transmitted solar radiation in the upper layers of the planet. It covered the 385-780 nm range when Venus was over the disc, and 540-680 nm (including the O_2 terrestrial bands) during the 18 minutes-long egress. The Hα and He I D3 lines were recorded repeatedly. The atmospheric Lomonossov arc of Venus was simultaneously imaged using Hα and TiO filters, allowing us to check the slit position on the images of Venus and to locate the spectroscopic features on its disc. The spectra show the signature of the Northern Pole horn part; a second part was evidenced on the spectra taken near but outside the limb. We studied the O_2, H_2O and Hα line profiles searching for signatures arising from Venus and we compared the observed spectra with synthetic models. The spectroscopic dataset can now be used by a large community for discussing the properties of the upper atmosphere of Venus and the future detection of Venus-like exoplanets. Finally, the study is completed using a unique very high resolution deconvolved image of the arc and Venus silhouetted at the limb of the Sun, from the SOT of the Hinode space mission. Title: Spectral atlases of the Sun from 3980 to 7100 Å at the center and at the limb Authors: Fathivavsari, H.; Ajabshirizadeh, A.; Koutchmy, S. Bibcode: 2014Ap&SS.353..347F Altcode: 2014arXiv1407.5727F In this work, we present digital and graphical atlases of spectra of both the solar disk-center and of the limb near the Solar poles using data taken at the UTS-IAP & RIAAM (the University of Tabriz Siderostat, telescope and spectrograph jointly developed with the Institut d'Astrophysique de Paris and Research Institute for Astronomy and Astrophysics of Maragha). High resolution and high signal-to-noise ratio (SNR) CCD-slit spectra of the sun for 2 different parts of the disk, namely for μ=1.0 (solar center) & for μ=0.3 (solar limb) are provided and discussed. While there are several spectral atlases of the solar disk-center, this is the first spectral atlas ever produced for the solar limb at this spectral range. The resolution of the spectra is about R∼70 000 (Δ λ∼0.09 Å) with the signal-to-noise ratio (SNR) of 400-600. The full atlas covers the 3980 to 7100 Å spectral regions and contains 44 pages with three partial spectra of the solar spectrum put on each page to make it compact. The difference spectrum of the normalized solar disk-center and the solar limb is also included in the graphic presentation of the atlas to show the difference of line profiles, including far wings. The identification of the most significant solar lines is included in the graphic presentation of the atlas. Telluric lines are producing a definite signature on the difference spectra which is easy to notice. At the end of this paper we present only two sample pages of the whole atlas while the graphic presentation of the whole atlas along with its ASCII file can be accessed via the ftp server of the CDS in Strasbourg via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via this link: http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/other/ApSS. Title: Oscillations in solar jets observed with the SOT of Hinode: viscous effects during reconnection Authors: Tavabi, E.; Koutchmy, S. Bibcode: 2014Ap&SS.352....7T Altcode: 2014arXiv1403.0814T Transverse oscillatory motions and recurrence behavior in the chromospheric jets observed by Hinode/SOT are studied. A comparison is considered with the behavior that was noticed in coronal X-ray jets observed by Hinode/XRT. A jet like bundle observed at the limb in Ca II H line appears to show a magnetic topology that is similar to X-ray jets (i.e., the Eiffel tower shape). The appearance of such magnetic topology is usually assumed to be caused by magnetic reconnection near a null point. Transverse motions of the jet axis are recorded but no clear evidence of twist is appearing from the highly processed movie. The aim is to investigate the dynamical behavior of an incompressible magnetic X-point occurring during the magnetic reconnection in the jet formation region. The viscous effect is specially considered in the closed line-tied magnetic X-shape nulls. We perform the MHD numerical simulation in 2-D by solving the visco-resistive MHD equations with the tracing of velocity and magnetic field. A qualitative agreement with Hinode observations is found for the oscillatory and non-oscillatory behaviors of the observed solar jets in both the chromosphere and the corona. Our results suggest that the viscous effect contributes to the excitation of the magnetic reconnection by generating oscillations that we observed at least inside this Ca II H line cool solar jet bundle. Title: VizieR Online Data Catalog: 398-710nm Sun spectral atlases (Fathivavsari+, 2014) Authors: Fathivavsari, H.; Ajabshirizadeh, A.; Koutchmy, S. Bibcode: 2014yCatp017035301F Altcode: The "spectrum.pdf" file contains 44 pages of graphic presentation of the solar disk-center vs. solar limb spectra with the identification of most of the lines included. Each page contains 3 partial spectra. The identification of lines is made using the reference atlas of Moore et al. (1966). Each page contains three spectral windows, with each window made up of two panels. The upper panel shows the spectrum of the solar disk-center (black curve) on which the spectrum of the solar limb is overplotted as red curve while the lower panel illustrates the difference spectrum of the two. The difference spectrum of the lower panel clearly indicates that the depth of the absorption lines taken at the solar disk-center is usually deeper than those taken at the solar limb (in this panel the two pink dashed lines indicate the residual intensity of 0.05 above and below zero). Note that, in the solar limb spectrum, the level of the continuum was put to the reference level given in the "Astrophysical Quantities, 3rd Edition by C. W. Allen, p. 169".

(2 data files). Title: Observation of the prominence cavity region using slitless eclipse flash spectra and space borne EUV filtergrams Authors: Bazin, Cyrille; Koutchmy, Serge; Lamy, Philippe; Tavabi, Ehsan Bibcode: 2014IAUS..300..151B Altcode: We used total solar eclipse free of parasitic light for studying the prominence to corona interface, and the corresponding cavity in the context of the coronal physics. We analysed the visible continuum between the prominences to directly look at the electron density. We demonstrate some enhanced heating in the cavity region. Some similarities with the interface regions are shown: the photosphere to the chromosphere and the prominence to the corona interface. The optically thin neutral Helium at 4713 Å and the singly ionized Helium 4686 Å Paschen α lines are considered. We summed 80 slitless visible eclipse flash spectra that we compare with simultaneously obtained EUV SWAP/Proba2 174 Å images of ESA and AIA/SDO 171Å 193 Å 304 Å and 131 Å filtergrams. Intensity profiles in a radial direction are studied. We deduce the variation of the intensity ratio I(He I 4713) / I(He II 4686). Discussion: the temperature rises at the edge of the prominences. We evaluate for the first time with spectrophotometric accuracy the continuum modulations in prominence spectra. W-L intensity deficits are observed near the prominence boundaries in both eclipse spectra and in EUV images, confirming that the prominence -cavity regions correspond to a relative depression of plasma density of the surrounding corona. Conclusion: we demonstrate some enhanced heating occurring in these regions assuming hydrostatic equilibrium. Title: 3D dynamical structuring of a high latitude erupting prominence: I- Analysis of the cool plasma flows before the eruption Authors: Koutchmy, Serge; Filippov, Boris; Tavabi, Ehsan; Bazin, Cyril; Weiller, Sylvain Bibcode: 2014IAUS..300..430K Altcode: Both the origin of the quiescent prominences and their eruption related to CMEs are still a matter of extended studies. The small scale dynamic aspects like vortex structures and counter- flows are now seriously taken into account having in mind that the flows are a good proxy of the line of force of the omnipresent but rather unknown in detail force free or not magnetic field. Large scale vortex has been detected in a high latitude prominence observed on November 13- 14, 2011 before its eruption. Title: 3D dynamical structuring of a high latitude erupting prominence: II- Analysis of the coronal context and eruption Authors: Koutchmy, Serge; Filippov, Boris; Tavabi, Ehsan; Bazin, Cyrille; Weiller, Sylvain Bibcode: 2014IAUS..300..433K Altcode: Both the origin of the quiescent prominences and their eruption related to CMEs event are still a matter of extended studies. The case of high latitudes quiescent prominences producing slow CMEs can be considered as a potential component of the slow wind. A high latitude prominence was observed on November 13 - 14, 2011. A schematic representation of flux rope is proposed to describe the magnetic structure of the prominence prior to its eruption. Title: Solar eruptive phenomena Authors: Filippov, B.; Koutchmy, S.; Martsenyuk, O.; Platov, Y. Bibcode: 2013AIPC.1551..117F Altcode: At the beginning of the 1990s, it was found out that the strongest disturbances of space weather were associated with huge ejections of matter from the solar corona, which took the form of the magnetic clouds when moved from the Sun. It is the collisions of the magnetic clouds with the Earth's magnetosphere that lead to strong, sometimes to catastrophic, changes in space weather. The onset of a coronal mass ejection (CME) is sudden and no reliable forerunners of CMEs have been found till now. The problem of CME prediction is less developed than the problem of solar flare prediction. The most probable initial magnetic configuration of a CME is a flux rope consisting of twisted field lines which fill the whole volume of a dark coronal cavity. Cold dense prominence material can be collected in the lower parts of the helical flux tubes. Filaments are then the best tracers of the flux ropes in the corona, visible long before the beginning of the eruption. Title: Formation of a White-Light Jet Within a Quadrupolar Magnetic Configuration Authors: Filippov, Boris; Koutchmy, Serge; Tavabi, Ehsan Bibcode: 2013SoPh..286..143F Altcode: 2011arXiv1111.2150K; 2012SoPh..tmp....1F We analyze multi-wavelength and multi-viewpoint observations of a large-scale event viewed on 7 April 2011, originating from an active-region complex. The activity leads to a white-light jet being formed in the outer corona. The topology and evolution of the coronal structures were imaged in high resolution using the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). In addition, large field-of-view images of the corona were obtained using the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) telescope onboard the PRoject for Onboard Autonomy (PROBA2) microsatellite, providing evidence for the connectivity of the coronal structures with outer coronal features that were imaged with the Large Angle Spectrometric Coronagraph (LASCO) C2 on the Solar and Heliospheric Observatory (SOHO). The data sets reveal an Eiffel-tower type jet configuration extending into a narrow jet in the outer corona. The event starts from the growth of a dark area in the central part of the structure. The darkening was also observed in projection on the disk by the Solar TErrestrial RElations Observatory-Ahead (STEREO-A) spacecraft from a different point of view. We assume that the dark volume in the corona descends from a coronal cavity of a flux rope that moved up higher in the corona but still failed to erupt. The quadrupolar magnetic configuration corresponds to a saddle-like shape of the dark volume and provides a possibility for the plasma to escape along the open field lines into the outer corona, forming the white-light jet. Title: Prominence Cavity Regions Observed Using SWAP 174 Å Filtergrams and Simultaneous Eclipse Flash Spectra Authors: Bazin, C.; Koutchmy, S.; Tavabi, E. Bibcode: 2013SoPh..286..255B Altcode: 2012arXiv1205.1325B; 2012SoPh..tmp..309B SWAP images from PROBA2 taken at 174 Å in the Fe IX/X lines are compared with simultaneous slitless flash spectra obtained during the solar total eclipse of 11 July 2010. Myriad faint low-excitation emission lines together with the He I and He II Paschen α chromospheric lines are recorded on eclipse spectra where regions of limb prominences are obtained with space-borne imagers. We analyzed a deep flash spectrum obtained by summing 80 individual spectra to evaluate the intensity modulations of the continuum. Intensity deficits are observed and measured at the prominences boundaries in both eclipse and SWAP images. The prominence cavities interpreted as a relative depression of plasma density, produced inside the corona surrounding the prominences, and some intense heating occurring in these regions, are discussed. Photometric measurements are shown at different scales and different, spectrally narrow, intervals for both the prominences and the coronal background. Title: Helium shells and faint emission lines from slitless flash spectra Authors: Bazin, Cyril; Koutchmy, Serge Bibcode: 2013JAdR....4..307B Altcode: At the time of the two last solar total eclipses of August 1st, 2008 in Siberia and July 11th, 2010 in French Polynesia, high frame rate CCD flash spectra were obtained. These eclipses occurred in quiet Sun period and after. The slitless flash spectra show two helium shells, in the weak Paschen α 4686 Å line of the ionized helium HeII and in the neutral helium HeI line at 4713 Å. The extensions of these helium shells are typically 3 Mm. In prominences, the extension of the interface with the corona is much more extended. The observations and analysis of these lines can properly be done only in eclipse conditions, when the intensity threshold reaches the coronal level, and the parasitic scattered light is virtually zero. Under the layers of 1 Mm above the limb, many faint low FIP lines were also seen in emission. These emission lines are superposed on the continuum containing absorption lines. The solar limb can be defined using the weak continuum appearing between the emission lines at the time of the second and third contact. The variations of the singly ionized iron line, the HeI and HeII lines and the continuum intensity are analyzed. The intensity ratio of ionized to neutral helium is studied for evaluating the ionization rate in low layers up to 2 Mm and also around a prominence. Title: Increasing the Fine Structure Visibility of the Hinode SOT Ca II H Filtergrams Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A. Bibcode: 2013SoPh..283..187T Altcode: 2012SoPh..tmp..107T; 2011arXiv1104.5580T We present an image processing technique, the improved OMC filter (also called Madmax), which selects maxima of convexities of intensity modulations of an image. The filter computes second derivatives of the image in multiple directions around each pixel. It is shown to be efficient for pattern recognition, and bright hair-like or small anisotropic features can be enhanced. The filter is tested on artificially generated images, and the effect of a different number of directions in which the second derivatives are calculated is evaluated. Ca II H line images of spicules and prominences obtained with Hinode/SOT are also used to illustrate its efficiency on real data. It is shown how to make the choice of the sensitive parameters to be used in improving the image visibility. Title: About the solar edge and solar diameter variation studies Authors: Bazin, C.; Koutchmy, S.; Rocher, P. Bibcode: 2012sf2a.conf..495B Altcode: Without spurious effects due to instrumental and/or Earth atmospheric parasitic light, the true solar edge can only be correctly analyzed at the time of solar total eclipses. We discuss the problems occurring when using solar diameter measurements made outside of solar total eclipses, including the possible limb effects related to different sources of solar activity. Effects due to the PSF and to the scattered light should be discussed with reference to coronagraphic methods used to reduce the ultimate sources of parasitic light. Title: Photometric properties of new solar H alpha commercial Fabry-Perot etalons. Application to the analysis of the chromospheric fringe Authors: Bazin, Cyril; Koutchmy, Serge Bibcode: 2012arXiv1209.1027B Altcode: We consider the use of the commercially available Fabry-Perot etalons (FP) for the imaging of the solar chromosphere in the H alpha line of HI. Three etalons of 40, 60 and 90 mm diameter were accurately analysed. At normal incidence the maximum transmission wavelength as well as the finesse were evaluated. Polynomial curves precisely fitting the transmitted central wavelength variations when using a quasi-parallel beam from a point-like source are presented. Further calibrations have been done with photometric accuracy using a laboratory set-up comprising i/ a 16 bits CCD camera; ii/ a Littrow spectrograph of a spectral power 110000 giving a linear dispersion of 0.0058 nm/pixel and iii/ an artificial Sun used as a light source and iv/ precisely adjustable in position optical components, including the F-P etalons. In addition, a precise laboratory wavelength calibration was performed using a low pressure deuterium 2D spectral lamp simultaneously illuminating the adjustable entrance slit using a splitter before. The variations of the FWHM of the spectral transmission variations as a function of the incidence angle of a parallel beam are also given for each etalon. Consequences resulting from the use of a low but significant aperture/ratio are tentatively discussed for the first time. An application to a precise photometric work of solar physics interest when using limb filtergrams is illustrated and discussed, with emphasis on the photometric accuracy resulting from the use of such etalons put before the entrance aperture of an imaging telescope. Monochromatic images of the solar chromosphere shell in the vicinity of the polar and equatorial limbs were made using a small telescope, in order to deduce the variation of the typical average thicknesses at poles and equator interpreted as a prolateness effect of the chromospheric shell observed during the last minimum of solar activity (2009). Title: Prominence-cavity regions observed using SWAP 17.4 nm filtergrams and simultaneous eclipse flash spectra Authors: Bazin, C.; Koutchmy, S.; Tavabi, E. Bibcode: 2012arXiv1207.1857B Altcode: SWAP images from PROBA2 taken at 174 Å in the Fe IX/X lines are compared with simultaneous slitless flash spectra obtained during the solar total eclipse of 11 July, 2010. Myriads of faint low excitation emission lines together with the He I and He II Paschen {\alpha} chromospheric lines are recorded on eclipse spectra where regions of limb prominences are obtained with space-borne imagers. We analyzed a deep flash spectrum obtained by summing 80 individual spectra to evaluate the intensity modulations of the continuum. Intensity deficits are observed and measured at the prominences boundaries in both eclipse and SWAP images. The prominence cavities interpreted as a relative depression of plasma density, produced inside the corona surrounding the prominences, and some intense heating occurring in these regions, are discussed. Photometric measurements are shown at different scales and different, spectrally narrow, intervals for both the prominences and the coronal background. Title: Detection of Chromospheric Alfven Waves in Solar Spicule Authors: Ajabshirizadeh, Ali; Koutchmy, Serge; Tavabi, Ehsan Bibcode: 2012cosp...39...30A Altcode: 2012cosp.meet...30A No abstract at ADS Title: Plasmoid Ejection at a Solar Total Eclipse Authors: Koutchmy, S.; Bazin, C.; Berghmans, D.; De Groof, A.; Druckmüller, M.; Tavabi, E.; Engell, A.; Filippov, B.; Golub, L.; Lamy, Ph.; Linker, J.; Mikic, Z.; Mouette, J.; Nitschelm, Ch.; Seaton, D.; Slemzin, V. Bibcode: 2012EAS....55..223K Altcode: The existence of coronal plasmoids has been postulated for many years in order to supply material to streamers and possibly to the solar wind (SW). The W-L SoHO C2 Lasco coronagraph observations were made under the 2.2 solar radii (R0) occulting disk to look at the ultimate sources of the SW; EUV imagers are preferably devoted to the analysis of the corona on and very near the solar disk. Here, in addition to eclipse white-light (W-L) snapshots, we used the new SWAP space-borne imager designed for the systematic survey of coronal activity in the EUV lines near 17.4 nm, over a field of view (FOV) up to 2 R0. Using summed and co-aligned images, the corona can then be evaluated for the 1st time up to the limit of this FOV. At the time of the July 11, 2010, solar total eclipse a 20h continuous run of observations was collected, including images taken during eclipse totality from several ground observing locations where W-L data were collected. A plasmoid-like off-limb event was followed using the SWAP summed Title: Homologous flares inducing EUV filament oscillations with subsequent eruption Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J.; Tavabi, E. Bibcode: 2012EAS....55..335B Altcode: We focus our analysis on an event which occurred at the W-limb on May 30, 2003. The dynamical behavior of the filament, including damped oscillations, was investigated with the CDS and EIT (SoHO) experiments, as well as with Hα filtergrams (movies). The eruptive phase is analyzed taking into account the approximate phasing with other eruptive phenomena occurring at the same time or before, called homologous flares and eruptions. Title: About the magnetic origin of Chromospheric Spicules and Coronal Jets Authors: Koutchmy, S.; Filippov, B.; Tavabi, E. Bibcode: 2012EAS....55..257K Altcode: Observations of jet- like phenomena near the solar limb are reported for a long time, first in Hα (Secchi observations of spicules in the 1870 ies), and after, from eclipse high resolution coronal images taken in white-light (1920-1973) as spiky structures. EUV jets were reported in the 70 ies from rocket and space-borne CIV filtergrams and finally X-EUV jets were reported from SXT observations of Yohkoh and from EIT and CDS SoHO observations. There is now little doubt that they are of magnetic origin although no magnetic field measurements exist for these regions and thermo-dynamical models are still work out. New observations of both spicules and jets with the SOT/SXT of Hinode were subjected to an analysis showing the influence of the null point(s) of the magnetic field. The collective behavior of the H CaII SOT(Hinode) time sequences of processed with the Madmax operator images of limb spicules show the torsional effects which were partly suggested before from the interpretation of high resolution limb spectra taken on Russian coronagraphs and the VTT at SacPeak. 100 s and shorter period waves are recorded. We propose a reconnection process occurring at the top of an emerging twisted flux tube for explaining some peculiarities of the spicular eruptions and possibly, as a viable mechanism for explaining the SXR jet eruptions. The result of a numerical 3D modeling illustrates this erupting mechanism although the behavior of the magneto-plasma structure near a null point, as shown by coronal filtergrams, does not necessary imply reconnections, especially the case of jets making a long coronal ray we observed in white-light with Lasco C2. Title: Prominence-cavity regions observed in 2010 eclipse flash spectra and SWAP images Authors: Bazin, C.; Koutchmy, S.; Tavabi, E. Bibcode: 2012EAS....55..185B Altcode: Images from the SWAP (Proba 2 mission) taken in the Fe IX/X coronal line emission are compared to simultaneous slitless flash spectra taken during the total solar eclipse of July, 11th 2010. Many faint low excitation emission lines together with the HeI and the HeII Paschen α (Pα) chromospheric lines are recorded in the regions of limb prominences observed in space. We consider a deep flash spectrum obtained by summing 80 individual spectra to show the intensity modulations of the continuum between HeI and HeII lines. Intensity depressions are observed around the prominences in both eclipse and SWAP images. The prominence cavities are interpreted as a relative depression of plasma density produced inside the corona surrounding the prominences, and some evidence of intense heating occuring in the region around the prominence is discussed. Title: solar spicules and jets Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A. Bibcode: 2012EAS....55...71T Altcode: In order to clear up the origin and possibly explain some solar limb and disc spicule quasi-periodic recurrences produced by overlapping effects, we present a simulation model assuming quasi- random positions of spicules. We also allow a set number of spicules with different physical properties (such as: height, lifetime and tilt angle as shown by an individual spicule) occurring randomly. Results of simulations made with three different spatial resolutions of the corresponding frames and also for different number density of spicules, are analyzed. The wavelet time/frequency method is used to obtain the exact period of spicule visibility. Results are compared with observations of the chromosphere from i/ the Transition Region and Coronal Explorer (TRACE) filtergrams taken at 1600 angstrom, ii/ the Solar Optical Telescope (SOT) of Hinode taken in the Ca II H-line and iii/ the Sac-Peak Dunn's VTT taken in H? line. Our results suggest the need to be cautious when interpreting apparent oscillations seen in spicule image sequences when overlapping is present, i.e.; when the spatial resolution is not enough to resolve individual components of spicules. Title: New Technology Solar Coronagraphs Authors: Koutchmy, S.; Bazin, C.; Damé, L.; Rochain, S.; Tavabi, E. Bibcode: 2012EAS....55..375K Altcode: We present the Mirror Advanced technology Coronagraph (MAC) as a new generation solar telescope to be put at suitable high altitude coronal sites in order to resolve modern problems of solar physics, like the origin of the heating of the chromosphere and of the corona, the analysis of the mesospheric layers of the solar atmosphere and the effects of shearing the photospheric magnetic fields on the dynamics of the upper coronal layers. Title: SOHO observations of oscillatory motions in an eruptive filament: Intensity and velocity variations Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J. Bibcode: 2011sf2a.conf..369B Altcode: The variations in intensity and velocity inside an eruptive filament, observed on May 30, 2003 with CDS and EIT on-board SOHO, are analysed in the transition region He I line and the coronal Mg X line. Vertical oscillating motions of the filament with damped velocity oscillations before its disappearance are revealed. The link between theses oscillations, the flaring regions nearby and the filament eruption is investigated. Title: The helium shells of HeI and HeII at solar minimum: New results from eclipse flash spectra of 2008- 2010 Authors: Bazin, C.; Koutchmy, S.; Lamy, P. Bibcode: 2011sf2a.conf..203B Altcode: Flash spectra taken at high frame rate during the total solar eclipse of August 1st 2008 in Siberia and during the July 11th 2010 in French Polynesia are compared in the context of the quiet Sun near the minimum of activity. They both reveal the weak Paschen α 468.6 nm ionized helium line, seen as a helium shell in layers up to the 8 Mm heights. The preliminary evaluated effective height of the He I 4713 shell is 1.8 Mm and it is approximately 2.0 Mm for the He II 4686 emissions outside polar regions. These lines can be measured only in eclipse conditions, when the parasitic scattered light is negligible for very low solar fluxes corresponding to the coronal levels. Many faint lines are also seen in emission such as Ba +, Ti +, Fe +, but with a much lower radial extension. They were observed to be superposed to F-lines when defining the solar limb using the continuum background. A cartoon is proposed to describe the structuration of these low layers and to illustrate the contribution of the magnetic field. These observations are important new insights for understanding (i) the magnetic field inference in the very low layers of the solar transition region and (ii) the ionisation mechanisms producing the big jump of the temperature towards the corona, including the source of heating. Title: The Three-Dimensional Behavior of a Twisted Flux Tube Expanding in the Corona: Reconnection, Writhe, and Jets Authors: Tavabi, Ehsan; Koutchmy, Serge; Ajabshirizadeh, Ali Bibcode: 2011ITPS...39.2436T Altcode: 2011arXiv1103.3814T We discuss some aspects of magnetic reconnection which could help in understanding many aspects of magnetic plasma interactions. We will show that the helical structure often observed in polar jets is a natural consequence of magnetic helicity conservation in 3D reconnection driven by a collision of two parts of an emerging flux tube within the single emerged loop. We perform 3D simulations by solving the time-dependent, ideal MHD equations with a uniform initial twist. We deduce that the emergence of highly twisted magnetic flux introduces several null points, which in turn causes reconnection between opposite directions of magnetic field within a single loop at nearest part and the release of the trapped twist in the form of a helical jet-like emission. Title: Oscillatory motions observed in eruptive filaments Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S.; Pouget, G.; Solomon, J. Bibcode: 2011A&A...533A..96B Altcode: 2011arXiv1107.0596B Context. The origin of the variable component of the solar wind is of great intrinsic interest for heliophysics and spaceweather, e.g. the initiation of coronal mass ejections and the problem of mass loss of all stars. It is also related to the physics of coronal neutral sheets and streamers, which occur above lines of magnetic polarity reversal. Filaments and prominences correspond to the cool coronal component of these regions.
Aims: We examine the dynamical behaviour of these structures where reconnection and dissipation of magnetic energy in the turbulent plasma are occurring. The link between the observed oscillatory motions and the eruption occurrence is investigated in detail for two different events.
Methods: Two filaments were analysed using two different datasets: time series of spectra using a transition region line (He I at 584.33 Å) and a coronal line (Mg X at 609.79 Å) measured with CDS on-board SOHO, observed on May 30, 2003, and time series of intensity and velocity images from the NSO/Dunn Solar Telescope in the Hα line on September 18, 1994 for the other. The oscillatory content was investigated using Fourier transform and wavelet analysis and compared to different models.
Results: In both filaments, oscillations are clearly observed, in intensity and velocity in the He I and Mg X lines, in velocity in Hα, with similar periods from a few minutes up to 80 min, with a main range from 20 to 30 min, simultaneously with eruptions. Both filaments exhibit vertical oscillating motions. For the filament observed in the UV (He I and Mg X lines), we provide evidence of damped velocity oscillations, and for the filament observed in the visible (Hα line), we provide evidence that parts of the filament are oscillating, while the filament is moving over the solar surface, before its disappearance. Title: A statistical analysis of the SOT-Hinode observations of solar spicules and their wave-like behavior Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A. Bibcode: 2011NewA...16..296T Altcode: 2010arXiv1004.1692T Spicules are an important very dynamical and rather cool structure extending between the solar surface and the corona. They are partly filling the space inside the chromosphere and they are surrounded by a transition thin layer. New space observations taken with the SOT of the Hinode mission shed some light on their still mysterious formation and dynamics. Here we restrict the analysis to the most radial and the most interesting polar spicules situated at the base of the fast solar wind of coronal holes. We consider a first important parameter of spicules as observed above the solar visible limb: their apparent diameter as a function of the height above the limb which determines their aspect ratio and leads to the discussion of their magnetic origin using the flux tube approximation. We found that indeed spicules show a whole range of diameters, including unresolved "interacting spicules" (I-S), depending of the definition chosen to characterize this ubiquitous dynamical phenomenon occurring into a low coronal surrounding. Superposition effects along the line of sight have to be taken into account in order to correctly measure individual spicules and look at I-S. We take advantage of the so-called mad-max operator to reduce these effects and improve the visibility of these hair-like features. An excellent time sequence of images obtained above a polar region with the Hinode SOT through the HCaII filter with a cadence of 8 s was selected for analysis. 1-D Fourier amplitude spectra (AS) made at different heights above the limb are shown for the first time. A definite signature in the 0.18-0.25 Mm range exists, corresponding to the occurrence of the newly discovered type II spicules and, even more impressively, large Fourier amplitudes are observed in the 0.3-1.2 Mm range of diameters and spacing, in rough agreement with what historical works were reporting. Additionally, some statistically significant behavior, based on AS computed for different heights above the limb, is discussed. "Time slice or x- t diagrams" revealing the dynamical behavior of spicules are also analyzed. They show that most of spicules have multiple structures (similarly to the doublet spicules) and they show impressive transverse periodic fluctuations which were interpreted as upward kink or Alfven waves. Evidence of the helical motion in spicules is now well evidenced, the typical periods of the apparent oscillation being around 120 s. A fine analysis of the time-slice diagram as a function of the effective heights shows an interesting new feature near the 2 Mm height. We speculate on the interpretation of this feature as being a result of the dynamical specificities of the spicule helical motion as seen in these unprecedented high resolution HCaII line emission time series. Title: Null-Point Oscillations of Chromospheric Large Cool Jets Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A. Bibcode: 2011AIPC.1356...99T Altcode: In addition of the whip-like behavior, null-point motions in the reconnection site can excite transversal oscillation along the magnetic dense jets, which was called the kink mode wave, and also this mode can evolve into Alfven wave after its propagation into the more homogeneous medium. The study of X-ray jets is an important topic to understand the heating of the solar corona and the origin of the fast wind. The recently launched Hinode mission permitted to observe the cool proxies of these jets with an unprecedented high spatial resolution of 120 km on the Sun. We selected a high cadence sequence of SOT (Hinode) observations taken with both the HCaII and the Hα filter to look at the details of the dynamics revealed by a large jet event. Both wavelet and amplitude spectra analysis were used to analyze the observed kink wave and the time variations of intensities during the event. The results are discussed in the frame of different models implying reconnections with the inference of the dynamical phenomena occurring in the vicinity of several null points including the oscillatory behavior. Title: Contribution to the modeling of solar spicules Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A. Bibcode: 2011AdSpR..47.2019T Altcode: 2011arXiv1101.2520T Solar limb and disk spicule quasi-periodic motions have been reported for a long time, strongly suggesting that they are oscillating. In order to clear up the origin and possibly explain some solar limb and disk spicule quasi-periodic recurrences produced by overlapping effects, we present a simulation model assuming quasi-random positions of spicules. We also allow a set number of spicules with different physical properties (such as: height, lifetime and tilt angle as shown by an individual spicule) occurring randomly. Results of simulations made with three different spatial resolutions of the corresponding frames and also for different number density of spicules, are analyzed. The wavelet time/frequency method is used to obtain the exact period of spicule visibility. Results are compared with observations of the chromosphere from (i) the Transition Region and Coronal Explorer (TRACE) filtergrams taken at 1600 Å, (ii) the Solar Optical Telescope (SOT) of Hinode taken in the Ca II H-line and (iii) the Sac-Peak Dunn's VTT taken in Hα line. Our results suggest the need to be cautious when interpreting apparent oscillations seen in spicule image sequences when overlapping is present, i.e., when the spatial resolution is not enough to resolve individual components of spicules. Title: The He I and He II chromospheric shells and the Transition Region Authors: Bazin, Cyril; Koutchmy, Serge; Tavabi, Ehsan Bibcode: 2010arXiv1008.0404B Altcode: Total eclipse observations were performed in 2008 and 2009 to study the He I and He II shells near the 1 Mm heights above the solar limb. They suggest that the corona penetrates deep into the chromosphere following magnetic chanels. Thanks to the use of a fast CCD camera, the observation of a second ionized helium shell is evidenced for the first time. The transition region is then seen at very low altitude where spicules are emerging. Spicule feet are also discussed, using the best resolution SOT/Hinode HCaII images processed with the non linear operator Madmax to look at details of this ubiquitous part of the solar atmosphere. Title: Coronal Fine Linear Rays: Are They Fast Streams From Active Regions? Authors: Koutchmy, Serge; Lamy, Philippe; Viladrich, Christian; Filippov, Boris; Nikoghossian, Arthur; Golub, Leon Bibcode: 2010AIPC.1216..339K Altcode: Eclipse observations of the W-L corona show linear rays above active regions at times of solar maximum. We show that these linear rays are also observed in the field-of-view of the C2-LASCO coronagraph, in perfect correspondence with the eclipse results. A selected prominent case taken from the 2001 eclipse observation in Angola is analysed with several different methods, including the use of a synoptic map constructed using SoHO/LASCO C2 images. A clear signature of time variations near the eclipse observation is detected, suggesting that at least some parts of the beam are collimated. These observations strongly suggest high speed streams that apparently ignore the potential large scale coronal magnetic field rooted rather low in the corona. A possible origin is the neutral magnetic points located above the active region. Several mechanisms exist to explain how the plasma is accelerated in these regions to large quasi-relativistic velocities, possibly related to the occurrence of type III radio bursts. We point out a curious analogy with phenomena occurring inside coronal holes. Title: Is there a flare-like precursor of EUV waves and CMEs ? Authors: Filippov, Boris; Podladhikova, Olena; Golub, Leon; Koutchmy, Serge Bibcode: 2010cosp...38.2889F Altcode: 2010cosp.meet.2889F Filament eruptions with a flux rope are usually considered the cause of CMEs. It is however not clear why after reaching some critical height, the filament suddenly erupts and whether or not we always have a one to one correspondence. Additional factors can be considered, starting with the ubiquitous chromospheric (in H) and/or coronal running disturbances or waves seen with EUV and SXR filtergrams collected by different missions, including the newly operated SWAP of Proba-2, the GOES 14 SXR patrol instrument and the high resolution XRT of Hinode. The eruptions seem to be induced by a well focused but large explosive event originating from an unresolved region presumably situated rather low in the atmosphere, near the chromosphere-corona interface. A similar picture can be drawn from a new type of coronal flare observed with the XRT of Hinode outside of any active region and without any precursor. Both the quasi-thermal coronal flare and the large dynamical phenomenon originate or start from a very small unresolved region. We discuss the difference in mass, momentum and amount of energy involved for 2 selected events (25 Dec 2006 with XRT and 5 Feb 2010 with SWAP and other instruments) that are well documented. We want to examine at what height in the atmosphere these events are triggered and what is the relevance to the CME phenomenon, without speculating on the unresolved magnetic field context. The events were observed at solar activity minimum without any complication resulting from numerous active regions being present on the disk. Title: 5 min loop oscillations and propagating waves in the upper solar atmosphere Authors: Veselovsky, Igor; Koutchmy, Serge Bibcode: 2010cosp...38.2942V Altcode: 2010cosp.meet.2942V Solar resonant P-mode oscillations in the 5min range are excited by the convective motions under its visible surface. Those oscillations are mostly known to be trapped acoustic Eigen-modes and waves propagating near the temperature minimum. They are readily observed in velocity and temperature (intensity) variations at the photospheric level, but not too often in the chromosphere and the corona, where they are documented only under some specific favor-able conditions when waves are guided and transformed by the concentrated magnetic field. Their quantitative role in the physics of the solar atmosphere, its heating and plasma acceler-ation is still unclear. It is due to their mode transformation, reflection and dissipation during the propagation from the source regions which are also not well determined. Estimates of the propagating and standing parts are still not certain. Those estimates are needed for the en-ergy budget evaluations in the solar atmosphere. Observations of 5-min oscillations in the solar corona are scarce and puzzling because of the poor knowledge of many relevant physical param-eters. We discuss the suggested interpretations of available "Hinode" data as well as of recent observations onboard the "Coronas -Photon" satellite in 2009 and indicate their insufficiency for obtaining correct one-valued solutions. We point out the impossibility to identify and split the modes in the inhomogeneous and time variable solar atmosphere because of non-linearity in many instances. Finally, we analyze the question of the role of other waves and non-wave structures linking the levels in the solar atmosphere and conclude that this role is generally increasing with the height. This also means that quasi-steady models of the solar wind outflow formation are of very limited usefulness. Title: Jet phenomena above null points of the coronal magnetic field Authors: Filippov, B.; Koutchmy, S.; Golub, L. Bibcode: 2009Ge&Ae..49.1109F Altcode: Short-lived plasma jets of various scales, from giant X-ray jets more than 300 Mm in extent to numerous small jets with sizes typical of macrospicules, are the phenomena observed in the solar corona in extreme ultraviolet and X-ray emission. Small jets are particularly prominent in polar coronal holes. They are close neighbors of tiny bright loops and coincide in time with their sudden brightening and increase in size. The geometric shape of the jets and their location suggest that they arise near singular null points of the coronal magnetic field. These points appear in coronal holes due to the emergence of small bipolar or unipolar magnetic structures within large-scale unipolar cells. Polar jets show a distinct vertical plasma motion in a coronal hole that introduces significant momentum and mass into the solar wind flow. Investigating the dynamics of polar jets can elucidate certain details in the problem of fast solar wind acceleration. Title: Propriétés photométriques d'étalons fabry-pérot pour la raie halpha. application à l'analyse de la frange chromosphérique du soleil. Title: Propriétés photométriques d'étalons fabry-pérot pour la raie halpha. application à l'analyse de la frange chromosphérique du soleil. Title: Photometric properties of solar halpha fabry-perot etalons. application to the analysis of the chromospheric fringe. Authors: Bazin, C.; Koutchmy, S. Bibcode: 2009O&T....74....2B Altcode: We consider the use of the commercially available Fabry-Perot etalons (FP) for the imaging of the solar chromosphere in the Ha line of hydrogen. Three etalons of 40, 60 and 90 mm of diameter were evaluated and accurately analysed. At normal incidence the maximum transmission wavelength is 656.285 nm for the 60 and 40 mm etalons FP. The finesse has been found to be 13.3 for the FP 60mm, 8.7 for the FP 40 and 13.9 for the FP 90 mm. Shifts of the central wavelength as a function of the incidence angle were accurately measured. Polynomial curves giving the variation of the transmitted central wavelength when using a quasi-parallel beam from a point-like source are presented. Calibrations were done with a photometric accuracy using i/ a 16 bits CCD camera; ii/ a Littrow spectrograph of a spectral power 110000, a linear dispersion giving a .0058 nm/ pixel resolution and iii/ an artificial Sun with different angular extension used as a light source and iv/ adjustable in position optical components. The precise laboratory wavelength calibration was performed using a low pressure deuterium spectral lamp simultaneously illuminating the entrance slit. The variations of the FWHM of the transmission curves as a function of the incidence angle are also given for a typical etalon. Consequences resulting from the use of a significant aperture/ratio are tentatively discussed for the first time. An application to a precise solar photometric work using filtergrams is illustrated, with emphasis on the photometric accuracy resulting from the use of such etalons put before the entrance aperture of the imaging telescope. Monochromatic images of the solar chromospheric shell near the limbs were made, in order to deduce the variation of its thickness at poles and equator in order to measure the prolateness effect during this current minimum of solar activity (2009). Title: Isolated quasi-axisymmetric sunspots Authors: Koutchmy, Serge; Le Piouffle, Vincent Bibcode: 2009IAUS..259..227K Altcode: We briefly review the question of the origin, during a sunspot cycle, of well isolated sunspots. This includes big sunspots like the one observed in Nov. 2006. An overall axi-symmetric morphology is not perfectly observed when the morphological details of both the umbra and of the penumbra are considered. This is especially the case of umbral dots always present inside the core of a sunspot and also of penumbral filaments with non radial parts. However, the distribution of the surrounding fields, including deep layers, the occurrence of persistent coherent running penumbral waves, the magnetic moat behavior, the bright ring phenomena, etc. seem to justify a revival of the naive former but revised (converging motions are considered) Larmor model of a sunspot (as suggested by Lorrain et al. 2006). To discuss the “emergence” of single isolated sunspots from deep layers we performed a quasi-statistical analysis limited to cycle 23. It is based on MDI data taken in the continuum, using the accompanying magnetograms to check our assertion. Surprisingly, single sunspots are definitely and preferably found to occur at low latitude and during the descending branch of the cycle. To explain our observations we speculate about the behavior of the deeply seated magnetic loop, following the original idea of H. Alfven (with whirl rings which follow the global dipolar field when approaching the surface). It could lead to a closed loop approximately orthogonal to the local radius, similar to “smoke rings” arriving at the surface of the Sun and sometimes also called a plasmoid. The ring will only very weakly feel the destabilizing Coriolis force, when emerging at very low latitudes, which seems consistent with our observations. Title: Scientific requirements for future spatially resolved white-light and broad-band high-cadence observations of the Sun Authors: Veselovsky, Igor S.; Koutchmy, Serge Bibcode: 2009AdSpR..43..995V Altcode: Several important issues are open in the field of solar variability and they wait their solution which up to now was attempted using critical ground-based instrumentations. However, accurate photometric data are attainable only from space. New observational material should be collected with high enough spatial and spectral resolution, covering the whole visible range of the electromagnetic spectrum as well infrared and ultraviolet to reconstruct the total solar irradiance: (1) the absolute contributions of different small-scale structural entities of the solar atmosphere from the white light flares and from micro-flares are still poorly known; (2) we do not know the absolute contributions of different structural elements of the solar atmosphere to the long-term and to the cyclic variations of the solar irradiance, including features of the polar regions of the Sun; (3) the variations of the chromospheric magnetic network are still poorly evaluated; (4) only scarce information is available about the spectral variations of different small-scale features in the high photosphere. Variability of the Sun in white light can be studied with higher spectral, spatial and time resolution using space-born telescopes, which are more appropriate for this purpose than ground based observatories because of better seeing conditions, no interference of the terrestrial atmosphere and a more precise calibration procedure. Scientific requirements for such observations and the possible experimental tools proposed for their solution. Suggested solar studies have broader astrophysical importance. Title: ASPIICS, a giant externally occulted coronagraph for the PROBA-3 formation flying mission Authors: Vivès, S.; Lamy, P.; Koutchmy, S.; Arnaud, J. Bibcode: 2009AdSpR..43.1007V Altcode: Formation flying opens new perspectives for coronal physics, and allow to conceive giant, externally occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft. ASPIICS (Association de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne Solaire) is a mission proposed to ESA in the framework of the PROBA-3 program of formation flying which is presently in phase A, to exploit this technique for coronal observations. ASPIICS is composed of a single coronagraph which performs high spatial resolution imaging of the corona as well as 2-dimensional spectroscopy of several emission lines from the coronal base out to 3 R⊙. The selected lines allow to address different coronal regions: the forbidden line of Fe XIV at 530.285 nm (coronal matter), Fe IX/X at 637.4 nm (coronal holes), HeI at 587.6 nm (cold matter). An additional broad spectral channel will image the white light corona so as to derive electron densities. The classical design of an externally occulted coronagraph is adapted to the detection of the very inner corona as close as 1.01 R⊙ and the addition of a Fabry-Perot interferometer using a so-called " étalon". This paper is dedicated to the description of the optical design and its critical components: the entrance optics and the Fabry-Pérot interferometer. ASPIICS will address the question of coronal heating and of the role of waves by characterizing propagating fluctuations (waves and turbulence) in the solar wind acceleration region and by looking for oscillations in the intensity and Doppler shift of spectral lines. The combined imaging and spectral diagnostics capabilities available with ASPIICS will allow to map the velocity field of the corona both in the sky plane (directly on the images) and along the line-of-sight by measuring the Doppler shifts of emission lines. We will attempt to determine how the different components of the solar wind, slow and fast are accelerated. ASPIICS will observe the corona during the maximum of solar activity, insuring the detection of many Coronal Mass Ejections (CMEs). By rapidly alternating high resolution imaging and spectroscopy, CMEs will be thoroughly characterized. In addition, ASPIICS will attempt to characterize the topology of the magnetic field in the corona. Title: X-Ray Jet Dynamics in a Polar Coronal Hole Region Authors: Filippov, Boris; Golub, Leon; Koutchmy, Serge Bibcode: 2009SoPh..254..259F Altcode: 2007arXiv0711.4320F New X-ray observations of the north polar region taken from the X-ray Telescope (XRT) of the Hinode spacecraft are used to analyze several time sequences showing small loop brightenings with a long ray above. We focus on the formation of the jet and discuss scenarios to explain the main features of the events: the relationship with the expected surface magnetism, the rapid and sudden radial motion, and possibly the heating, based on the assumption that the jet occurs above a null point of the coronal magnetic field. We conclude that 2-D reconnection models should be complemented in order to explain the observational details of these events and suggest that alternative scenarios may exist. Title: Magneto-acoustic wave oscillations in solar spicules Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S. Bibcode: 2009Ap&SS.319...31A Altcode: 2008arXiv0806.1418A Some observations suggest that solar spicules show small amplitude and high frequency oscillations of magneto-acoustic waves, which arise from photospheric granular forcing. We apply the method of MHD seismology to determine the period of kink waves. For this purposes, the oscillations of a magnetic cylinder embedded in a field-free environment is investigated. Finally, diagnostic diagrams displaying the oscillatory period in terms of some equilibrium parameters are provided to allow a comparison between theoretical results and those coming from observations. Title: Une grande éclipse totale de soleil le 22 juillet 2009 Title: Une grande éclipse totale de soleil le 22 juillet 2009 Title: The great total eclipse of july 22, 2009; Authors: Koutchmy, S.; Mouette, J.; Bazin, C. Bibcode: 2008O&T....71....2K Altcode: Planning observations of the Total Eclipse of July 22, 2009. We shortly review the circumstances of this forthcoming big Solar Total Eclipse, giving references, ephemeris and maps to show the sites where to go for observing it in good conditions. The probabilities of a clear sky at time of totality are discussed using 2 different sources of statistical analysis and the conditions for making an enjoyable eclipse trip are commented. We also briefly review what can be done during the totality, taking into account the scientific priorities existing in coronal physics and using an example of what has been outstandingly done at the last 2008 eclipse as well as the general interest of the eclipse phenomenon. Finally we give in Annexe an overview of the post-eclipse projected international conference organized by the Chinese Academy of Sciences, which will take place in Souzhou, including its preliminary scientific program. Title: Causal relationships between eruptive prominences and coronal mass ejections Authors: Filippov, B.; Koutchmy, S. Bibcode: 2008AnGeo..26.3025F Altcode: 2007arXiv0711.4752F A close association between eruptive prominences and CMEs, both slow and fast CMEs, was reported in many studies. Sometimes it was possible to follow the material motion starting from the prominence (filament) activation to the CME in the high corona. Remnants of the prominence were found in the bright core of the CME. However, detailed comparisons of the two phenomena reveal problems in explaining CMEs as a continuation of filament eruptions in the upper corona. For example, the heliolatitudes of the disappeared filaments and subsequent coronal ejections sometimes differ by tens of degrees. In order to clear up the problems appearing when considering this association EP-CME, we tentatively analyse the more general question of the dynamics of the generic magnetic flux rope. Prominences and filaments are the best tracers of the flux ropes in the corona long before the beginning of the eruption. A twisted flux rope is held by the tension of field lines of photospheric sources until parameters of the system reach critical values and a catastrophe happens. We suggest that the associated flux rope height above the photosphere is one of these parameters and that it is revealed by the measured height of the filament. 80 filaments were analysed and we found that eruptive prominences were near the so-called limit of stability a few days before their eruptions. We suggest that a comparison of actual heights of prominences with the calculated critical heights from magnetograms could be systematically used to predict filament eruptions and the corresponding CMEs. Title: Small-scale Coronal Jets Authors: Koutchmy, S.; Filippov, B.; Golub, L. Bibcode: 2008ESPM...12.2.93K Altcode: Jet-like events are observed on different scales in the solar corona in EUV and X-rays. They range from gigantic coronal X-ray jets greater than 300 Mm in length to small but numerous jetlets. Polar coronal holes show a significant activity manifested in small loop brightenings and jetlet formation. Geometrical shape of the jetlets and their position indicate that they appear near the singular points of the magnetic field, namely, null points or X-points. These nulls arise due to the interaction between new emerging small dipoles and large-scale magnetic field of the coronal hole. The jetlets reveal some real observable vertical mass motion inside the coronal hole. It is difficult to measure the radial velocity of plasma within the jetlets but it seems large enough to significantly contribute as a large momentum into the solar wind. Finally jetlets could serve as injectors to the process of the solar fast wind acceleration. We believe that similar but even smaller processes could very often happen at smaller scale in the chromosphere near emerging magnetic ephemeral regions forming numerous jetlets of the upper chromosphere. They form the upper chromosphere and follow the direction of the surrounding magnetic field. At the epoch of low activity, the difference in the large-scale structure of the polar magnetic field and that of the low latitude quiet region magnetic field results in a prolateness of the chromosphere. Title: Resolution Effect in the Solar Spicules Oscillations Authors: Ajabshirizadeh, A.; Koutchmy, S.; Tavabi, E. Bibcode: 2008ESPM...12.2.44A Altcode: In order to explain solar limb spicule periodic recurrence, we have adopted a simulation model based on random position of spicule on the Sun limb, we allow a set number of spicules with different physical properties (such as height, lifetime and tilt angle) randomly occur along the Z-axis and after reaching the maximum length falling back to the solar surface.

This simulation has been applied for three different resolutions of frames and then analysis spicule visibility using the wavelet time/frequency method to obtain the exact period for them.

Finally, the simulation results have been compared with observations. This investigation is prompted by observations of chromosphere from the Transition Region and Coronal Explorer (TRACE) at 1600 Ångstrom , Solar Optical Telescope (SOT) on Hinode revealing at Ca II H-line and Sac-Peak H-alpha line. Title: About Isolated Quasi-axi-symetric Sunspots: Description, Statistical Analysis and Theoretical Modelling Authors: Koutchmy, S.; Le Piouffle, V. Bibcode: 2008ESPM...12..3.6K Altcode: We briefly review the question of the occurrence, during a sunspot cycle, of well isolated sunspots. This includes big sunpots like the one observed in Nov. 2006. We note that a quasi- axi-symmetric morphology is clearly NOT observed when the morphological details of both the umbra and penumbra are considered. However, the occurrence of persistent coherent penumbral waves, the magnetic moat behavior, the bright ring phenomena, etc. seem to justify a revival of the former and revised Larmor model of a sunspot (the so-called the P. Lorrain model).

To discuss the "emergence" of single sunspots from deep layers, we performed statistical analysis limited to cycle 23 based on MDI images taken in the continuum and using magnetograms. Surprisingly, single sunspots are definitely and preferably found to occur at low latitude and during the descending branch of the cycle.

To explain our observations, we suggest the occurrence of magnetic loops orthogonal to the local radius, similar to "smoke rings" arriving at the surface of the Sun. The rings will only very slightly feel the Coriolis force at low latitudes, which is consistent with our observations. Title: New perspectives in solar coronagraphy offered by formation flying: from PROBA-3 to Cosmic Vision Authors: Lamy, P.; Vivès, S.; Damé, L.; Koutchmy, S. Bibcode: 2008SPIE.7010E..1HL Altcode: Formation flying opens new perspectives in solar physics, and allow to conceive giant, externally-occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft at a distance of hundred meters. Conditions close to those of a solar total eclipse can then be achieved offering the capability of imaging the solar corona down to the limb at very high spatial resolution. ASPIICS (Association de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne Solaire) is a mission proposed to ESA in the framework of its PROBA-3 demonstration program of formation flying which is presently in phase A. ASPIICS is a single coronagraph which will perform both high spatial resolution imaging of the solar corona as well as 2-dimensional spectroscopy of several emission lines from the coronal base out to 3 R\beye using a Fabry-Pérot étalon interferometer. The classical design of an externally-occulted coronagraph is adapted to the formation flying configuration allowing the detection of the very inner corona as close as 0.01 R\beye from the solar limb. Super-ASPIICS is an even more ambitious instrument part of the scientific payload of HiRise, the High Resolution Imaging and Spectroscopy Explorer proposed to ESA in the framework of its Cosmic Vision program. With an increased inter-satellite distance of 280 m, an aperture of 300 mm, a spectral domain extending from the ultraviolet to the near-infrared, and spectroscopic capabilities, Super-ASPIICS will offer unprecedented diagnostic capabilities, including the measurement of coronal magnetic fields. Title: Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare, and EUV dimming Authors: Koutchmy, S.; Slemzin, V.; Filippov, B.; Noens, J. -C.; Romeuf, D.; Golub, L. Bibcode: 2008A&A...483..599K Altcode: 2008arXiv0801.2746K Aims: Coronal mass ejections or CMEs are large dynamical solar-corona events. The mass balance and kinematics of a fast limb CME, including its prominence progenitor and the associated flare, will be compared with computed magnetic structures to look for their origin and effect.
Methods: Multi-wavelength ground-based and spaceborne observations are used to study a fast W-limb CME event of December 2, 2003, taking into account both on and off disk observations. Its erupting prominence is measured at high cadence with the Pic du Midi full Hα line-flux imaging coronagraph. EUV images from SOHO/EIT and CORONAS-F/SPIRIT space instruments are processed including difference imaging. SOHO/LASCO images are used to study the mass excess and motions. Computed coronal structures from extrapolated surface magnetic fields are compared to observations.
Results: A fast bright expanding coronal loop is identified in the region recorded slightly later by GOES as a C7.2 flare, followed by a brightening and an acceleration phase of the erupting material with both cool and hot components. The total coronal radiative flux dropped by ~7% in the 19.5 nm channel and by 4% in the 17.5 nm channel, revealing a large dimming effect at and above the limb over a 2 h interval. The typical 3-part structure observed 1 h later by the Lasco C2 and C3 coronagraphs shows a core shaped similarly to the eruptive filament/prominence. The total measured mass of the escaping CME (~1.5×1016 g from C2 LASCO observations) definitely exceeds the estimated mass of the escaping cool prominence material although assumptions made to analyze the Hα erupting prominence, as well as the corresponding EUV darkening of the filament observed several days before, made this evaluation uncertain by a factor of 2. This mass budget suggests that the event is not confined to the eruption region alone. From the current free extrapolation we discuss the shape of the magnetic neutral surface and a possible scenario leading to an instability, including the small scale dynamics inside and around the filament. Title: En attendant l'éclipse totale de soleil du 1er août 2008 Title: En attendant l'éclipse totale de soleil du 1er août 2008 Title: Planning to observe the total solar eclipse of aug. 1st 2008 Authors: Koutchmy, S. Bibcode: 2008O&T....69...36K Altcode: We shortly review the circumstances of this forthcoming 2008 Solar Total Eclipse, giving ephemeris, references and maps to show the sites where to go for observing it in good conditions. The probabilities of a clear sky at time of totality are discussed. We also briefly review what can be done during the totality, taking into account i/ the scientific priorities existing in coronal physics and Heliophysics; ii/ the general interest of the eclipse phenomenon. References to planned scientific "2008-eclipse" meetings in China and Russia are given. Title: Magneto-Acoustic Wave (KINK) Oscillations In Solar Spicules Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S. Bibcode: 2008mear.confE..22A Altcode: No abstract at ADS Title: Wavelet analysis of solar macro-spicule recurrences Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S. Bibcode: 2008NewA...13...93A Altcode: We looked at the temporal behavior of intensity variations of spicules and macro-spicules observed at the solar limb by TRACE (transition region and coronal explorer) EUV telescope in the 1600 Å channel. Using wavelet analysis technique we got evidence of spicule oscillations. The time-frequency analysis provided by the wavelet analysis shows a temporal behavior of spicules with recurrences at periods of about 210-260 s with a typical lifetime of 10 min. Finally, we shortly discuss two scenarios regarding the possible origin of spicule oscillations. Title: The dynamic solar Corona : violent phenomena of Sun. Authors: Koutchmy, S. Bibcode: 2008LAstr.122c..16K Altcode: No abstract at ADS Title: Solar Astrophysics, Interferometry, and Coronagraphy at DomeC/Concordia Authors: Damé, L.; Amans, J. -P.; Dournaux, J. -L.; Koutchmy, S.; Lamy, P.; Preumont, A. Bibcode: 2008EAS....33..105D Altcode: Excellent seeing, coronal conditions, and very low IR thermal background are qualities of the Dome C/Concordia station site that will allow unique solar astrophysics science. We review the science case for inner corona observations (onset of the coronal heating mechanism still poorly understood) and the promises of high angular resolution to disentangle the possible mechanisms at work between waves, convection, and reconnection in this particularly magnetically structured solar atmosphere between the high chromosphere and inner corona. For coronagraphy, IR and high resolution possibilities, Dome C is a case by itself between classical ground-based sites and space opportunities. Telescopes from 50 cm (coronagraphy oriented) to 4 m (full high resolution advantage including IR access) are proposed to benefit from these remarkable observing capabilities. Using 3×O50 cm off-axis telescopes, we first propose a medium size facility (1.4 m equivalent telescope) for very high resolution access, ADSIIC (Antarctica Demonstrator of Solar Interferometric Imaging & Coronagraphy), before the ultimate 9-telescope Solar Facility equivalent to a 4 m diameter telescope: A-FOURMI (Antarctica 4 m Interferometer). Finally, 30 m tower designs and their logistics using standard containers and elementary elements of 6 m maximum length, are presented and discussed. These towers are indeed of general interest also for the other optical and IR telescopes intended for Dome C/Concordia, allowing to get over most of the turbulent ground layer and to reach the best possible permanent seeing conditions (better than half an arcsec). Title: Old and New Aspects of Prominence Physics from Coronal Observations Authors: Koutchmy, S.; Filippov, B.; Lamy, P. Bibcode: 2007ASPC..368..331K Altcode: Classical W-L eclipse observations at typical spatial resolution of 10 arcsec show dark cavities surrounding prominences. Images at higher spatial resolution processed with a spatial filter reveal small dynamical cool clouds moving inside the inner corona around prominences. More recently EIT/SoHO observations taken using the 304 Å channel showed He+ prominences sometimes not seen in cooler lines. TRACE movies of the Fe IX and XI emissions where prominences are seen in absorption also bring appreciable informations on the dynamical surrounding of prominences, without showing obvious correlations between prominence and coronal structures. Accordingly, we re-examine the significance of the cavity and propose a possible interpretation as magnetic interlaced 3-D flux ropes and loops evacuating the corona, in addition to twisted flux ropes where the prominence plasma is condensing. Future space missions like ASPIICS should pay more attention to cavities and emptiness, to coronal dynamics around prominences, in order to resolve the long-standing problem of the origin of prominences and perhaps, perform a new diagnostic of the erupting process responsible for many CMEs. Title: Coronagraphic Broad-Band Hα Observations 1998 -- 2000 Authors: Meunier, N.; Noëns, J. -C.; Romeuf, D.; Koutchmy, S.; Jimenez, R.; Wurmser, O.; Rochain, S. Bibcode: 2007ASPC..368..351M Altcode: Broad-band full-limb Hα images of the inner corona were obtained since the beginning of the solar cycle 23 using one of the Pic-du-Midi coronagraph. We developed a tool to process the complete set of stored images and to automatically extract the properties and evolutions of the observed cold H I coronal structures over a large range of sizes and light fluxes, from small jets and/or spikes to large prominences. The paper describes the recognition techniques implemented in our software and discusses its use. Then we present some new results following a statistical analysis of the occurrence of structure parameters applied to a large sample of observations. It illustrates the capabilities of this software when applied to our database. Strong activity-asymmetries over the solar poles are shown, confirming similar results from elsewhere. We also discuss the distribution of relative light fluxes of these structures over a wide range of sizes. See also http://bass2000.bagn.obs-mip.fr. Title: On the Dynamic Nature of the Prolate Chromosphere Authors: Filippov, B.; Koutchmy, S.; Vilinga, J. Bibcode: 2007ASPC..368..177F Altcode: The upper edge of the solar chromosphere looks not like a perfect circle in some spectral lines. It is prolate in the South-North direction at the epoch of minimum solar activity and nearly spherically symmetrical at the maximum phase. We attribute the effect to the dynamical nature of the upper chromosphere, which consists of a large number of small cool jets (jetlets) ascending into the corona. A proposed simple geometric model can explain the effect of the prolateness of the solar chromosphere. Due to the dynamic nature of the solar atmosphere above the 2 Mm level, the magnetic field is considered to play a very important role in the density distribution with the height, guiding the mass flows along the field lines. The difference of the magnetic field topology in the polar and the equatorial regions leads to different heights of the chromospheric limb. We could not resolve a source region of an individual jetlet, however similar but larger structures are visible in EUV coronal lines. We present an example of the jet formation obtained by TRACE in the 171 Å channel. Field aligned motion arises above the null point created in the corona by the emerging magnetic bipole. The scale of bipole is large enough to recognize the saddle structure around the 3D null point in the TRACE images. We believe that similar but smaller processes could happen very often at smaller scale in the chromosphere near emerging magnetic ephemeral regions forming numerous jetlets of the upper chromosphere. Title: The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona Authors: Wang, Y. -M.; Biersteker, J. B.; Sheeley, N. R., Jr.; Koutchmy, S.; Mouette, J.; Druckmüller, M. Bibcode: 2007ApJ...660..882W Altcode: Solar eclipse observations have long suggested that the white-light corona is permeated by long fine rays. By comparing photographs of the 2006 March 29 total eclipse with current-free extrapolations of photospheric field measurements and with images from the Solar and Heliospheric Observatory (SOHO), we deduce that the bulk of these linear features fall into three categories: (1) polar and low-latitude plumes that overlie small magnetic bipoles inside coronal holes, (2) helmet streamer rays that overlie large loop arcades and separate coronal holes of opposite polarity, and (3) ``pseudostreamer'' rays that overlie twin loop arcades and separate coronal holes of the same polarity. The helmet streamer rays extend outward to form the plasma sheet component of the slow solar wind, while the plumes and pseudostreamers contribute to the fast solar wind. In all three cases, the rays are formed by magnetic reconnection between closed coronal loops and adjacent open field lines. Although seemingly ubiquitous when seen projected against the sky plane, the rays are in fact rooted inside or along the boundaries of coronal holes. Title: Chromospheric and Prominence Physics with the ASPIICS Formation Flying Coronagraph Authors: Lamy, P.; Vivès, S.; Koutchmy, S.; Arnaud, J. Bibcode: 2007ASPC..368..639L Altcode: Classical externally-occulted coronagraphs are presently limited in their performances by the distance between the external occulter and the front objective. The diffraction fringe from the occulter and the vignetted pupil which degrades the spatial resolution prevent observing the inner corona inside typically 2--2.5 solar radii (R⊙). Formation flying opens new perspectives and allow to conceive giant, externally-occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft. ASPIICS (Association de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne Solaire) is a mission proposed to ESA in the framework of the PROBA-3 program of formation flying which is presently under study, to exploit this technique for coronal observations. ASPIICS is composed of a single coronagraph which performs high spatial resolution imaging of the corona as well as 2-dimensional spectroscopy of several emission lines (in particular the forbidden line of Fe XIV at 530.285 nm) from the coronal base out to 3 R⊙. The classical design of an externally occulted coronagraph is adapted to the detection of the very inner corona, and the addition of a Fabry-Pérot interferometer. By tuning the position of the occulter spacecraft, it will be possible to reach the chromosphere and the upper part of the spicules. Filtergrams on the helium D3 line or even better, the hydrogen Hβ line (which is optically thin contrary to Hα) will give access to the ``cold corona'', and could allow measuring the chromospheric prolateness. Title: On the dynamic nature of the prolate solar chromosphere: jet formation Authors: Filippov, B.; Koutchmy, S.; Vilinga, J. Bibcode: 2007A&A...464.1119F Altcode: Context: In "cool" spectral lines, the smoothed upper edge of the solar chromosphere is prolate in the South-North direction at the epoch of minimum solar activity and nearly spherically symmetric at the maximum phase. We attribute the effect to the dynamical nature of the upper chromosphere, which consists of a large number of small jet-like structures ascending into the corona. We could not resolve the source region of an individual jetlet, although similar but larger structures are visible, especially in EUV coronal lines.
Aims: We consider the problem of the formation of an individual jet above the limb, assuming that a large number of jet-like events is responsible for the prolate solar upper chromosphere. We then assume that spicules, being the cool part of the phenomenon, behave similarly, and we will mainly concentrate the analysis on the magnetic origin of the event.
Methods: Image processing is used to reveal the displacement of magnetic field tubes filled with coronal plasma and jet formation due to field aligned motion above the null point created in the corona by the emerging magnetic bipole.
Results: The growth of the bipole leads to a reconnection of the field lines and to a specific plasma motion in the vicinity of the null point that results in a plasma flow along the spine line of the 3D null. We assume that similar but smaller processes could happen very often at a smaller scale in the chromosphere, near emerging magnetic ephemeral regions, forming numerous jetlets in the upper chromosphere. As the field aligned motion is guided by the magnetic field, at the epoch of low activity the large-scale structure of the polar magnetic field and the one of the quiet equatorial region is sufficiently different to explain the prolateness of the chromosphere. Title: Analysis of broad-band Hα coronagraphic observations Authors: Romeuf, D.; Meunier, N.; Noëns, J. -C.; Koutchmy, S.; Jimenez, R.; Wurmser, O.; Rochain, S.; "Observateurs Associés" Team Bibcode: 2007A&A...462..731R Altcode: Context: Daily broad-band full-limb Hα images of the inner corona were obtained during solar cycle 23 (1994-2005) using the 15 cm Pic-du-Midi coronagraph.
Aims: We want to automatically extract the properties and evolutions of the observed cool HI coronal structures over a wide range of sizes and light fluxes, from small jets and/or spikes to large prominences.
Methods: A tool was developed to process the complete set of stored images. This paper describes the recognition techniques implemented in our software and discusses its use. It includes the removal of the parasitic diffraction ring produced by the set of different occulting disks used throughout the year.
Results: We present and discuss selected results from a statistical analysis of the occurrence of parameters characterizing the observed structures applied to a large sample of observations. It illustrates the capabilities of this software when applied to our database. Strong asymmetries of the activity level over the solar poles become evident, confirming similar results from previous works. We also discuss the distribution of relative light fluxes of these structures over a wide range of sizes.
Conclusions: The complete series of FITS and calibrated images, the list of the detected structures, and their geometric and luminosity evolutions are stored in the BASS2000 solar database catalogue (http://bass2000.bagn.obs-mip.fr) and are made publicly available. The Hα HI structures observed over the limb of the sun present statistical properties of great interest for understanding its eruptive activity. Title: Analysis of broad-band Hα coronagraphic observations Authors: Noëns, J. -C.; Romeuf, D.; Meunier, N.; Koutchmy, S.; Jimenez, R.; Wurmser, O.; Rochain, S.; "O. A. " Team Bibcode: 2006sf2a.conf..557N Altcode: Broad-band full-limb H-alpha images of the inner corona were obtained since the beginning of the solar cycle 23 using one of the Pic-du-Midi coronagraph. We developed a tool to process the complete set of stored images and to extract automatically the properties and evolutions of the observed cold HI coronal structures over a large range of sizes and light fluxes, from small jets and/or spikes to large prominences. The paper describes the recognition techniques implemented in our software and discusses its use. Then we present some new results following a statistical analysis of the occurrence of structure parameters applied to a large sample of observations. It illustrates the capabilities of this software when applied to our database. Strong activity-asymmetries over the solar poles are shown, confirming similar results from elsewhere. We also discuss the distribution of relative light fluxes of these structures over a wide range of sizes. See also: http://bass2000.bagn.obs-mip.fr. Title: Preliminary results from the March 29, 2006 total eclipse observations in Egypt Authors: Koutchmy, S.; Daniel, J. -Y.; Mouette., J.; Vilinga, J.; Noëns, J. -C.; Damé, L.; Faurobert, M.; Dara, H.; Hady, A.; Semeida, M.; Sabry, M.; Domenech, A.; Munier, J. -M.; Jimenez, R.; Legault, Th.; Viladrich, Ch.; Kuzin, S.; Pertsov, A.; O. A. Team Bibcode: 2006sf2a.conf..547K Altcode: A coordinated effort has been carried in the framework of the French-Egyptian scientific cooperation to permit joined simultaneous eclipse observations of the solar corona during the total solar eclipse of March 29, 2006. Spaceborne EIT and Lasco (SoHO) observations were also planned at the same time and were successfully collected. Scientists from other countries collaborated on different experiments. The synthetic image showing the magnetic coronal structure of this quasi-minimum corona seen in W-L is given. Some preliminary results are presented; a White Light (W.L.) movie has been also taken during the totality. Title: ASPIICS, a giant externally occulted coronagraph for the PROBA-3 formation flyer mission Authors: Vivès, S.; Lamy, P.; Koutchmy, S.; Arnaud, J. Bibcode: 2006cosp...36.3063V Altcode: 2006cosp.meet.3063V Formation flyers open new perspectives and allow to conceive giant externally-occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft at approximately 100 m from the first one ASPIICS Association de Satellites Pour l Imagerie et l Interferometrie de la Couronne Solaire is a mission proposed to ESA in the framework of the PROBA-3 program of formation flyers which is presently in phase A to exploit this technique for coronal observations ASPIICS is composed of a single coronagraph which performs high spatial resolution imaging of the corona as well as 2-dimensional spectroscopy of several emission lines from the coronal base out to 3 Rs The selected lines allow to address different coronal regions the forbidden line of FeXIV at 530 285 nm coronal matter Fe IX X at 637 4 nm coronal holes HeI at 587 6 cold matter An additional broad spectral channel will image the white light corona and derive electron densities The classical design of an externally occulted coronagraph is adapted to the detection of the very inner corona as close as 1 01 Rs and the addition of a Fabry-Perot interferometer using a so-called etalon ASPIICS will address the question of the coronal heating and the role of waves by characterizing propagating fluctuations waves and turbulence in the solar wind acceleration region and by looking for oscillations in the intensity and Doppler shift of spectral lines The combined imaging and spectral diagnostics capabilities available with ASPIICS Title: On the solar white-light high resolution observations from space Authors: Veselovsky, I. S.; Koutchmy, S. Bibcode: 2006AdSpR..37.1576V Altcode: Absolutely calibrated telescopic observations of the Sun in white-light with a sufficiently high space-time resolution from space have not been regularly performed. They are needed to resolve several important problems in the solar physics. Contributions of different morphological features to the total solar irradiance variations in the broad range of time scales from seconds up to many years can be definitely established in this manner for the first time. The quantitative role of the white-light emission in the overall energy balance of flares and eruptions on the Sun can be evaluated. More adequate theoretical models of corresponding processes on the Sun can be constructed using this new data. Title: Chromospheric Prolateness: Solar Cycle Variations Authors: Vilinga, J.; Koutchmy, S.; Auchere, Fr.; Baudin, Fr.; Filippov, B.; Noens, J. -C. Bibcode: 2006IAUS..233..240V Altcode: The solar prolateness (also known as Ovalisation, a french origin name) of the extended dynamical chromosphere is established from measurements performed above 2 Mm heights during the years of solar minimum, using the Hα, Ca II K and HeII 304 line emissions from both ground-based and space-based observations. Coronal X-EUV emissions usually penetrate deep enough into the chromosphere to completely mask this effect on transition region lines and produce the so-called coronal hole effect. However, cool lines like Hα and Ca II lines, do NOT show this Coronal Hole (CH) effect. Coronal lines and HeI (D3; 1083 nm) do show CHs but do not show the prolateness effect. We first briefly review different methods which can potentially be used to measure the prolateness. Further we note the similarity of the geometric behaviour of the prolateness and its variation along the solar cycle compared to the behaviour of the fast solar wind. It suggests the same origin possibly related to the emergence of the small scale network and internetwork magnetic field towards the corona and small scale magnetic reconnections. A simple geometric model was proposed to explain the effect of the prolateness of the solar chromosphere by considering that the specific dynamical part of the solar atmosphere above the 2 Mm level, being a mixture of up and down moving jets of chromospheric matter with the coronal plasma between them, is responsible for the solar prolateness (Filippov and Koutchmy, 2000). We however note that polar regions are also showing different types of activity in the low corona, including small prominence eruptions seen e.g. in Hα and linear jets seen in SXR and EUV as well as in W-L (eclipses). Some kind of dynamical dissipation of the newly emerged magnetic field is needed. More systematic measurements should be done to build a more complete, possibly 3D, picture to explain the extended in the horizontal direction lifting effect of a large part of the polar chromosphere. Title: SOLARNET & LAIME: Imaging & Spectroscopy in the Far Ultraviolet Authors: Damé, Luc; Koutchmy, Serge Bibcode: 2006IAUS..233..435D Altcode: SOLARNET is a medium size high resolution solar physics mission proposed to CNES and ESA for a new start in 2007 and a possible launch in 2012 (CNES) or later (ESA Cosmic Vision framework: 2015-2016). Partnerships with India and China are under discussion, and several European contributions are considered. At the center of the SOLARNET mission is a 3-telescope interferometer of 1 meter baseline capable to provide 40 times the best ever spatial resolution achieved in Space with previous, current or even planned solar missions: 20 mas - 20 km on the Sun in the FUV. The interferometer is associated to an on-axis Subtractive Double Monochromator coupled to an Imaging Fourier Transform Spectrometer capable of high spectral (0.01 nm) and high temporal resolutions (50 ms) on a field of view of 40 arcsec and covering the FUV and UV spectral domains (from 117.5 to 400 nm). This will allow to access process scales of magnetic reconnection, dissipation, emerging flux and much more, from the chromosphere to the low corona with emphasis on the transition zone where the magnetic confinement is expected to be maximum. A whole new chapter of the physics of solar magnetic field structuring, evolution and mapping from the photosphere to the high atmosphere will be opened. The interferometer is completed by instruments providing larger field of view and higher temperature (EUV-XUV coronal imaging & spectroscopy) to define the context and extension of the solar phenomena. The 3-telescope interferometer design results of an extensive laboratory demonstration program of interferometric imaging of extended objects. We will review the scientific program of SOLARNET, describe the interferometer concept and design, present the results of the breadboard and give a short overview of the mission aspects. In a different category, LAIME, the Lyman Alpha Imaging-Monitor Experiment, is a remarkably simple (no mechanisms) and compact full Sun imager to be flown with TESIS on the CORONAS-PHOTON mission in 2008. It could be the only chromospheric imager to be flown in the next years, supporting Solar-B, STEREO, SDO and the Belgian LYRA Lyman Alpha flux monitor. We will give a short description of this unique 60 mm aperture imaging telescope, dedicated to the investigation of the UV sources of solar variability and of the chromospheric and coronal disruptive events (Moreton waves, prominences, CMEs, etc.). Title: The CME dynamics associated to the prominence eruption of December 2, 2003 Authors: Slemzin, Vladimir A.; Koutchmy, S.; Noens, J. -C.; Romeuf, D. Bibcode: 2006IAUS..233..395S Altcode: We report on a complex study of a typical large W-limb CME event occurring on December 2, 2003 in the vicinity of AR 0508. It is associated with a prominence eruption which has been observed with the Pic du Midi Ha flux coronagraph as well as in EUV by both the SOHO/EIT and the Coronas/SPIRIT space telescopes. The eruption started with the emergence of a fast expanding loop between 9 and 10 UT, followed by a heating and an acceleration of the erupted material and resulted in three-part CME observed by LASCO after 10:50 UT. A temporal analysis of the prominence motion and the EUV dimming light curve have shown that both the frontal structure and the core of a CME were initiated simultaneously with the peak of the X-ray C7.2 flare. The total mass of the prominence including the Hα filament and EUV filament channel is close to the mass of the core but significantly less than the total CME mass. Title: Scientific requirements for future spatially resolved W-L observations of the Sun Authors: Veselovsky, I.; Koutchmy, S. Bibcode: 2006cosp...36..202V Altcode: 2006cosp.meet..202V Several important issues are open in the field of solar variability and they wait their solution which up to now was attempted using critical ground-based instrumentations However precise photometric data are attainable only from space The new observational material should be collected with high enough spatial resolution starting with the visible range of the electromagnetic spectrum 1 the absolute contributions of different small-scale structural entities of the solar atmosphere from the white light flares and from micro-flares are still poorly known 2 we do not know the absolute contributions of different structural elements of the solar atmosphere to the long-term and to the cyclic variations of the solar irradiance including features of the polar regions of the Sun 3 the variations of the chromospheric magnetic network are still poorly evaluated 4 only scarce information is available about the spectral variations of different small-scale features in the high photosphere The variability of the Sun in white light can be studied with higher spectral spatial and time resolution using space-born telescopes which is much more appropriate for this purpose than ground based observatories because of better seeing conditions no interference of the terrestrial atmosphere and a more precise calibration procedure We discuss the scientific requirements for such observations and the possible experimental tools proposed for their solution The broader astrophysical context of the suggested solar studies is also considered Title: The Lyman Alpha Imaging-Monitor Experiment (LAIME) for TESIS/CORONAS-PHOTON Authors: Damé, L.; Koutchmy, S.; Kuzin, S.; Lamy, P.; Malherbe, J. -M.; Noëns, J. -C. Bibcode: 2006cosp...36.3524D Altcode: 2006cosp.meet.3524D LAIME the Lyman Alpha Imaging-Monitor Experiment is a remarkably simple no mechanisms and compact 100x100x400 mm full Sun imager to be flown with TESIS on the CORONAS-PHOTON mission launch expected before mid-2008 As such it will be the only true chromospheric imager to be flown in the next years supporting TESIS EUV-XUV imaging SDO and the Belgian LYRA Lyman Alpha flux monitor on the ESA PROBA-2 microsatellite launch expected in September 2007 We will give a short description of this unique O60 mm aperture imaging telescope dedicated to the investigating of the magnetic sources of solar variability in the UV and chromospheric and coronal disruptive events rapid waves Moreton waves disparitions brusques of prominences filaments eruptions and CMEs onset The resolution pixel is 2 7 arcsec the field of view 1 4 solar radius and the acquisition cadence could be as high as 1 image minute The back thinned E2V CCD in the focal plane is using frame transfer to avoid shutter and mechanisms Further more the double Lyman Alpha filtering allows a 40 AA FWHM bandwidth and excellent rejection yet providing a vacuum seal design of the telescope MgF2 entrance window Structural stability of the telescope focal length 1 m is preserved by a 4-INVAR bars design with Aluminium compensation in a large pm 10 o around 20 o Title: The Chromospheric Prolateness and its Variations Authors: Vilinga, J.; Koutchmy, S. Bibcode: 2005ASPC..346..269V Altcode: The chromospheric prolateness (also called ovalisation) of the extended dynamical chromosphere was established from measurements performed above 2Mm heights during the years of solar minimum, using the Hα, Ca II K and HeII 304 line emissions from both groundbased and spacebased observations. Coronal X-EUV emissions usually penetrate deep enough into the chromosphere to completely mask this effect on transition region lines and produce the so-called coronal hole effect. However, cool lines like Hα and Ca II lines, do not show this CH effect. Coronal lines and HeI (D3; 1083 nm) do show coronal holes but no prolateness effect. We briefly review different methods which can potentially be used to measure the prolateness. Further we note the similarity of the geometric behaviour of the prolateness and its variation along the solar cycle compared to the behaviour of the fast solar wind. It suggests the same origin related to the emergence of the small scale network and internetwork magnetic field towards the corona. A simple geometric model was proposed to explain the effect of the prolateness of the solar chromosphere by considering that the specific dynamical part of the solar atmosphere above the 2 Mm level, being a mixture of up and down moving jets of chromospheric matter with the coronal plasma between them, is responsible for the solar prolateness. We however note that polar regions are showing different types of activity in the low corona, including prominence eruptions seen in Hα and jets seen in SXR and EUV. Some kind of dissipation of the newly emerged magnetic field is needed. More systematic measurements should be done to build a more complete, possibly 3D, picture to explain this lifting effect of a large part of the chromosphere. Title: About the fe XIV 530.3 NM Line Emissions of the Middle Corona Authors: Koutchmy, S.; Contesse, L.; Viladrich, Ch.; Vilinga, J.; Bocchialini, K. Bibcode: 2005ESASP.600E..26K Altcode: 2005ESPM...11...26K; 2005dysu.confE..26K No abstract at ADS Title: The Center Limb Behavior of Facular-Element Fluxes Authors: Ajabshirizadeh, A.; Koutchmy, S. Bibcode: 2005ESASP.600E..76A Altcode: 2005dysu.confE..76A; 2005ESPM...11...76A No abstract at ADS Title: 29 mars 2006 : éclipse totale sur 4 continents Title: 29 mars 2006 : éclipse totale sur 4 continents Title: March 29, 2006 : total eclipse over four continents Authors: Crussaire, D.; Durand, P.; Koutchmy, S. Bibcode: 2005O&T....60...28C Altcode: We first shortly review the ephemerides of the forthcoming March 29, 2006 solar total eclipse, reminding some definitions for computing the circumstances and providing maps of the eclipse path. The probabilities for a clear sky is also considered. Further we review some of the proposed eclipse imaging experiments which are of interest during the totality, including monochromatic CCD imaging and the complementary aspects with space experiments analysing the solar corona. High spatial resolution images of coronal white-light structures are also of great interest. Title: Formation flyers applied to solar coronal observations: the ASPICS mission Authors: Vives, S.; Lamy, P.; Auchere, F.; Vial, J. -C.; Koutchmy, S.; Arnaud, J.; Prado, J. -Y.; Frassetto, F.; Naletto, G. Bibcode: 2005SPIE.5901..305V Altcode: Classical externally-occulted coronagraphs are presently limited in their performances by the distance between the external occulter and the front objective. The diffraction fringe from the occulter and the vignetted pupil which degrades the spatial resolution prevent observing the inner corona inside typically 2-2.5 solar radii. Formation flyers open new perspectives and allow to conceive giant, externally-occulted coronagraphs using a two-component space system with the external occulter on one spacecraft and the optical instrument on the other spacecraft at approximately 100 m from the first one. ASPICS (Association de Satellites Pour l'Imagerie Coronographique Solaire) is a mission proposed to CNES in the framework of their demonstration program of formation flyers which is presently under study to exploit this technique for coronal observations. In the baseline concept, ASPICS includes three coronagraphs operating in three spectral domains: the visible continuum (K-corona brightness), the HI Lyman alpha emission line at 121.6 nm, and the HeII emission line at 30.4 nm. Their unvignetted fields of view extend from 1.1 to 3.2 solar radii with a typical spatial resolution of 3 arcsec. In order to connect coronal activity to photospheric events, ASPICS further includes two disk imagers. The first one is devoted to the HI Lyman alpha emission line. The second one is a multi-channel instrument similar to SOHO/EIT and devoted to the HeII (30.4 nm), FeIX/X (17.1 nm) and FeXII (19.5 nm) emission lines. Two concepts of the space system are under consideration: a symmetric configuration where the disk imagers and the external occulter are on one spacecraft and the coronagraphs on the other, an asymmetric configuration where the external occulter is on one spacecraft and the scientific instruments are regrouped on the other one. Title: Magnetic Configurations of Streamer Structures in the Solar Atmosphere Authors: Koutchmy, S. L.; Molodensky, M. M. Bibcode: 2005AstL...31..398K Altcode: We consider two types of streamer structures observed in the solar atmosphere. Structures of the first type are medium-scale configurations with scale lengths comparable to the scale height in the corona, kT/mg = 100 thousand km, which appear as characteristic plasma structures in the shape of a dome surrounding the active region with thin streamers emanating from its top. In configurations of this type, gravity plays no decisive role in the mass distribution. The plasma density is constant on magnetic surfaces. Accordingly, the structure of the configurations is defined by the condition ψ = const, where ψ is the flux function of the magnetic field. Structures of the second type are large-scale configurations (coronal helmets, loops, and streamers), which differ from the above structures in that their scale lengths exceed the scale height in the corona. For them, gravity plays a decisive role; as a result, instead of the magnetic surfaces, the determining surface is BgradΦ = 0. We constructed three-dimensional images of these structures. Some of the spatial curves called “visible contours” of the B r = 0 surface are shown to be brightest in the corona. We assume that the helmet boundaries and polar plumes are such curves. Title: Analysis of the radiation of coronal suprathermal streams Authors: Koutchmy, S.; Nikoghossian, A. G. Bibcode: 2005Ap.....48...62K Altcode: This paper reports on the first measurements of the color index of the coronal suprathermal streams. Observations performed during the total eclipse of 2001 in Angola imply that the color index of streams differs markedly from that for adjacent parts of the surrounding corona taken as reference. The registered drifts to the longwave and shortwave domains of the spectrum are in agreement with theoretical results obtained recently by the authors. Title: Solar origins of intense geomagnetic storms in 2002 as seen by the CORONAS-F satellite Authors: Panasenco, O.; Veselovsky, I. S.; Dmitriev, A. V.; Zhukov, A. N.; Yakovchouk, O. S.; Zhitnik, I. A.; Ignat'ev, A. P.; Kuzin, S. V.; Pertsov, A. A.; Slemzin, V. A.; Boldyrev, S. I.; Romashets, E. P.; Stepanov, A.; Bugaenco, O. I.; Bothmer, V.; Koutchmy, S.; Adjabshirizadeh, A.; Fazel, Z.; Sobhanian, S. Bibcode: 2005AdSpR..36.1595P Altcode: We analyze solar origins of intense geomagnetic perturbations recorded during 2002. All of them were related to coronal mass ejections (CMEs). The initiation of CMEs was documented using the SPIRIT instrument (SPectrohelIographic Soft X-Ray Imaging Telescope) onboard the CORONAS-F satellite. Monochromatic full Sun images taken in the Mg XII doublet at 8.418 and 8.423 Å showed the appearance of free energy release sites at altitudes up to 0.4 solar radii. CMEs were initiated at these sites and propagated in interplanetary space under appropriate local conditions including the geometry of the magnetic fields. Title: Analysis of non-thermal velocities in the solar corona Authors: Contesse, L.; Koutchmy, S.; Viladrich, C. Bibcode: 2004AnGeo..22.3055C Altcode: Available from http://www.copernicus.org/site/EGU/annales/22/8/3055.htm?FrameEngine=false; Title: The August 11th, 1999 CME Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Daniel, J. -Y.; Delaboudinière, J. -P.; Golub, L.; Lamy, P.; Adjabshirizadeh, A. Bibcode: 2004A&A...420..709K Altcode: We present here a set of observations, space borne and ground based, at different wavelengths, of the solar corona at and after the time of the total solar eclipse of August 11{th}. It is used to consider some unusual features of the coronal dynamics related to a limb Coronal Mass Ejection (CME) observed after the total eclipse. The complementary aspect of simultaneous ground-based and space-borne observations of the corona is used to produce an accurate composite image of the White Light (W-L) corona before the CME. A high arch system (possibly a dome-like structure, with large cavities inside but without a cusp further out) which appeared on the eclipse W-L images, is suggested to be a large-scale precursor of the CME, well preceding the eruption of the top part of the brightest prominence recorded in W-L. This bright prominence is shown as a filament in absorption using the Transition Region And Corona Explorer (TRACE) images taken in different coronal lines. The analysis of the images of the Large Angle and Spectrometric Coronograph (LASCO) on board the Solar and Heliospheric Observatory (SoHO), showing the progression of the CME, is discussed in an attempt to make a connection with the surface event. A SoHO-EIT (Extreme UV Imager Telescope) image sequence details the prominence eruption and shows the sudden heating processes of the ejected parts. We found that there is no reason to assume that the huge cavity is significantly destabilised well before the eruption of the upper part of the low-lying bright twisted filament which coincides with the position of one of the legs of the high arch. Observations are still compatible with the assumption of both the break-out model and of the flux rope erupting model as a result of a shear or of an increasing poloıdal magnetic flux from below. We stress the possible role of buoyancy of the giant cavity as a destabilizing factor leading to the CME, noticing that some motion of coronal material back toward the surface can be seen during at least the first phase of the CME, from both EIT and LASCO observations. Title: Dynamics of the loop prominence and coronal mass ejection observed on March 2, 2002 Authors: Panasenco, O.; Veselovsky, I. S.; Zhukov, A. N.; Yakovchouk, O. S.; Koutchmy, S.; Delaboudiniere, J. -P. Bibcode: 2004cosp...35.2974P Altcode: 2004cosp.meet.2974P SOHO/EIT and LASCO data are used for the case study of the coronal mass ejection initiation and development. The shape, velocity and temperature of the loop prominence before and during the ejection as well as the new arcade formation are well documented. The prominence consisted of two spirals interweaved on the semi-torus. Both spirals are clearly seen during the initial stage of the expansion with a velocity about 300 km/s. Than, one of them is rapidly heated, when other remained cool. The number of curls is conserved during the expansion. The main axis of the torus is initially represented by the planar curve resembling a semi-circle. After some time, the summit of the torus is twisted in the manner that the main axis looks not planar at the top in the field of view of LASCO C3 when the velocity attains about 1000 km/s. The topological connectivity of the loops to the Sun is preserved for more than three hours even after the new arcade formation. Title: H/He+ intensity variations of the cool corona Authors: Noens, J. -C.; Balestat, M. -F.; Jimenez, R.; Rochain, S.; Romeuf, D.; Auchere, F.; Delaboudiniere, P.; Koutchmy, S. Bibcode: 2004IAUS..223..291N Altcode: 2005IAUS..223..291N No abstract at ADS Title: Structure and Dynamics of the Solar Corona Authors: Koutchmy, S. Bibcode: 2004IAUS..223..509K Altcode: 2005IAUS..223..509K We briefly review several aspects of the quasi-stationary structure of the corona in relation with the helio-sheet and, also, of the more confined by the magnetic field structures, including streamers, loops, jets, plumes and narrow linear rays. Both the temperature and the density structures are tentatively considered. Flows deduced from proper motions analysis are discussed. We did not include CMEs and flares in this presentation but other more radial and possibly highly impulsive beams with flows are discussed. We stress the importance of the variations of the coronal magnetic field and inferred currents in explaining the observed structures. Title: Wavelet Analysis of Umbral Oscillations Authors: Christopoulou, E. B.; Skodras, A.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 2003ApJ...591..416C Altcode: We study the temporal behavior of the intensity and velocity chromospheric umbral oscillations, applying wavelet analysis techniques to four sets of observations in the Hα line and one set of simultaneous observations in the Hα and the nonmagnetic Fe I (5576.099 Å) line. The wavelet and Fourier power spectra of the intensity and the velocity at chromospheric levels show both 3 and 5 minute oscillations. Oscillations in the 5 minute band are prominent in the intensity power spectra; they are significantly reduced in the velocity power spectra. We observe multiple peaks of closely spaced cospatial frequencies in the 3 minute band (5-8 mHz). Typically, there are three oscillating modes present: (1) a major one near 5.5 mHz, (2) a secondary near 6.3 mHz, and (3) oscillations with time-varying frequencies around 7.5 mHz that are present for limited time intervals. In the frame of current theories, the oscillating mode near 5.5 mHz should be considered as a fingerprint of the photospheric resonator, while the other two modes can be better explained by the chromospheric resonator. The wavelet spectra show a dynamic temporal behavior of the 3 minute oscillations. We observed (1) frequency drifts, (2) modes that are stable over a long time and then fade away or split up into two oscillation modes, and (3) suppression of frequencies for short time intervals. This behavior can be explained by the coupling between modes closely spaced in frequency or/and by long-term variations of the driving source of the resonators.

Based on observations performed on the National Solar Observatory/Sacramento Peak Observatory Richard B. Dunn Solar Telescope (DST) and on the Big Bear Solar Observatory Harold Zirin Telescope. Title: Chromospheric Evershed flow Authors: Georgakilas, A. A.; Christopoulou, E. B.; Skodras, A.; Koutchmy, S. Bibcode: 2003A&A...403.1123G Altcode: We studied the chromospheric Evershed flow from filtergrams obtained at nine wavelengths along the Hα profile. We computed line-of-sight velocities based on Becker's cloud model and we determined the components of the flow velocity vector as a function of distance from the center of the sunspot, assuming an axial symmetry of both the spot and the flow. We found that the flow velocity decreases with decreasing height and that the maximum of the velocity shifts towards the inner penumbral boundary. The flow related to some fibrils deviates significantly from the average Evershed flow. The profile of the magnitude of the flow velocity as a function of distance from the spot center, indicates that the velocity attains its maximum value in the downstream part of the flow channels (assumed to have the form of a loop). This behavior can be understood in terms of a critical flow that pass from subsonic to supersonic near the apex of the loop, attains its higher velocity at the downstream part of the loop and finally relaxes to subsonic through a tube shock. We computed the average flow vector from segmented line-of-sight velocity maps, excluding bright or dark fibrils alternatively. We found that the radial component of the velocity does not show a significant difference, but the magnitude of the vertical component of the velocity related to dark fibrils is higher than that related to bright fibrils.

Based on observations performed on the NSO/SPO Richard B. Dunn Solar Telescope (DST). Title: The solar high-resolution imager - coronagraph LYOT mission Authors: Vial, Jean-Claude; Song, Xueyan; Lemaire, Philippe; Gabriel, Alan H.; Delaboudiniere, Jean-Pierre; Bocchialini, Karine; Koutchmy, Serge L.; Lamy, Philippe L.; Mercier, Raymond; Ravet, Marie Francoise; Auchere, Frederic Bibcode: 2003SPIE.4853..479V Altcode: The LYOT (LYman Orbiting Telescope) solar mission is proposed to be implemented on a micro-satellite of CNES (France) under phase A study. It includes two main instruments, which image the solar disk and the low corona up to 2.5 Ro in the H I Lyman-α line at 121.6 nm. The spatial resolution is about 1” for the disk and 2.5” for corona. It also carries an EIT-type telescope in the He II (30.4 nm) line. The coronagraph needs a super polished mirror at the entrance pupil to minimize the light scattering. Gratings and optical filters are used to select the Lyman-α wavelength. VUV cameras with 2048×2048 pixels record solar images up to every 10 seconds. The satellite operates at a high telemetry rate (more then 100 kb/s, after onboard data compression). The envisaged orbits are either geostationary or heliosynchronous. Possible launch dates could be end of 2006 - beginning of 2007. Title: Coronal linear threads: W-L radiation of supra-thermal streams Authors: Koutchmy, S.; Nikoghossian, A. G. Bibcode: 2002A&A...395..983K Altcode: The paper aims at revealing the role of the Compton effect when considering the W-L scattering of the solar photospheric radiation by coronal supra-thermal streams. We first document several examples of well observed cases of linear W-L coronal threads extending above flaring active regions which are good candidates to give the signature known from the interpretation of radio type III bursts. The height-dependent model problem of Compton scattering on the beam of fast electrons gyrating around the lines of force of the magnetic field is considered. The resulting change in frequency averaged over the beam and the solid angle, within which the photospheric radiation falls, is computed for both sunward and antisunward directed streams. The dependence of the effect on the height above the solar surface, the speed of electrons and the slope angle is discussed. For illustration, we consider the case, in which the frequency distribution of the incident radiation is Planckian. The effective value of the cross-section of interaction is compared with that for the Thomson scattering. In particular, we conclude that, depending on the angle between the directions of the initial outburst and the magnetic field, the streams moving away from the Sun may produce drifts in frequency to the shortwave, as well as to the longwave domains of the spectrum. The effect may become essential even for moderate energies of fast electrons, and it should be measurable using precise photometric color index determination, if only the fractional density of fast electrons is not too small. Title: Center-limb and shape-factor variations of facular elements Authors: Adjabshirizadeh, Ali; Koutchmy, Serge Bibcode: 2002ESASP.506..415A Altcode: 2002ESPM...10..415A; 2002svco.conf..415A Digital processing is used to measure the contrast of solar faculae from a set of high resolution selected images observed at the R.B. Dunn's 76 cm clear aperture vacuum telescope of NSO-Sacramento Peak Observatory. Five ultra-narrow passbands from Red to Blue (Red, Hα, Mgbl, Green, Blue) were given by the UBF. The range of heliocentric distances covered by our measurements is 0.1 < μ = cosθ < 0.4 (θ ɛ 84°, 66°). About 104 facular "points" were measured over nearly 100 selected images. By averaging and normalizing the contrast of faculae and plotting them vs. heliocentric angle, we found that the contrast increases monotonically towards the limb for all wavelengths. The contrast increases as wavelength decreases. We did not introduce any correction for the smearing in our measurements, in order not to bias the results. In addition, we study the variations of integrated brightnesses or fluxes in order to discuss the flux contribution of faculae. Fluxes definitely show a peak value near μ = 0.25, and then a decrease towards the limb. The center limb effect of the shape-factor of facular elements is finally analyzed; the ratio of apparent sizes in the radial and in the tangential directions do not show the foreshortening effect expected to be observed over cell-like structures, suggesting that facular elements are structured by a small scale highly concentrated magnetic field and not just by the gravity. Title: On Interpretation of the Radiation of Coronal Suprathermal Streams. II Authors: Nikoghossian, A. G.; Koutchmy, S. Bibcode: 2002Ap.....45..489N Altcode: This is the second part of the series of two articles which consider the effect of Compton scattering of the photospheric radiation on fast electrons of the coronal suprathermal streams. As compared to the previous part, a more realistic height-dependent model problem is treated. The results of numerical calculations for the mean frequency change and the proper cross-section for both the sunward and antisunward directed beams of electrons are given as a function of height and the slope angle. It is concluded that, depending on the angle between directions of the initial outburst and magnetic field, the scattering on the beams moving away the Sun may produce measurable drifts in frequency to shortwave as well as to longwave domains of the spectrum. At the same time, the sunward directed beams result only in an increase in the photon energy. Title: About the prominence heating mechanisms during its eruptive phase Authors: Filippov, B.; Koutchmy, S. Bibcode: 2002SoPh..208..283F Altcode: Recent EUV observations reveal that the `image' of the prominence overlaying coronal emission sometimes suddenly changes from absorption of EUV radiation to emission during the eruptive phase. This change reveals fast heating of the plasma within the prominence. We propose a kinetic mechanism of heating the fluid particles that transforms magnetic energy of the pre-eruptive magnetic configuration stored in the filament electric current into heat through collision processes of counteracting flows. The shape of the flux that the filament is made of should include upward concave segments to provide the counter flows within the erupting prominence. A typical twisted flux rope easily meets this requirement. Gas dynamic calculations are offered in addition to permit a quantitative evaluation of the relevant parameters and their time variations. Title: Coronal Linear Supra-thermal Streams Authors: Koutchmy, S.; Nikoghossian, A. Bibcode: 2002sf2a.conf..143K Altcode: Linear structures of the Solar Corona seen on eclipse images above active regions after the flaring activity are good candidates for being produced by primary supra-thermal streams of electrons. We propose a method to compute the Compton scattering effect applied to this case and compute the corresponding diagrams. This predicted effect will be search for on eclipse data and possibly using the SoHO Lasco coronagraph observations. Title: The global August 11, 1999 eclipse corona and solar cycle variations Authors: Adjabshirizadeh, Ali; Koutchmy, Serge Bibcode: 2002ESASP.477...65A Altcode: 2002scsw.conf...65A Qualitative results from the last solar total eclipse (August 11th, 1999) are presented in order to extract some quantitative parameters permitting to discuss the structure of the near-maximum corona and insert the results among what is known of the changing with the solar cycle of activity structure. The collaborative study of the solar corona has been performed in Iran, using a radial gradient filter in white light and other techniques. From the eclipse-processed pictures, a structural drawing was analysed to give the distribution of streamlines over the entire corona, in order to look at the deviations from the local radial direction of identified coronal streamers. From the deduced parameter and the known solar cycle variations of this instantaneous "average deviation" of coronal streamers, as deduced from eclipse observations of 4 preceding cycles, we correctly predicted the moment of the following maximum of activity. We further discuss the method, using the "average deviations" measured in 1996 - 2001 from the Lasco C2 coronagraph processed images (from NRL) of SoHO and found an excellent agreement with the parameters deduced from the last total eclipses of 1998, 1999 and 2001. We believe that "average deviations" are a good parameter to contribute in the understanding of the origin of solar cycle variations of the solar wind and of the magnetic field. Title: The August 11th, 1999 total eclipse CME Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Delaboudinière, J. -P.; Adjabshirizadeh, A. Bibcode: 2002ESASP.477...55K Altcode: 2002scsw.conf...55K We use spaceborne observations and ground-based eclipse observations to analyse the spectacular W-limb CME which occurred several hours after the totality in Iran. The underlying high arch system (possibly a dome-like structure with cavities inside) which appeared on the eclipse White-Light (W-L) images, is suggested to be a large scale precursor of the CME, taking into account the related coronal cavities (as measured from the broadening of the green Fe XIV line) and the properties of the inserted prominence which erupted during the CME. Title: The Three-Dimensional Structure of the Solar Corona Authors: Koutchmy, S. L.; Merzlyakov, V. L.; Molodenskii, M. M. Bibcode: 2001ARep...45..834K Altcode: The surface where the radial component of the solar magnetic field changes sign is computed for a minimum corona. It is shown that (1) the projection of the folds of this surface onto the plane of the sky is consistent with the helmet structures observed during the eclipse of June 30, 1954; (2) there are type 1 and type 2 helmets, according to the well-known classification of coronal structures; (3) some elements of this sign-change surface of the radial field can be classified as so-called envelopes. The results obtained suggest that more complex coronal structures can be described in a similar way. An MHD model of polar plumes is considered. Title: Interpretation of the Radiation of Coronal Suprathermal Streams. I. Authors: Nikoghossian, A. G.; Koutchmy, S. Bibcode: 2001Ap.....44..528N Altcode: This is the first part of a series of two articles aimed at revealing the role of the Compton effect in scattering of the solar photospheric radiation by coronal suprathermal streams. The simplest situation of a single beam of electrons gyrating around the strength lines of magnetic field is considered. Attention is focused on the height-independent problem, in which the role of the spatial angle of incident radiation is ignored. Analytical expressions for the frequency change of interacting photons and for the proper cross-section of the scattering process are derived. The results of numerical calculations show that the effect may by significant even for moderate energies of fast electrons and will be observable only if the fractional density of fast electrons is not too small. Title: Multi-wavelength study of Network Bright Points near the limb* Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S. Bibcode: 2001SoPh..202..241G Altcode: We analyze the morphology of network bright points (NBPs), their relation to fine dark mottles and their temporal variations, using observations of a quiet region near the polar solar limb, obtained during the solar minimum. For our analysis we used an image-processing method for the selection and identification of NBPs. Further we constructed 'maximum power frequency' maps computing the power spectrum for each pixel of a field and selecting the frequency of maximum spectral power as the most representative oscillating frequency for this pixel. The morphological analysis of our data indicates that the enhancement of NBPs is part of a complicated process that is responsible for the formation of mottles. The analysis of the lifetimes of NBPs indicates that although the general patterns of NBPs remain constant for time intervals larger than an hour, the lifetime of individual bright points is of the order of 16 min. Furthermore, our results indicate an association of the lifetime of NBPs with that of mottles. From the analysis of temporal variations we confirm that the power of NBPs is smaller than the corresponding power for intra-network points at both the 3-min and the 5-min oscillating modes and in both the Mg b1−0.4 Å and the continuum. Our analysis revealed enhanced power in the 7-min range, which is theoretically considered a candidate frequency for transverse waves related to NBPs at the base of the chromosphere (Kalkofen, 1997). However, we consider more likely that this period is related to the evolution of individual NBPs. Title: Fine Structure of the Quiet Solar Chromosphere: Limb-Crossing Features Authors: Zachariadis, Th. G.; Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.; Gontikakis, C. Bibcode: 2001SoPh..202...41Z Altcode: In this article we study chromospheric structures (spicules) crossing the solar limb in Hα images corrected for limb darkening. This correction enabled us to view structures both on the disk and beyond the limb in the same image. The observations were obtained at the Sacramento Peak Observatory at Hα±0.75 Å. The processed images reveal both bright and dark (relative to the local background) features crossing the limb. We also observed bushes (rosettes) crossing the limb, as well as structures indicating probably arch-shaped mottles beyond the limb. Title: Oscillations and running waves observed in sunspots. III. Multilayer study Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 2001A&A...375..617C Altcode: We continue our study of waves and oscillations observed in sunspots using an improved method for enhancing the waves, giving the opportunity to identify them and determine their properties in far Hα wings. We found that the running penumbral waves are observable at least up to the formation height of the Hα +/- 0.5 Å line, but not in the Hα +/- 0.75 Å or the Fe I+/-0.12 Å. We found a time lag between the waves in the blue and the red wing of the Hα line corresponding to a phase shift of 180o, that indicates a pure Doppler shift of the line. There is a lag in the propagation of the waves seen at Hα center and at Hα wings. Also there is a lag in the variation of the umbral oscillations as they are observed from lower to higher atmospheric layers. The correlation between umbral oscillations at various atmospheric heights and running penumbral waves strongly indicates that the latter are excited by photospheric umbral oscillations and not the chromospheric ones. We found a new category of photospheric waves that originate at approximately 0.7 of the distance between the umbra and the penumbra boundary and propagate beyond the outer penumbra boundary with a velocity of the order of 3-4 km s-1. Further, we found 3 min penumbral oscillations apparent in the inner penumbra at lower chromospheric layers (far Hα wings). Based on observations performed on the NSO/SPO Richard B. Dunn Solar Telescope (DST) Title: Polar surges and macrospicules. II. Dynamics of an eruptive event from off-limb observations Authors: Georgakilas, A. A.; Koutchmy, S.; Christopoulou, E. B. Bibcode: 2001A&A...370..273G Altcode: We continue our study of polar surges and macrospicules at the period of solar minimum, analyzing high resolution multiwavelength limb observations that provide a clearer picture of the dynamical phenomena occurring well above the chromosphere of a polar cap. The time sequence of an erupting and impulsive polar event is examined from the low chromosphere to coronal heights, deriving both proper motions and Doppler velocities. Our observations suggest that there is a close association of polar surges with explosive events, supporting the hypothesis that magnetic reconnection triggered by emerging flux provides the accelerative mechanism for this polar region event. Title: Fine Structure of the Magnetic Chromosphere: Near-Limb Imaging, Data Processing and Analysis of Spicules and Mottles Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 2001SoPh..199...61C Altcode: The origin and the dynamical evolution of spicules and mottles continue to be a highly interesting research subject. Using high-resolution Hα observations obtained with the Dunn Solar Telescope of the Sacramento Peak Observatory and an image processing technique for the enhancement of near-limb solar images, we study the dynamics of spicules and mottles as well as their relation. Our image-processing technique is based on the correction for the limb darkening and the use of a directionally sensitive operator, the `MadMax'. The temporal evolution of characteristic cases of spicules, dark and bright mottles, indicates an association between them and supports the suggestion that the magnetic field and probably related forces play a fundamental role in their generation and dynamics. We present characteristic cases of fine bright mottles, observable in the Hα far wings, that appear in close juxtaposition to dark mottles. The phenomenon appears to be common, suggesting that the velocities derived from marginal resolution spectroscopic observations could be underestimated. Typical examples of individual mottles crossing the solar limb further support the association between spicules and mottles. Finally we show images of arch-shaped mottles above the limb and especially on the disk, confirming the existence of chromospheric small loops. Our image-processing method substantially enhances near-limb observations and permits an insight into the studies of the very fine chromospheric structures. Title: Brightness Variations of mg ib Bright Features Authors: Dara, H. C.; Koutchmy, S.; Zachariadis, Th. G.; Alissandrakis, C. E. Bibcode: 2001SoPh..198..313D Altcode: We study the temporal intensity variations of Mgib bright features and investigate the corresponding Hα velocity pattern. The network bright features are well visible in the continuum, in images averaged over the duration of the observations (130 min). We detected `flashing' bright features, which appear and disappear within two to five minutes, while the rest of the bright features undergo small variations of either their shape and/or their intensity. A power spectrum analysis reveals a 10-min oscillation for approximately half of the stable bright features. The 5-min oscillations are detected mainly at the network boundaries, where stable bright features are located, while 3-min oscillations coincide with few bright features, but are also quite intense inside the network cells. The majority of bright features are associated with Hα downflows. The downflow is very intense at the location of `flashing' bright features. Title: Helical Magnetic Structure of White Light Polar Plumes Authors: Zhukov, A. N.; Veselovsky, I. S.; Koutchmy, S.; Llebaria, A. Bibcode: 2001IAUS..203..434Z Altcode: We describe the fine structure of white light polar plumes observed by SOHO/LASCO C2coronagraph. The evolving helical structures of different scales are clearly seen on the specifically processed images (the processing reveals the faint contrast objects). The observed structures trace the magnetic field lines, sothe electric currents flow along the axis of the plumes. The MHD model of a plume takinginto account field-aligned electric currents is developed. The model permits to understand the existence of high-density plasma inside the plume due to the balance between the Ampere force and transversal pressure gradient. Consequences for the solar wind acceleration process and for the structure of heliospheric current circuit are discussed. Title: Coronal Streamers Authors: Koutchmy, S. Bibcode: 2000eaa..bookE2271K Altcode: Streamers are the most outwardly extended structures of the solar CORONA; they suggest that a permanent mass flow exists around and further out, inside the furthest parts of streamers. The significance of streamers in the solar corona should be found in the frame of our knowledge of the slow solar wind and of the continuous dissipation of the large-scale solar magnetic field in thin neutral sheet... Title: Oscillations and running waves observed in sunspots. II. Photospheric waves Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S. Bibcode: 2000A&A...363..306G Altcode: To continue our study of waves related to sunspots in the photosphere, we analyzed CCD, high resolution sunspot observations obtained in the Fe i 557.6 nm line. We produced ``time slice images" which reveal inward slow propagating waves in the photospheric penumbra and outward propagating waves in the area around the sunspot. The phase velocity of the waves is near 0.5 km s-1 in both cases and their horizontal wavelength about 2500 km. The waves could be related either to solar p-modes or to the subphotospheric layer large-scale convection. Based on observations performed on the NSO/SPO Dunn's Solar Telescope (DST). Title: On the origin of the prolate solar chromosphere Authors: Filippov, Boris; Koutchmy, Serge Bibcode: 2000SoPh..196..311F Altcode: A simple geometric model is proposed to explain the recently reported effect of the prolateness of the solar chromosphere. We assume that a specific dynamical part of the solar atmosphere above the 2 Mm level, being a mixture of moving up and down jets of chromospheric matter with the coronal plasma between them, is responsible for the solar prolateness. Due to the dynamic nature of this layer, the magnetic field is considered to play a very important role in the density distribution with the height, guiding the mass flows along the field lines. The difference of the magnetic field topology in the polar and the equatorial regions leads to different heights of the chromospheric limb. Calculations show a satisfactory coincidence with observations when the mean separation between opposite polarity concentrations is about 9 Mm. The possible observational signature of this network in low photospheric and chromospheric layers is discussed. Title: Eclipse Science Results: Past and Present (Invited review) Authors: Livingston, W.; Koutchmy, S. Bibcode: 2000ASPC..205....3L Altcode: 2000ltse.conf....3L We have investigated X-ray ejecta above flare loops, which were observed before soft X-ray peak time, using the Yohkoh soft X-ray observations in 1996 when the background corona was very weak. We found 35 plasma ejecta out of 84 flares and studied soft X-ray data to discover the probability to observe the plasma ejecta. On the other hand, we searched for prominence eruptions using Solar-Geophysical Data in the same flare series and found 16 prominence eruptions out of 29 flares having soft x-ray plasma ejecta. As a result, 76% of flares have plasma ejecta observed in either Hα or soft X-ray wavelength. It follows from this that there are many flare associated ejecta. Title: Oscillations and running waves observed in sunspots Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 2000A&A...354..305C Altcode: In order to study umbral oscillations, running penumbral waves and the relationship between them, we analyzed CCD, high resolution, sunspot observations obtained at center and the wings of the Hα line and the Fe I 5576 Ä line. The UBF filter was used in order to produce high cadence sequences of filtergrams. Images were processed to remove the sharp intensity gradient between the umbra and the penumbra. They show the waves to start out around umbral oscillating elements and to propagate outwards forming concentric cycles around the elements. The waves appear to propagate beyond the outer edge of the photospheric penumbra, in the superpenumbra, where they dilute. Comparing images in 9 wavelengths along the Hα profile we found out that the waves are definitely better observed near the Hα center and near the blue wing -0.35 Ä. This indicates a possible vertical upward mass motion in the oscillating penumbral structure and that the oscillation is not symmetric about zero. We found different oscillating modes. Standing umbral oscillations are dominant in the umbra and inner penumbra; their frequency is around 6.5 mHz. Similar oscillations are observed in the penumbra - superpenumbra boundary but with considerably lower frequency (2 mHz). Oscillations are absent or have reduced magnitude in the central part of the penumbra. Penumbral waves are running waves propagating with a constant phase velocity around 13 km s-1; their frequency is remaining constant over the whole penumbra, in the band of 3 mHz. We produced ``time slice images" which show, that there is not a clear relationship between umbral oscillations and running penumbral waves. Title: On Stereoimages of Some Structures in the Solar Atmosphere Authors: Vedenov, A. A.; Koutvitsky, V. A.; Koutchmy, S.; Molodensky, M. M.; Oraevsky, V. N. Bibcode: 2000ARep...44..112V Altcode: Three-dimensional structures in the solar chromosphere and corona are considered. It is demonstrated that two photoheliograms separated by ∼1 day can be used (using computer-graphics methods) to construct a stereo image of the Sun. The algorithm for this is presented and carried out for Hα images of the total disk. A bulge in the equatorial region resulting from the differential rotation of the Sun can be seen in the stereo image. Structures called Whitney pleats in catastrophe theory are observed in the solar corona. Such structures are encountered in prominences. The well-known helmets (or streamers) are pleats of heliospheric plasma sheets. Isophotes for such a sheet and the degree of polarization of the radiation in the pleat are calculated and compared with observational data. Title: Commission 12: Solar Radiation and Structure (Radiation et Structure Solaires) Authors: Foukal, Peter; Solanki, Sami; Mariska, J.; Baliunas, S.; Dravins, D.; Duvall, T.; Fang, C.; Gaizauskas, V.; Heinzel, P.; Kononovich, E.; Koutchmy, S.; Melrose, D.; Stix, M.; Suematsu, Y.; Deubner, F. Bibcode: 2000IAUTA..24...73F Altcode: No abstract at ADS Title: Coronal plasmoid dynamics. II. The nonstationary fine structure Authors: Zhukov, A. N.; Veselovsky, I. S.; Koutchmy, S.; Delannée, C. Bibcode: 2000A&A...353..786Z Altcode: We analyze the non-uniform motion of a white light coronal plasmoid of 1.5 Mm in diameter, which has been followed at the prime focus of the Canada-France-Hawaii Telescope (CFHT) during the July 11, 1991 total solar eclipse. Two possibilities are considered to explain the acceleration of the plasmoid by the magnetic force: large amplitude oscillations and the rotation of the plasmoid magnetic dipole about the external inhomogeneous magnetic field vector. We then describe for the first time the fine structure of the plasmoid, its splitting and its interaction with the surrounding thread-like coronal structures. The smallest-scale inhomogeneities (knots inside the plasmoid) have a characteristic length of about 400 km. The observed complex behaviour of these plasma objects leads us to conclude that existing models of mass supply to the corona by expanding plasmoids and their input into the process of the solar wind acceleration seem to be oversimplified, mainly because the fine structure and the turbulent intermixing have not been realistically taken into account. We also conclude on the importance of dynamical processes at the smallest scales coronal structures when the heating problem is considered. Title: Multiwavelength Observations of Ellerman Bombs Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S. Bibcode: 1999ESASP.448..279G Altcode: 1999mfsp.conf..279G; 1999ESPM....9..279G No abstract at ADS Title: Fine Structure of the Solar Chromosphere: Dynamics of Spicules and Fine Dark Mottles Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S. Bibcode: 1999ESASP.448..285G Altcode: 1999mfsp.conf..285G; 1999ESPM....9..285G No abstract at ADS Title: New Results about Running Penumbral Waves Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 1999ESASP.448..245C Altcode: 1999mfsp.conf..245C; 1999ESPM....9..245C No abstract at ADS Title: Chromospheric Mass Motions Associated with an Emerging Flux Region Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S. Bibcode: 1999ESASP.448..593C Altcode: 1999ESPM....9..593C; 1999mfsp.conf..593C No abstract at ADS Title: Eclipse of August 11, 1999: White-light Images and Simultaneous EIT/SOHO Observations Authors: Adjabshirizadeh, A.; Baudin, F.; Bocchialini, K.; Delaboudinière, J. -P.; Grorod, P. -A.; Koutchmy, S.; Laal Aaly, M.; Lamy, P.; Lochard, J.; Mouette, J. Bibcode: 1999ESASP.448.1283A Altcode: 1999ESPM....9.1283A; 1999mfsp.conf.1283A No abstract at ADS Title: Dynamics and Nature of Macrospicules Authors: Georgakilas, A. A.; Koutchmy, S.; Christopoulou, E. B. Bibcode: 1999ESASP.448..291G Altcode: 1999mfsp.conf..291G; 1999ESPM....9..291G No abstract at ADS Title: L'éclipse du 11 aou^t 1999 et la couronne. Un premier bilan scientifique. Authors: Baudin, F.; Koutchmy, S. Bibcode: 1999LAstr.113..326B Altcode: No abstract at ADS Title: The Prolate Solar Chromosphere Authors: Koutchmy, S.; di Folco, E.; Auchere, F.; Baudin, F.; Delaboudinière, J. -P.; Koutchmy, O.; Noëns, J. -C.; Rondi, S.; Jimemez, R.; Smartt, R. N. Bibcode: 1999ESASP.446..385K Altcode: 1999soho....8..385K The solar prolateness above h=2Mm is now well established from measurements performed during the years of solar minimum in HeII, Hα and K3CaII lines. Low level coronal emissions usually penetrate deep enough to completely mask this effect and show CH, quite similarly to the behaviour of the HeI lines (D3; 1083nm) which does not show the prolateness. We discuss the most recent observations for 1999 given by a new facility developped at Pic du Midi Observatory (HACO II) and we compare the results with EIT results in HeII. We also brielfly discuss the possible interpretations of the prolateness effect. We favor topological effects implying a large number of nano-flares and ejecta during the interactions of small-scale low level network magnetic fields with the more static large-scale magnetic field. Title: Helical Magnetic Structure Of EUV Polar Plumes Authors: Veselovsky, I. S.; Zhukov, A. N.; Koutchmy, S.; Delannée, C.; Delaboudinière, J. -P. Bibcode: 1999ESASP.446..675V Altcode: 1999soho....8..675V The results of an analysis of joint CDS of SOHO and SXT of Yohkoh observations of a decaying post-flare loop system are presented. The SXT images were used to explain some peculiar structural features visible in the examined CDS raster, resulting from the rapid evolution of the observed system and from the way the CDS rasters are built. The SXT data was also used to determine the time evolution of the temperature and the emission measure of the hot part of the system during its decay. The CDS data, with a very good temperature coverage, contains a density sensitive line pair of Fe XIV which was used for electron density analysis and a temperature sensitive line pair of Fe XVI and Si XII which was used to study the temperature structure of the loop system. From the integrated intensities of selected lines the emission measures were calculated. From these measurements we estimated the filling factor of the loop system in Fe XIV line. Title: The Global Activity of the Solar Corona Authors: Llebaria, A.; Lamy, P.; Koutchmy, S. Bibcode: 1999ESASP.446..441L Altcode: 1999soho....8..441L The question of the global activity of the solar corona, as a function of time and distance from the center of the Sun, is considered by analyzing long time-series of LASCO-C2 images. Polarized images are first considered to perform the separation of the K and F components. The F-corona images are used to construct a photometric model of the F-corona wich reflects its annual variations resulting from geometric effects. This time-varying model is then subtracted from all corrected and calibrated images (unpolarized) to yield images of the K-corona. Synoptic maps are created at different distances between 2.5 and 6 solar radii and the total white-light intensity is integrated to estimate the total mass of the corona. Its variations in the range of heliocentric distance and over a time span of 3 years will be presented and discussed. Title: Simultaneous LASCO/1998-Eclipse Observations Of A Large-Scale Polar Event Authors: Zhukov, A.; Koutchmy, S.; Lamy, Ph.; Delaboudinière, J. -P.; Delannée, C.; Bocchialini, K.; Guisard, S.; Filippov, B.; Veselovsky, I. Bibcode: 1999ESASP.446..731Z Altcode: 1999soho....8..731Z A relatively faint but large scale polar region event was observed in Aug. 1996 by Boulade et al. 1998 (SoHO SP 404, 217); we first reconsider this event which has been related to a high latitude filament disappearance. We continue the study of this class of events by analyzing the large scale restructuring which occurred above the N-Pole region at the time of the last Feb. 26, 1998 total solar eclipse. Well calibrated WL-eclipse images are used to provide the absolute values of electron densities of the quasi-radial structure appearing at the feet of the event. This structure can also be considered as a type of abnormally broad and curved polar plume, a type of activity already reported in the literature. Unfortunately, the examination of sequences of EIT images taken at that time seems to indicate that the roots of the structure are on the back side of the Sun. However the most impressive effects are seen in the high polar region, at several radii, based on the analysis of processed Lasco-C2 difference images. Large proper motions are deduced over density structures. Both these events confirm that polar regions are indeed showing a new class of CME activity (possibly related to the Hewish's CMEs), which is seen inside coronal holes. A whole set of interesting questions is then appearing to understand the occurrence of a polar CME propagating in the heart of a large unipolar magnetic region of the corona. Title: Propagating Magneto-Acoustic Waves in the Network Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S. Bibcode: 1999ASPC..184..232B Altcode: The analysis of spectroscopic data taken in the chromospheric network is interpreted as evidence for propagating waves. These waves are seen from the photospheric level propagating upward to the highest levels of the chromosphere at velocities around 40 km/s, suggesting a magneto-acoustic nature. We note the lack of an adequate one-dimensional model of the solar chromosphere to interpret these data. Title: Running Penumbral Waves in Sunspots Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, Serge Bibcode: 1999ASPC..184..103C Altcode: In order to study running penumbral waves, we analyzed high resolution sunspot observations obtained at the center and the wings of the Hα line. The sharp intensity gradient between the umbra and the penumbra has been removed by using an image processing technique. The processed images show the waves to start out from the umbral oscillating elements and to propagate outwards forming concentric circles around the elements. The propagation velocity is between 6 to 18 km s1; and the average period is about 190 sec. Title: Coordinated observations between SOHO/SUMER and ground during the 1998 total eclipse: Non-thermal line broadenings and electron densities in a polar coronal hole Authors: Patsourakos, S.; Vial, J. -C.; Gabryl, J. -R.; Koutchmy, S.; Schühle, U. Bibcode: 1999AIPC..471..285P Altcode: 1999sowi.conf..285P Alfvén waves represent one of the most prominent ways of heating the solar corona and accelerating the solar wind. One of their signatures is to broaden the spectral lines in excess of their thermal width. Here we aim to combine observations of non-thermal broadenings measured by SUMER in OVI (1037.6 Å) line and electronic densities derived from white-light observations during the 1998 total eclipse. After checking the validity of the frequently-used assumption of equal ion and electron temperatures, we compute the variation of the non-thermal velocity as a function of height in an interplume region within the south polar coronal hole. Title: Erratum: "Fine structure of the solar chromosphere: arch-shaped mottles" [Sol. Phys., Vol. 184, No. 1, p. 77 - 86 (Jan 1999)]. Authors: Zachariadis, T. G.; Georgakilas, A. A.; Koutchmy, S.; Dara, H. C.; Alissandrakis, C. E. Bibcode: 1999SoPh..187..227Z Altcode: No abstract at ADS Title: L'imagerie haute résolution. Pourquoi et comment? Authors: Koutchmy, S. Bibcode: 1999LAstr.113..116K Altcode: No abstract at ADS Title: Eclipse 99: l'imagerie haute résolution: pourquoi et comment? Authors: Koutchmy, S. Bibcode: 1999C&T...115...82K Altcode: No abstract at ADS Title: Steady-state configuration of the heliospheric sheet Authors: Koutchmy, S. L.; Molodensky, M. M.; Matsuura, O. T.; Picazzio, E. Bibcode: 1999AstL...25..258K Altcode: An analysis of the coronal structure for several eclipses, including the eclipse of November 3, 1994, shows that coronal streamers and helmets can be described as folds and pleats produced when the B_r = 0 plane is projected onto the plane of the sky (Vial and Molodensky 1993; Molodensky et al. 1996). We consider equilibrium conditions for plasma in the heliospheric sheet from the corona base out to distances of several R_solar. We construct an analytic model that represents the equilibrium configuration of plasma near the equatorial plane of the equivalent dipole. This model is characterized by two parameters: the sheet thickness 1/k (radians) and M/qR_solar. We show the following: (1) the current in the sheet is opposite in sign to the current that produces the initial dipole moment of the Sun, and (2) the parameter that determines the sheet thickness is k = 20. The temperature, the density, and the magnetic field match the real values of the corresponding parameters in the corona. Title: Eclipse 99 -- High Resolution Imaging: Why and how? Authors: Koutchmy, S. Bibcode: 1999CoSka..28..173K Altcode: A very large white-light (W-L) coronal flux is made available during total eclipses. High speed analysis of very fine-scale structures of the magnetically dominated solar atmosphere is then possible, including the deeply seeded sources of the solar mass loss. Additional observations of both the disk and of the more outer corona should be simultaneously collected from space, using the SOHO and the Yohkoh missions to complement the data. The most optimum eclipse studies should concentrate on the intermediate corona where acceleration processes are taking place. MHD waves, including magneto-acoustic propagating waves and standing loop-resonance waves are everywhere present with rather short periods. W-L fine imaging at high-speed and high signal-noise ratio is needed to avoide the overlapping problem and measure their magnitude. Ubiquitous plasmoid-like objects are also produced in this region near the temperature maximum and they need a special attention. They are the rather privileged site where both the radiative cooling and the magnetic dissipation mechanisms are occuring. Eclipses are good opportunities to look at the dynamics of coronal ejecta. At larger scale, sharp edges of streamers and plumes can be used to deduce a 3-D view of the coronal neutral sheets, provided pictures taken at several hours interval are made available along the path of the totality. Both the quasi-rigid rotation and the more subtil outward motions of coronal material are then evidenced, giving a good tool to study the origine of the slow wind. Title: The plane of polarization of the solar corona during eclipse observations Authors: Koutchmy, S.; Matsuura, O.; Molodensky, M. M.; Picazzio, E.; Starkova, L. I. Bibcode: 1999ARep...43..198K Altcode: Analyses of the orientation of the plane of polarization for the solar corona are presented, based on polarization isophotes of the solar eclipses of June 30, 1973 (Africa), November 3, 1994 (Brazil), and March 9, 1997 (Eastern Siberia). Deviations of the polarization plane from the radial direction, indeed, exist at distances from the solar limb greater than 0.5 R_solar. These deviations cannot be explained by the aberration of scattered photons on moving coronal electrons or by F-corona emission. It is proposed that the deviations are produced by sky polarization (the auroral ring), i.e., by Rayleigh scattering in the Earth's atmosphere during the eclipse. A model of the total emission of the corona taking into account the sky background is constructed, and the positions of singular points of the polarization tensor with topological index -1/2 are indicated. Title: Polar surges and macrospicules: simultaneous Hα and He BT II 304 Angstroms observations Authors: Georgakilas, A. A.; Koutchmy, S.; Alissandrakis, C. E. Bibcode: 1999A&A...341..610G Altcode: We compare simultaneous sequences of Hα and He ii 304 Angstroms images near the solar limb. We propose to distinguish polar surges and giant spicules (macrospicules), among the He ii structures observed beyond the solar limb. Polar surges have a complex structure when observed in Hα and an eruptive nature, reminiscent of normal surges in small scale. Giant spicules are simple spikes, very narrow compared to surges. They don't go as high as polar surges and apparently have shorter lifetimes. We found that most polar surges and giant spicules observed in He ii are associated with Hα spikes; however there were cases without any corresponding Hα structure. Furthermore we observed Hα spikes that did not have He ii counterparts. We analyze an example of a polar surge that appeared in He ii well before its appearance in Hα and remained visible for a longer time. Most polar surges that we observed showed a similar behavior. Title: Mg bright points and the corresponding velocity pattern. Authors: Dara, H. C.; Zachariadis, T.; Alissandrakis, C.; Koutchmy, S. Bibcode: 1999joso.proc..135D Altcode: The authors study the temporal intensity variations of the Mg b1 bright points, in an effort to detect oscillations and investigate the corresponding Hα velocity pattern. Apart from the "flashing bright points", bright points which appear and disappear within two to three minutes, the rest of the bright points undergo small intensity variations. Power spectrum analysis revealed a 10-min oscillation for half of the stable bright points. The 5-min oscillations are detected mainly at sites where there are no bright points, while 3-min oscillations coincide with some of the bright points. The majority of the bright points are associated with Hα downflows. The downflow is very intense at the "flashing bright points". Title: Outflow Velocities at the Base of a Polar Coronal Hole During the 1998 Total Eclipse Authors: Patsourakos, S.; Vial, J. -C.; Gabryl, J. -R.; Koutchmy, S.; Schühle, U. Bibcode: 1999SSRv...87..291P Altcode: Polar coronal holes represent the most convincing site from which the high-speed solar wind originates. Here we report high-accuracy Doppler shifts measured in the O VI (1037.6 Å) line obtained by SUMER on SOHO inside an interplume region within the south polar coronal hole. We infer limits on the outflow velocity and draw hints about the flow geometry. Title: Large-Scale Polar Coronal Magnetic Field Model and the Expected August 11, 1999 Eclipse Corona Authors: Veselovsky, I. S.; Zhukov, A. N.; Panassenko, O. A.; Koutchmy, S. Bibcode: 1999RoAJ....9S..29V Altcode: We compare available SOHO/LASCO C2 images with the model calculations of the large-scale coronal magnetic field near the magnetic poles of the Sun. The model field consists of the ones of the dipole and of the thin current sheet in the plane perpendicular to the dipole. The positions of the dipole and the current sheet (representing the heliospheric current sheet) are obtained via comparison of the SOHO/LASCO, SOHO/EIT observations and coronal magnetic field calculations (Wilcox Solar Observatory). The values of the solar dipole vector components are taken from the same calculations of the coronal magnetic field. The strength of the heliospheric current sheet is obtained via analyses of the interplanetary magnetic field preliminary data from the ACE spacecraft. This model is better applicable during the solar cycle minimum. However, the obtained model polar magnetic field is in agreement with the observations near the solar maximum, when the polar plumes could be visible over the magnetic (and not heliographic) poles of the Sun if the magnetic dipole is perpendicular to the line of sight. The configuration of the solar corona during the August 11, 1999 total solar eclipse expected from our analysis does not contain polar plumes and will be close to the maximal-shape corona dominated by coronal rays and streamers. Title: Total eclipses : science, observations, myths, and legends Authors: Guillermier, Pierre; Koutchmy, Serge Bibcode: 1999teso.conf.....G Altcode: No abstract at ADS Title: Fine structure of the Solar Chromosphere: Arch-Shaped Mottles Authors: Zachariadis, Th. G.; Georgakilas, A. A.; Koutchmy, S.; Alissandrakis, C. E.; Dara, H. C. Bibcode: 1999SoPh..184...77Z Altcode: We analyze a time series of high resolution observations near the solar limb, obtained in Hα and the Mg b1 line. We identified arch-shaped dark mottles, which are thin, faint Hα structures observable under very good seeing conditions, best seen in Hα +0.75 Å. Their mean length is about 15'', their mean height about 6'' and indicative lifetimes is of the order of 5 min. They show negative (away from the observer) line-of-sight velocities. A possible interpretation is that material flows from the apex towards the feet of the arches. Title: SOPHIE: a solar EUV multilayer reflecting coronagraph Authors: Hassler, Donald M.; Slater, David C.; Smartt, Raymond N.; Koutchmy, Serge L. Bibcode: 1998SPIE.3443...61H Altcode: SOPHIE (Solar Photometric Helium Imaging Experiment) is a design for a new space-borne EUV multi-layer reflecting coronagraph to obtain full coronal field-of-view (solar disk and 1.1 to 3.0 solar radii above the limb) observations in He II 304 angstrom, and to measure the coronal helium abundance as a function of structure and time in the corona. Knowledge of the coronal helium abundance is fundamental to understanding the dynamics of the solar wind acceleration region, yet its value is not well known. SOPHIE will open up a new observational domain by providing full field-of-view coronagraph observations of helium, as opposed to electrons observed with traditional white light coronagraphs. Moreover, it has been recognized in the last several years that time variable phenomena is important and relevant to every aspect of the transition region and corona. Title: High Resolution Analysis of the Eclipse Solar Corona Authors: Koutchmy, S. Bibcode: 1998jena.conf...13K Altcode: A very large W-L coronal flux is made available during total eclipses. High speed analysis of very fine-scale structure of the magnetically dominated solar atmosphere is made possible, including the deeply seeded sources of the solar mass loss.

Additional observations of both the disk and of the more outer corona should be simultaneusly collected from space, using the SOHO and the Yohkoh missions to complements the data.

The most optimum eclipse studies should concentrate on the intermediate corona where acceleration processes are taking place. MHD waves, including magneto-acoustic propagating waves and standing loop-resonance waves are everywhere present with rather short periods. W-L fine imaging at high signal-to noise ratio is needed to avoid the overlapping problem and measure their magnitude. Ubiquituos plasmoid like objects are also produced in this region near the temperature maximum and they need a special attention. They are rather privileged site where both the radiation cooling and the magnetic dissipation mechanisms are occurring. Eclipses are good opportunities to look at the dynamics of coronal ejections.

At larger scale, sharp edges of streamers and plumes can be used to deduce a 3-D view of the corona neutral sheets, provided pictures taken at several hours interval are made available along the path of the totality. Both the quasi-rigid rotation and the more subtle outward motions of coronal material are then evidenced, giving a good tool to study the origin of the slow wind. Title: The prolate solar chromosphere Authors: Auchere, F.; Boulade, S.; Koutchmy, S.; Smartt, R. N.; Delaboudiniere, J. P.; Georgakilas, A.; Gurman, J. B.; Artzner, G. E. Bibcode: 1998A&A...336L..57A Altcode: We present a comparative analysis of the chromospheric solar limb prolateness, using strictly simultaneous H_alpha ground-based observations and Heriptsize{II} space-based observations. The typical prolateness is found to be Delta D/D=5.5*E(-3) in Heriptsize{II} and 1.2*E(-3) in H_alpha . The first measurements in the 30.4 nm Heriptsize{II} line over a period of two years, as well as coronal data, are discussed to explore further the origin of the prolateness and its possible consequences. Title: Advances in ground-based and space-based reflecting coronagraph designs Authors: Smartt, Raymond N.; Koutchmy, Serge L. Bibcode: 1998SPIE.3352..614S Altcode: A program to develop ground-based emission-line solar coronagraphs based on super-polished primary objective mirrors has been underway at the National Solar Observatory/Sacramento Peak over the last several years. The fundamental design requirements for effective coronagraph performance are discussed. The instrument currently under development has a 60-cm diameter objective with a 700-cm primary focal length. This design has been refined with an emphasis on achieving an extremely low level of instrumental stray light, suitable for both visible and IR operation and for carrying out high-precision polarimetry. It is seen as a possible prototype for a new generation of much larger aperture, low-scattered-light solar telescopes. Special applications include measurements of the signatures of waves in coronal loops, transient events such as coronal loop interactions, the spatial variation of magnetic fields in prominences allowing computation of electric currents, and the determination of the magnitude of coronal magnetic fields. For applications in space, a white-light reflecting coronagraph has been developed under the USAF program, SWATH (Space Weather and Terrestrial Hazards). This novel catadiopric design has a 10-cm diameter superpolished primary objective mirror, and a unique external occulter. It has a significantly higher throughput and resolution as compared with conventional space-borne lens-objective coronagraphs. Two basic modifications of this design are proposed that result in an in-line symmetric configuration, with a decrease in mass, while improving the scattered-light performance. Some special applications are described. Title: Chromospheric heating by electric currents induced by fluctuating magnetic elements Authors: Lorrain, Paul; Koutchmy, Serge Bibcode: 1998SoPh..178...39L Altcode: 1998SoPh..178..477L We refer to two papers by Goodman (1995, 1996) on the heating of the chromosphere by large-scale electric currents, and to our paper (Lorrain and Koutchmy, 1993) on magnetic elements. Goodman assumes that the dynamo that runs a magnetic element stops operating at t = 0. From then on, the magnetic field decays exponentially, and the induced currents heat the chromosphere. The time constants calculated by Goodman disagree with the observed values, possibly because he disregards the driving dynamo. Also, he assumes static conditions, but his magnetic force density appears suddenly when the dynamo stops, and it is about equal to the gravitational force density. The magnetic force acts downward and fluctuations in the current flowing through the magnetic element should induce vertical oscillations at the photosphere. This point should be investigated further. Title: Cor-I: a coronal white-light imager for a solar probe Authors: Vial, J. -C.; Koutchmy, S.; Habbal, S. R. Bibcode: 1998AdSpR..21..291V Altcode: Solar and heliospheric observations acquired over several decades, have shown that the corona is a highly structured medium. There is no doubt that these structures reflect the response of the coronal plasma - confined by the highly inhomogeneous magnetic field - to different forms of energy input. While in-situ plasma measurements have provided the characteristic properties of both fast and slow solar winds, they have fallen short in connecting them to the source regions of the wind. A near-Sun flyby mission offers an unprecedented opportunity to explore the solar wind at distances much closer to the Sun than ever achieved before. However, it is essential that in-situ measurements be coordinated with simultaneous imaging of the structures encountered in the corona. We present the concept and design of a white-light imager called Cor-I, as a key instrument for a near-Sun flyby mission which makes it possible to distinguish spatial structures from temporal changes in the plasma parameters. With the inference of the electron density from the Thomson scattered emission, white-light measurements are also a very powerful tool for quantitative studies of the acceleration region of the solar wind. In addition, the proposed instrument carries the potential for discovery of transient events and waves in these parts of the acceleration region of fast and slow solar winds that are inaccessible to in-situ plasma instruments. Title: A Model of Plasma Sheets in Equilibrium Authors: Koutchmy, S.; Molodensky, M.; Vibert, D. Bibcode: 1998ASPC..150..127K Altcode: 1998IAUCo.167..127K; 1998npsp.conf..127K No abstract at ADS Title: Corona of the polar regions Authors: Starkova, L.; Molodensky, M.; Kouvitsky, Vi.; Koutchmy, S. Bibcode: 1998ESASP.421..317S Altcode: 1998sjcp.conf..317S No abstract at ADS Title: Solar plume formation in the solar corona Authors: Veselovsky, I. S.; Panassenko, O. A.; Koutchmy, S. Bibcode: 1998ESASP.421..345V Altcode: 1998sjcp.conf..345V No abstract at ADS Title: The polar extension of the solar chromosphere Authors: Auchère, F.; Delaboudinière, J. P.; Koutchmy, S.; Boulade, S. Bibcode: 1998ESASP.421..245A Altcode: 1998sjcp.conf..245A No abstract at ADS Title: About polar ejection events and surges Authors: Loucif, M. L.; Koutchmy, S.; Stellmacher, G.; Georgakilas, A.; Bocchialini, K.; Delaboudinière, J. -P. Bibcode: 1998ESASP.421..299L Altcode: 1998sjcp.conf..299L No abstract at ADS Title: Wave Activity and Prominence Eruption Authors: Baudin, F.; Bocchialini, K.; Delannee, C.; Koutchmy, S.; Stellmacher, G.; Shibata, K.; Veselovsky, I. S.; Panasenko, O. A.; Zhukov, A. N. Bibcode: 1998ASPC..150..314B Altcode: 1998IAUCo.167..314B; 1998npsp.conf..314B No abstract at ADS Title: Coronal plasmoid dynamics. I. Dissipative MHD approach Authors: Delannee, C.; Koutchmy, S.; Veselovsky, I. S.; Zhukov, A. N. Bibcode: 1998A&A...329.1111D Altcode: Energy and momentum balance equations of the dissipative MHD approach are applied to the coronal plasmoid phenomenon observed with the Canada-France-Hawaii Telescope during the July 11, 1991 total solar eclipse. The situation is marginal for the applicability of the MHD description,which has been used for orders of magnitude estimates of the governing physical parameters. Their analysis confirms the suggestion about the possibility for a relatively cold but rapidly moving plasma body to heat the corona through dissipative viscous effects. It also shows that magnetic stresses, gas pressure gradients and viscous drags by the fast plasma flows from the chromosphere are viable candidates to lift the plasmoid against the gravity force. Title: Properties of Hα spicules from disk and limb high-resolution observations Authors: Dara, H. C.; Koutchmy, S.; Suematsu, Y. Bibcode: 1998ESASP.421..255D Altcode: 1998sjcp.conf..255D No abstract at ADS Title: SXR Coronal Polar Jets and Recurrent Flashes Authors: Koutchmy, S.; Hara, H.; Shibata, K.; Suematsu, Y.; Reardon, K. Bibcode: 1998ASSL..229...87K Altcode: 1998opaf.conf...87K No abstract at ADS Title: Foreword Authors: Koutchmy, S.; Martens, P.; Shibata, K. Bibcode: 1998ESASP.421...14K Altcode: 1998sjcp.conf...14K No abstract at ADS Title: Time domain analysis of polar plumes observed with LASCO-C2 and EIT Authors: Llebaria, A.; Lamy, P.; Deforest, Ce.; Koutchmy, S. Bibcode: 1998ESASP.421...87L Altcode: 1998sjcp.conf...87L No abstract at ADS Title: Spicules and Macrospicules: Simultaneous Hα and He II (304 Å) Observations Authors: Georgakilas, A. A.; Dara, H.; Zachariadis, Th.; Alissandrakis, C. E.; Koutchmy, S.; Delannée, C.; Delaboudinière, J. -P.; Hochedez, J. -F. Bibcode: 1998ASPC..155..376G Altcode: 1998sasp.conf..376G No abstract at ADS Title: Coronal Plasmoid Dynamics Authors: Delannee, C.; Koutchmy, S.; Zhukov, A.; Veselovsky, I. Bibcode: 1998ASPC..150..388D Altcode: 1998npsp.conf..388D; 1998IAUCo.167..388D No abstract at ADS Title: White-light polar plumes from solar eclipses Authors: Koutchmy, S.; Bocchialini, K. Bibcode: 1998ESASP.421...51K Altcode: 1998sjcp.conf...51K No abstract at ADS Title: European Plans for the Solar/Heliospheric Stereo Mission Authors: Bothmer, V.; Bougeret, J. -L.; Cargill, P.; Davila, J.; Delaboudiniere, J. -P.; Harrison, R.; Koutchmy, S.; Liewer, P.; Maltby, P.; Rust, D.; Schwenn, R. Bibcode: 1998ESASP.417..145B Altcode: 1998cesh.conf..145B No abstract at ADS Title: Coronal jet turbulent activity to explain distorted emission line Authors: Loucif, M. L.; Ben Jaffel, L.; Koutchmy, S.; Vial, J. -C. Bibcode: 1998ESASP.421..303L Altcode: 1998sjcp.conf..303L No abstract at ADS Title: Polar jets and plasmoids:Results from JOP 57 Authors: Delannee, C.; Koutchmy, S.; Delaboudiniere, J. -P.; Hochedez, J. -F.; Vial, J. -C.; Dara, H.; Georgakilas, A. Bibcode: 1998ESASP.421..129D Altcode: 1998sjcp.conf..129D No abstract at ADS Title: Kinematics of Hα spicules from near-limb observations. Authors: Zachariadis, T. G.; Georgakilas, A. A.; Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1998joso.proc..126Z Altcode: The authors have studied the behavior of dark mottles near the solar limb. After the corrections for flat field and limb darkening the authors can identify spicules crossing the solar limb. Most of the mottles initially show an ascending velocity which gradually turns to descending. Moreover, the authors observe a group of dark mottles which have the shape of arches. One of the footpoints of the arch is in a chromospheric network cell, while the other in a nearby rosette. Title: Flashing Mgb1 bright points. Authors: Dara, H. C.; Georgakilas, A.; Zachariadis, T.; Alissandrakis, C.; Koutchmy, S. Bibcode: 1998joso.proc..124D Altcode: High resolution observations, obtained at the Sacramento Peak Observatory near the solar limb, are analysed for the study of the evolution of Mgb1 (5183.22 Å) bright points, as well as their association to bright features in the continuum (5256.40 Å) and Hα wings (±0.75 Å). The authors have detected stable bright points from the beginning to the end of the time series which hardly move and whose shape undergoes small changes, bright points whose brightness increases and decreases periodically, and bright points which suddenly appear and disappear within one or two minutes. Title: La mission SoHO vers un nouveau Soleil? Authors: Baudin, F.; Koutchmy, S. Bibcode: 1997LAstr.111..286B Altcode: No abstract at ADS Title: The heliospheric layer and the coronal structure on November 3, 1994 Authors: Koutchmy, S.; Molodenskii, M. M.; Starkova, L. I.; Kutvitskii, V. A.; Ershov, A. V.; Ivanov, A. A.; Petrov, B. B.; Sidorov, C. C. Bibcode: 1997AstL...23..818K Altcode: 1997PAZh...23..939K No abstract at ADS Title: Granulation and magnetism in the solar atmosphere. Authors: Baudin, F.; Molowny-Horas, R.; Koutchmy, S. Bibcode: 1997A&A...326..842B Altcode: The properties of the photosphere in magnetic and non magnetic regions, at two levels in the solar atmosphere, have been studied, using two virtually simultaneous time sequences of 109 mn duration of CCD images taken at the Vacuum Tower Telescope of the Sacramento Peak Observatory. The selected wavelengths correspond to the true continuum and to the wing of the MgIb_1_ line, where brightenings are taken as proxies of magnetic elements. Averaged intensities, intensity fluctuations and horizontal motions in different regions and levels of the photosphere have been compared. We obtained various results concerning: the intensities inside and outside an active region showing different behaviours; the granulation keeping a kind of remnant structure at the continuum level; the mapping of proper motions of the granules imaged in the continuum outlining clearly the super-granular cells in the deepest layers of the photosphere; the ``freezing'' influence of the magnetic field on these motions in active regions; and the temporal variation of the correlation between images at the two heights indicating that intensity variations at the higher level precede those of the lower one. These results are briefly discussed and compared with previous ones and with published model calculations. Title: Fine Structure of the solar atmosphere from near-limb observations in three wavelengths Authors: Georgakilas, A. A.; Dara, H.; Zachariadis, Th.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1997SoPh..172..133G Altcode: 1997ESPM....8..133G We analyze a time series of high-resolution observations near the limb, in the continuum, in the Mg b1 line (-0.4 Å off line center), and in the wings of Hα (+0.75 Å). The observations were obtained with a CCD camera at the Vacuum Tower telescope of the Sacramento Peak Observatory. We study the association of facular points, as they appear at different heights of the solar atmosphere (continuum, b1 - 0.4 Å, Hα + 0.75 Å) with the feet of fine dark mottles. Title: SXR Coronal Flashes. Authors: Koutchmy, S.; Hara, H.; Suematsu, Y.; Reardon, K. Bibcode: 1997A&A...320L..33K Altcode: We provide evidence for the existence of a new type of soft X-ray (SXR) brightening event that we call coronal flashes. The phenomenon was observed on deep time series taken with the SXT of Yohkoh in the north polar coronal hole, near the sunspot minimum. Events last as short as 1.5 mn and the corresponding SXR flux span the range of energies, from single pixel brightenings corresponding to fluxes of about 10^24^erg but barely surpassing the level of the noise, to higher and more smeared multiple px brightenings still orders of magnitude smaller than the known small SXR bright points and/or transient brightenings. The typical occurrence rate of flashes is 1-event/arcmin^2^/5mn with a 1/2mn integration time. At least part of the coronal flashes are recurrent and some of them could be associated with a SXR jet; it is not clear what is their optical counterpart. Title: Eclipse WL polar plumes: what is the connection with the disk activity? Authors: Koutchmy, Serge; Bocchialini, Karine Bibcode: 1997AIPC..385..137K Altcode: 1997recs.conf..137K We discuss both the origin and the role that eclipse WL-polar plumes could have in the context of the coronal hole physics: densities, temperatures and flows. Some new results coming from the campaigns of the 1994 and 95 eclipses are reported and YOHKOH data are also taken into account. Title: Distribution on halfwidths for the green coronal line (5303 Å). Authors: Alexeeva, I. V.; Kim, I. S.; Matsuura, O. T.; Picazzio, E.; Koutchmy, S. Bibcode: 1997ASIC..494....7A Altcode: 1997topr.conf....7A Distribution on halfwidths for Fe XIV (5303 Å) coronal line is analyzed. The Fabry-Perot interferogram obtained during the total solar eclipse of November 3, 1994 is used. The profiles not distorted by the white light corona contributions as well as by ghost images were selected. A multimodality with probability of 87% is found in the histogram. Average values of halfwidths differ for different coronal structures (0.91 Å for SW-helmet, 0.85 Å for NW and 0.81 Å for SE coronal regions). An evident increase of the halfwidths with distance is revealed for SW-helmet structure. Title: Polar Jets and Plasmoids: Preliminary Results from JOP 57 Authors: Delannée, C.; Koutchmy, S.; Delaboudiniè, J. -P.; Hochedez, J. -F.; Vial, J. -C.; Dara, H.; Georgakilas, A. Bibcode: 1997ESASP.404..327D Altcode: 1997cswn.conf..327D No abstract at ADS Title: Characterisation of Polar Plumes from LASCO-C2 Images in Early 1996 Authors: Lamy, P.; Liebaria, A.; Koutchmy, S.; Reynet, P.; Molodensky, M.; Howard, R.; Schwenn, R.; Simnett, G. Bibcode: 1997ESASP.404..487L Altcode: 1997cswn.conf..487L No abstract at ADS Title: Coronal physics inferred from the analysis of fine structures. Authors: Koutchmy, S. Bibcode: 1997ASIC..494...39K Altcode: 1997topr.conf...39K Solar total eclipses are rare occasions offering the opportunity to make a snapshot of the solar corona. The availability of a large radiative flux makes sophisticated methods usefull to analyse all parts of the highly structured white-light corona. Coronal absolute intensities and line emissions, including their polarization, are also studied to analyse density and temperature inhomogeneities, velocities and magnetic fields. Detailed density distribution is directly extracted for fine coronal structures. During the July 11, 1991 eclipse, the large 3.6 m aperture CFH optical telescope was used to analyse time sequences over small coronal fields and to image the finest structures never seen; results from this experiment are presented with emphasis on small-scale dynamical plasma processes including wave-phenomena. Finally, the author gives an overview of what is known on coronal structures from eclipse observations: temperatures, densities, velocities, occurrence and structure of streamers, coronal holes, threads, etc. Title: Analysis of a High Latitude Slow CME with Travelling Ejecta Authors: Boulade, S.; Delanné, C.; Koutchmy, S.; Lamy, P.; Llebaria, A.; Howard, R.; Schwenn, R.; Simnett, G. Bibcode: 1997ESASP.404..217B Altcode: 1997cswn.conf..217B No abstract at ADS Title: Mais où est passé le nouveau cycle d'activité solaire? Authors: Koutchmy, S. Bibcode: 1997LAstr.111....4K Altcode: Depuis plus d'un an les astrophysiciens solaires du monde entier analysent les magnétogrammes du soleil pour détecter les signes annonciateurs du nouveau cycle d'activité du Soleil, cycle qui portera le numéro 23. Title: Degree polarization distribution in the solar corona of 03 November 1994. Authors: Belenko, I. A.; Bougaenko, O. I.; Kim, I. S.; Koutchmy, S.; Matsuura, O. T.; Picazzio, E. Bibcode: 1997ASIC..494...15B Altcode: 1997topr.conf...15B Preliminary data reduction of the color index polarization wave experiment carried out in Brazil (Chapeco town) is described. Distributions of polarization degree (polarization images) in the range 1.1 - 1.6 Rsun are obtained by an algorithm developed on the basis of the Stokes vector presentation and IDL software. The polarization image of the "quasi-white-light" corona (summary of the blue and red spectral region emissions) is analyzed. On the average, no fit is found with the van de Hulst model for the inner corona at heliographic latitudes of ±45°. The polarization degree reaches a plateau at 1.2 - 1.35 Rsun. Title: High frequency magneto-acoustic waves in the chromosphere Authors: Bocchialini, Karine; Koutchmy, Serge Bibcode: 1997AIPC..385..153B Altcode: 1997recs.conf..153B From a time series taken over the disk center network and cell elements in different chromospheric and photospheric lines, we discuss the possible detection of wave-trains corresponding to frequencies higher than the 7 mHz frequency of the familiar chromospheric 3 mn oscillations. Their analysis would greatly benefit from observations taken with an improved spatial resolution, free of seeing effects which limit the precision in ground-based measurements. Title: The three-dimensional structure of the corona on November 3, 1994 Authors: Molodenskii, M. M.; Starkova, L. I.; Koutchmy, S.; Ershov, A. V. Bibcode: 1996ARep...40..848M Altcode: No abstract at ADS Title: The polarization and 3-D structure of the corona on 11.3.94 Authors: Koutchmy, S.; Molodenskii, M. M.; Starkova, L. I.; Kutvitskii, V. A.; Ershov, A. V. Bibcode: 1996R&QE...39..921K Altcode: We present the results of observations of the white-light corona in polarized light (Criciuma, Brazil) in 1994. The space location of the surface Br=0 is calculated using the synoptic map of filaments during the solar eclipse. A good agreement was found between the corona ray structure and the surface folds and pleats, which result from its projection onto the sky plane. The measured polarization degree is compared with calculations by the Van de Hulst model. A conclusion is made concerning the adequacy between the proposed model and the observation data. Title: MHD Shock Interactions in Coronal Structures Authors: Grib, S. A.; Koutchmy, S.; Sazonova, V. N. Bibcode: 1996SoPh..169..151G Altcode: We consider the magnetohydrodynamic (MHD) interactions of solar coronal fast shock waves of flare and/or nonflare origin with the boundaries of coronal streamers and coronal holes. Boundaries are treated as MHD tangential discontinuities (TD). Different parameters of the observed corona are used in the investigation. The general case of the oblique interaction is studied. Title: Propagating magneto-acoustic waves in the solar chromosphere. Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S. Bibcode: 1996A&A...314L...9B Altcode: We report on spectroscopic one dimensional observations showing for the first time upward propagating 5mn period waves, which emerge from the deep chromospheric network. Wavetrains are well measured at the height where the He I line (at A=1083nm) is formed by the coronal back radiation. We also present results from a time series of narrow filtergrams of a quiet region at the disk center. The two dimensional mapping of the power of waves observed in the chrormosphere shows the familiar cell-like distribution corresponding to the network magnetic field pattern. In addition, Fourier components with significantly longer periods than 5mn were detected in the chromospheric network. We suggest that the waves propagating in the open corona are reminescent of photospheric oscillations transmitted by the magnetic field of the chromospheric network. Title: White-Light Coronal Dark Threads and Density Fine Structure Authors: November, Laurence J.; Koutchmy, Serge Bibcode: 1996ApJ...466..512N Altcode: High spatial resolution white-light coronal observations from the eclipse of 1991 July 11 taken with the 3.6 m Canada-France-Hawaii Telescope on Mauna Kea are the best ever achieved because of the unique opportunity of observing the totally eclipsed Sun with a large aperture telescope. Photometric calibration of the photographic data is verified by the average radial intensity variation, which agrees with the classical function. Dividing out the average radial variation, we identify relatively dark and bright fine "threads" with enhanced spatial power in the range of 1-5 Mm. Spatial filtering using unsharp masking or "mad-max" algorithms clearly shows relatively dark and bright radial threads in loops as fine as the resolution limit of about 1 Mm. The main feature is an arcade of concentric dark and bright threads that extend above a small prominence just above the limb. A small coronal cavity near the prominence contains numerous fine dark threads. The relative electron-density depletion and enhancement required to explain the observed thread contrast, assuming that they are isolated cylindrically symmetric structures, is found to be ΔNe/Ne ∼ ± 100%, indicating that the dark threads are fully evacuated. An excess of approximately 1 G field strength in stationary non-force-free magnetic fields can produce the observed thread contrast. Evacuated threads representing non-force-free magnetic fields introduce special constraints on the coronal thermodynamics. Title: Two Dynamical Models for Solar Spicules Authors: Lorrain, Paul; Koutchmy, Serge Bibcode: 1996SoPh..165..115L Altcode: Solar spicules are luminous jets that erupt up to 10 000 km from the surface of the Sun and have diameters, all along their length, of only about 150-200 km. We first review some recent observations made at the Hα wavelength. According to our models, a solar spicule is a self-channelled proton beam emitted by a magnetic element and surrounded by a cold sheath. The beam originates in a self-excited dynamo that exploits a v × B field and that could be situated either below or above the element, where v is the local plasma velocity and B is the local magnetic flux density. In falling back, the sheath provides a return current of protons that cancels the outgoing current. We discuss the channelling of charged-particle beams of very large cross-section and propose velocity channelling, which is apparently a new concept. We assume a steady state and a hydrogen plasma. Title: L'ère SoHO a commencé. Authors: Baudin, F.; Koutchmy, S. Bibcode: 1996JAF....53...10B Altcode: No abstract at ADS Title: A coronal optical imager for a solar probe Authors: Lamy, P.; Koutchmy, S. Bibcode: 1996AdSpR..17c..95L Altcode: 1996AdSpR..17...95L A Coronal Optical Imager (COI) can make a significant contribution to a solar probe, for instance, by detecting the faintest plasma and magnetic structures, by analyzing the He/H ratio and the cool plasma component and by observing possible sources of dust near the Sun. We describe an instrument which combines the capability of EUV, UV and visible imaging as well as visible polarimetry, and propose two versions respectively adapted to a spinning and a 3-axis stabilized probes. Title: 3-D Structure of Heliospheric Current Sheet Deduced from Eclipse Observations Authors: Molodensky, Michael M.; Starkova, Lidia I.; Koutchmy, Serge L.; Ershov, Andre V. Bibcode: 1996ASPC...95..385M Altcode: 1996sdit.conf..385M No abstract at ADS Title: A coronal plasmoid crossing a magnetic structure. Authors: Delannee, C.; Koutchmy, S. Bibcode: 1996CRASB.322...79D Altcode: The authors observed, during the solar eclipse in 1991, a coronal plasmoid. They analyzed the trajectory, the dynamic and radiative flux variation of the plasmoid. The motion is upward and decelerated. The flux presents a strong decrease. The plasmoid appears to go across a structure, which is supposed to follow the local magnetic field. It travels across the magnetic field line; this is not in agreement with the theory of the "melon seed" acceleration and additional forces are needed to explain the motion. Title: On the three-dimensional structure of the solar corona Authors: Koutchmy, S.; Ershov, A. V.; Molodenskii, M. M. Bibcode: 1996ARep...40..109K Altcode: No abstract at ADS Title: 1995: une éclipse en Indochine. Authors: Koutchmy, S. Bibcode: 1995LAstr.109..340K Altcode: Solar eclipse 1995 October 24 in Indochina. Title: Chromospheric Oscillations from Simultaneous Sequences of HEL 1083 and Call K 393.4 Spectroscopic Measurements Authors: Bocchialini, K.; Koutchmy, S. Bibcode: 1995ESASP.376b.499B Altcode: 1995help.confP.499B; 1995soho....2..499B No abstract at ADS Title: The Space-Time Structure of the Upper Solar Atmosphere Authors: Koutchmy, S.; Veselovsky, I. S. Bibcode: 1995ESASP.376b.475K Altcode: 1995soho....2..475K; 1995help.confP.475K No abstract at ADS Title: Nonlinear MHD interactions in some solar coronal structures Authors: Grib, S. A.; Koutchmy, S.; Sazonova, V. N. Bibcode: 1995sowi.conf...60G Altcode: The magnetohydrodynamic (MHD) interactions of solar coronal fast shock waves of flare and/or nonflare origin with the boundaries of such structures like the streamer and the coronal hole are considered. These boundaries are treated as MHD tangential discontinuities (TD). Different parameters of the observed corona are used. The general case of oblique interaction is studied. It is shown that a fast shock wave is usually refracted as a fast shock wave inside the coronal streamer. But for a special case of the velocity shear across a TD a slow shock wave may be generated. On the contrary the shock wave is refracted inside the coronal hole, indeed as a slow shock wave. The significance of different effects due to the interaction of fast and slow shock waves with the coronal magnetic field is noticed, especially at the time of coronal mass ejection (CME). Thus slow shock waves may help to 'open' the coronal magnetic field, and fast shock waves - to 'close' it. It is also shown, that an oblique fast MHD coronal shock wave may trigger an instability at the boundary of a streamer considered as a TD. It might have a relation with the observed abrupt process of disappearance of the streamer's boundary in the solar corona. Title: L'éclipse totale de Soleil du 3 novembre 1994 sur les Andes chiliennes. Authors: Koutchmy, S.; Zimmermann, J. -P. Bibcode: 1995LAstr.109..110K Altcode: No abstract at ADS Title: Special Session - Waves on the Extended Transition-region and Loops Authors: Koutchmy, S. Bibcode: 1995ESASP.376a.233K Altcode: 1995heli.conf..233K No abstract at ADS Title: Equilibrium and stability of axially symmetrical plasma configurations in the Sun's atmosphere. Authors: Koutchmy, S. L.; Koutchmy, O. K.; Kutvitskij, V. A.; Molodenskij, M. M.; Solovev, L. S. Bibcode: 1995BRASP..59.1570K Altcode: On the basis of a unified approach the authors consider the conditions of the MHD equilibrium and stability of a number of axially symmetrical plasma configurations responsible for typical formations in the Sun's atmosphere, such as coronal helmets and loops, and also a new object, i.e., the coronal plasmoid observed 11 July 1991 during the solar eclipse. Title: Near-Infrared Coronagraphic Detection of Space Debris Authors: Neidig, D. F.; Smartt, R. N.; Kim, I. S.; Koutchmy, S. Bibcode: 1995itsa.conf..253N Altcode: No abstract at ADS Title: White-Light Coronal Fine Structure Authors: November, L. J.; Koutchmy, S. Bibcode: 1995itsa.conf...37N Altcode: No abstract at ADS Title: Advanced Coronagraphy Authors: Koutchmy, S. Bibcode: 1995itsa.conf....1K Altcode: No abstract at ADS Title: Mirror Coronagraphic Device and Its Application Authors: Kim, I. S.; Bougaenko, O. I.; Brouevitch, V. V.; Koutchmy, S.; Neidig, D. F.; Smartt, R. N.; Evseev, O. A. Bibcode: 1995itsa.conf..239K Altcode: No abstract at ADS Title: On the 3-D Structure of the November 3, 1994 Eclipse Corona Authors: Koutchmy, S.; Molodensky, M.; Starkova, L.; Ershov, A.; Matsuura, O. Bibcode: 1995pist.conf...60K Altcode: No abstract at ADS Title: Reflecting Coronagraphs: Prospects Authors: Smartt, R. N.; Koutchmy, S. Bibcode: 1995itsa.conf..163S Altcode: No abstract at ADS Title: Detection of a Dual "Disparition Brusque" at Pic-Du-Midi Authors: Niot, J. M.; Noëns, J. C.; Romeuf, D.; Koutchmy, S. Bibcode: 1995itsa.conf..247N Altcode: No abstract at ADS Title: Wave Properties of the Chromosphere in He I 1083 nm and CA II K Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S. Bibcode: 1995itsa.conf..423B Altcode: No abstract at ADS Title: Pic du Midi observations of dual `disparition brusque' Authors: Koutchmy, S.; Noëns, J. C. Bibcode: 1994ESASP.373...91K Altcode: 1994soho....3...91K No abstract at ADS Title: About small plasmoids propagating in the solar corona Authors: Koutchmy, S.; Bouchard, O.; Grib, S.; November, L.; Vial, J. -C.; Gouttebrone, P.; Koutvitsky, V.; Molodensky, M.; Solov'iev, L.; Veselovsky, I. Bibcode: 1994ESASP.373..139K Altcode: 1994soho....3..139K No abstract at ADS Title: White-Light Coronal Fine Structure Authors: November, L. J.; Koutchmy, S. Bibcode: 1994AAS...185.9204N Altcode: 1994BAAS...26.1472N No abstract at ADS Title: Fast coronal transient (CME) with twisted legs Authors: Airapetian, V. S.; Koutchmy, S. Bibcode: 1994ESASP.373..195A Altcode: 1994soho....3..195A No abstract at ADS Title: On the three-dimensional structure of coronal rays Authors: Koutchmy, S.; Molodenskii, M. M.; Vial, J. -C. Bibcode: 1994ARep...38..822K Altcode: No abstract at ADS Title: Magnetic configuration of coronal streamers and threads Authors: Koutchmy, S.; Koutvitsky, V. A.; Molodensky, M. M.; Solov'iev, L. S.; Koutchmy, O. Bibcode: 1994SSRv...70..283K Altcode: We give a short account of the most prominent structures of the intermediate corona. Then we propose an axially symmetrical model for coronal streamers, according to which charged particles move along magnetic surfaces whose sources are electrical currents situated in the vicinity of the photosphere. The simplest current configuration is a pair of coaxial, coplanar, circular, and oppositely directed currents parallel to the photosphere. Magnetic surfaces for this current distribution exhibit a helmet-shaped separatrix and a saddle point. The temperature profile along the streamer can be predicted qualitatively if one takes into account the conservation of an adiabatic invariant in the drift theory of the charged particle motion. Title: The Chromospheric network dynamics as derived from the analysis of CA II K and He I 1083 NM lines Authors: Bocchialini, S.; Vial, J. -C.; Koutchmy, S. Bibcode: 1994SSRv...70...57B Altcode: We present results of line profile analysis of observations simultaneously performed around the Ca II K and He I (1083 nm) lines, using the Horizontal Spectrograph of the Vacuum Tower Telescope of NSO/SP. From the spectral analysis of a 83 min long sequence of CCD spectra, we derive some dynamical properties of the main components of the quiet chromosphere: i) the magnetic network, ii) the cell interior. We present a whole set of amplitude spectra near 5 and 3 min periods for the two lines; K3 and He I velocity spectra extending up to 100 mHz are also considered, for the first time. Title: On the Visible Shape of the Cold Plasma Jets in the Solar Chromosphere Authors: Veselovsky, I. S.; Triskova, L.; Koutchmy, S. Bibcode: 1994SoPh..153..237V Altcode: Lines of equal optical thickness are calculated for cold plasma jets propagating in the simplest magnetic configuration. The paraxial approximation is used in the case of jets directed along the axis of a magnetic dipole. The results explain the apparently convergent as well as divergent shapes of the jets in a divergent magnetic configuration. Title: Moon-based UV reflecting coronagraph Authors: Vial, J. C.; Koutchmy, S.; Smartt, R. N. Bibcode: 1994AdSpR..14f..43V Altcode: 1994AdSpR..14...43V UV observations of the solar disc, and above the limb, have evidenced a wide range of possible diagnostics, especially in the Lα line. On the disc, Lα traces the magnetic (sometimes unexpected) structuring of the top of the atmosphere; out from the limb, it allows measurement of radial velocities up to a few solar radii where most optical techniques fail. Other diagnostics include the kinematics of ejections (e.g. CMEs, but also small-scale rapidly evolving plasmoïds). We propose a dual-channel reflecting coronagraph combining relatively-high angular resolution (0.2-0.4'') with large spatial (2.5 solar radii from Sun center) and temporal coverage. The advantages offered by a Moon-based instrument are discussed. Title: Magnetic configurations of ray structures of the solar corona Authors: Koutchmy, S.; Kutvitskii, V. A.; Molodenskii, M. M.; Solov'ev, L. S. Bibcode: 1994ARep...38..417K Altcode: No abstract at ADS Title: Coronal physics from eclipse observations Authors: Koutchmy, S. Bibcode: 1994AdSpR..14d..29K Altcode: 1994AdSpR..14...29K Solar total eclipses are rare occasions offering the opportunity to make a snapshot of the solar corona. Thanks to the availability of a large radiative flux in the optical region, sophisticated methods can be used from the ground to analyse all parts of the highly structured white-light corona. Coronal absolute intensities and line emissions, including their polarization, are also studied to analyse density and temperature inhomogeneities, velocities and magnetic fields. Detailed density distribution is directly extracted from fine coronal structures. During the July 11, 1991 eclipse, the large 3.6m aperture CFH optical telescope was used to analyse time sequences over small coronal fields and to image the finest structures; results from this experiment are presented with emphasis on small-scale dynamical plasma processes with possible inclusion of wave-phenomena. Finally, to prepare the SOHO mission on coronal physics, we give an overview of what is known on coronal structures from eclipse observations of the past solar cycles: temperatures, densities, velocities, occurence and structure of streamers, coronal holes, threads, overall variability.

associated with the Pierre et Marie Curie University of Paris VI, France Title: Dynamical Properties of the Chromosphere In and Out of the Solar Magnetic Network Authors: Bocchialini, Karine; Vial, Jean-Claude; Koutchmy, Serge Bibcode: 1994ApJ...423L..67B Altcode: We present the results of a comparative analysis of an 83 minute time sequence of spectra taken around the Ca II and He I 1083 lines, near the center of the solar disk and away from active regions. We discuss the behavior of the Fourier spectra at low frequency: 3 minute oscillations are well observed out of the network, and 5 minute oscillation waves are prominent in the network. The 5 s sampling time also permits the observation of the high-frequency part of the Fourier spectra of intensity and velocity fluctuations at different heights. At high frequencies, K2V-K2R and 1083 (velocity) results differ when magnetic and non-magnetic regions are compared. Title: Very High Resolution Analysis of the Dynamics of a Coronal Plasmoid Authors: Bouchard, O.; Koutchmy, S.; November, L.; Vial, J. -C.; Zirker, J. B. Bibcode: 1994scs..conf..593B Altcode: 1994IAUCo.144..593B The authors present the results of the analysis of a movie taken over a small field of view in the intermediate corona at a spatial resolution of 0.5", a temporal resolution of 1 s and a spectral passband of 7 nm. These CCD observations were made at the prime focus of the 3.6 m aperture CFHT telescope during the 1991 total solar eclipse. Title: Near-IR Solar Coronal Observations with New-Technology Reflecting Coronagraplis Authors: Smartt, R. N.; Koutchmy, S.; Noens, J. -C. Bibcode: 1994IAUS..154..603S Altcode: No abstract at ADS Title: On the Optical Polarization of the White-Light Coronal Structures Authors: Filippov, B. P.; Molodensky, M. M.; Koutchmy, S. Bibcode: 1994scs..conf..601F Altcode: 1994IAUCo.144..601F A special experiment was designed to measure the orientation of the polarization plane in the solar corona during the total eclipse of July 11, 1991. Rotating polaroids with the axes directed at +45° and at -45° of the radial direction in all directions were used. The polarization plane was found to be tangential to the solar limb everywhere with an accuracy within 1°. Title: The IR Contrast of Magnetic Elements Obtained from High Spatial Resolution Observations at 1.6 MU M Authors: Darvann, T. A.; Koutchmy, S. Bibcode: 1994IAUS..154..483D Altcode: No abstract at ADS Title: On Sunspot and Facular Contrast Variations Near 2 MU M and 4 MU M Authors: Kotov, V. A.; Koutchmy, S. Bibcode: 1994IAUS..154..265K Altcode: No abstract at ADS Title: A Method to Obtain Stereo-Diagrams of the Solar Disc Authors: Molodensky, M. M.; Starkova, L.; Koutchmy, S. Bibcode: 1994scs..conf..605M Altcode: 1994IAUCo.144..605M In order to obtain a 3D picture of the Solar disc planoconvex spherical and elliptical lenses were made by the authors using organic glass. The comparison between the effects produced by the lenses and the results of the calculation have shown that the elliptical lenses give the best results. Title: Wave Properties in the Upper Chromosphere and at the Base of the Corona Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S. Bibcode: 1994scs..conf..123B Altcode: 1994IAUCo.144..123B From a 83 min long sequence of observations of Ca II K and He I (1083 nm) line profiles, some dynamical properties of the main components of the quiet upper chromosphere are derived: for both the magnetic network and the internetwork, amplitude and phase spectra of the Doppler velocities are presented. Title: Analysis of Chromospheric Proxies of Coronal Bright Points Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S.; Zirker, J. B. Bibcode: 1994ASPC...68..389B Altcode: 1994sare.conf..389B No abstract at ADS Title: On the 3D Solar Corona Structure Authors: Koutchmy, S.; Molodensky, M. M.; Vial, J. -C. Bibcode: 1994scs..conf..585K Altcode: 1994IAUCo.144..585K The authors consider the 3D structure of the solar corona using eclipse observations. They use a pseudostereoscopic effect of the rigidly rotating corona to determine the true position of the main coronal structures: broad threads, rays and streamers. An example of stereo-view deduced from a simple analysis of results coming from the 1991 eclipse is given. The authors conclude that large helmet streamers are composed by the pleats of the heliosphere current sheet projected on the plane of the sky. Title: The Infrared Granulation - Observations Authors: Koutchmy, S. Bibcode: 1994IAUS..154..239K Altcode: No abstract at ADS Title: CFHT eclipse observation of the very fine-scale solar corona Authors: Koutchmy, S.; Belmahdi, M.; Coulter, R. L.; Demoulin, P.; Gaizauskas, V.; MacQueen, R. M.; Monnet, G.; Mouette, J.; Noens, J. C.; November, L. J. Bibcode: 1994A&A...281..249K Altcode: At the July 11, 1991 solar total eclipse, a modern large optical telescope, Canada-France-Hawaii telescope (CFHT), was used to probe the solar corona. The best possible pictures were obtained with the CFHT, using fast imaging techniques and post-facto image selection and processing. Several cameras were run during totality to acquire sub-arcsec spatial resolution white-light images, with both narrow-band and broad-band filters. The setup and the observing procedure are described. Preliminary results, together with an evaluation of the merits of the experiment, are given, as well as a sample of images. Fine-scale coronal features were observed for the first time in a time series, confirming the importance of plasmoid-like activity in the inner corona. The observation of the smallest coronal feature ever reported is analyzed, giving a typical cross-section of 0.4 +/- 0.1 arcsec. On a larger scale, dark loops around a foreground prominence are resolved for the first time, suggesting that sheet-like voids exist above a filament channel. Title: IR Observations of the K and F Corona During the 1991 Eclipse Authors: Kuhn, J. R.; Lin, H.; Lamy, P.; Koutchmy, S.; Smartt, R. N. Bibcode: 1994IAUS..154..185K Altcode: No abstract at ADS Title: Magnetic structures of the intermediate corona Authors: Koutchmy, S.; Molodensky, M. Bibcode: 1994LNP...432..167K Altcode: 1994LNPM...11..167K The fine structures of the corona are analyzed using SXR and W-L eclipse pictures. The measurement of the finest features observed at the CFHT on July 11, 1991 is discussed. We call the attention to the 3-D aspect of the magnetic structure which can be apprehended and analysed assuming the plasma is concentrated in thin curved sheets observed on eclipse W-L pictures. More geometrical parameters can be deduced from the stereo-view based on the hypothesis of a rigid rotation. A preliminary 2.5-D model calculation is put forward to explain the active region coronal rays. It is based on the assumption of ad hoc chromospheric current distribution and analytic calculations. Title: Magnetic Structures of the Intermediate Corona Authors: Koutchmy, S.; Molodensky, M. M.; Koutvitsky, V.; Solov'ev, L. S. Bibcode: 1994scs..conf...55K Altcode: 1994IAUCo.144...55K The fine structures of the corona are analyzed using SXR and WL eclipse pictures. The measurement of the finest features observed at the CFHT on July 11, 1991 is discussed. A preliminary 2.5D model calculation is put forward to explain the active region coronal rays. Title: on the Three-Dimensional Structure of Coronal Rays Authors: Koutchmy, S.; Molodenskii, M. M.; Vial, J. C. Bibcode: 1994AZh....71..925K Altcode: No abstract at ADS Title: The Magnetic Field of a Bipolar Sunspot Region in the Photosphere and the Chromosphere Authors: Dara, H. C.; Koutchmy, S.; Alissandrakis, C. E. Bibcode: 1994emsp.conf...61D Altcode: No abstract at ADS Title: Analysis of the Chromospheric Proxies of Coronal Bright Points - Preliminary Results Authors: Bocchialini, K.; Koutchmy, S.; Vial, J. -C.; Zirker, J. B. Bibcode: 1994emsp.conf..173B Altcode: No abstract at ADS Title: Chromospheric Faculae as Filaments Feet? Authors: Koutchmy, S.; Stellmacher, G. Bibcode: 1994emsp.conf...91K Altcode: No abstract at ADS Title: Solar eclipses. Authors: Koutchmy, S. Bibcode: 1994oga..book...81K Altcode: Contents: 1. Introduction. 2.Circumstances of eclipses. 3. Observation of the event. 4. Inner Coronal photography and photometry. 5. Photographing the K, or plasma, corona. 6. Photography of the outer corona. 7. Spectroscopic study of the corona. 8. Conclusions. Title: Toward High-Spatial Resolution IR Solar Observations Authors: Koutchmy, S.; Restaino, S. Bibcode: 1993rtpf.conf..171K Altcode: No abstract at ADS Title: The Finest White-Light Coronal Features Authors: Koutchmy, S.; Bouchard, O.; Mouette, J.; Koutchmy, O. Bibcode: 1993rtpf.conf..147K Altcode: No abstract at ADS Title: The Finest White-Light Coronal Features Authors: Koutchmy, Serge; Bouchard, Olivier; Mouette, Jean; Koutchmy, Olga Bibcode: 1993SoPh..148..169K Altcode: An attempt to detect the finest white-light coronal features observed with a large optical telescope was made at the July 11, 1991 Solar Total Eclipse. A few selected results taken from the video-CCD high speed observations obtained at the prime focus of the Canada-France-Hawaï-Telescope (CFHT) with a red coronal interference filter are presented. The smallest (sub-arsec) detected and/or resolved coronal features are shown. The methods that were used to extract them from the noisy and seeing-limited images taken from video frames are described. Title: Photospheric and chromospheric magnetic field structure of a bipolar sunspot region Authors: Dara, H. C.; Koutchmy, S.; Alissandrakis, C. E. Bibcode: 1993A&A...277..648D Altcode: We present high resolution magnetograms of a large split spot and an opposite polarity pore in the 6102.7 Å Ca I photospheric line and in Hα and we discuss their fine structure. We found important differences between the photospheric and chromospheric magnetic field. Although the large spot was apparently unipolar at the photospheric level, we detected an opposite polarity region at the chromospheric level. We also found that there was hardly any trace of the pore magnetic field in the Hα magnetogram. These results cannot be interpreted in terms of constant-α magnetic fields. Finally we confirm the occurrence of filamentary magnetic structures in Hα at the location of the superpenumbra of the large spot. Title: Measuring the polarization of the solar corona Authors: Koutchmy, S.; Molodenskii, M. M.; Nikol'Skii, G. M.; Filippov, B. P. Bibcode: 1993ARep...37..286K Altcode: 1993SvA....37..286K No abstract at ADS Title: Photospheric electric currents in solar magnetic elements Authors: Lorrain, P.; Koutchmy, S. Bibcode: 1993A&A...269..518L Altcode: In order to explain recent high-resolution magnetogram and filtergram observations, we propose a self-excited dynamo model for the magnetic elements, or network patches, that occur in the high photosphere of the sun at the periphery of supergranules. We assume that an element is a magnetic flux tube that stands more or less vertically and that results from the presence of azimuthal electric currents, and we describe a mechanism that could generate these currents. As a first approximation, we assume that the electric current density is uniform. This model accounts for the existence of magnetic elements, for their stability, for the existence of neighboring fields of opposite polarity, and for their mutual attraction and repulsion. The power dissipation associated with the azimuthal currents accounts for only a small part of the observed radiation in the low photosphere, so that other explanations for the brilliance will have to be considered. We also propose a more realistic but more elaborate model in which the azimuthal electric current distribution is not uniform. Title: Toward High Spatial Resolution Infrared Solar Observations Authors: Koutchmy, Serge; Restaino, Sergio R. Bibcode: 1992SoPh..142..359K Altcode: To achieve high spatial resolution capability for IR solar observations, we suggest the use of a special mask placed before the entrance aperture of large conventional optical telescopes. Such a mask would match well the resolution of a non-redundant array and would provide safe operation of a large telescope used for solar observations. The proposed solution has the additional advantage of relatively low cost because already-existing optical telescopes are used. Title: Three-dimensional image of the solar corona from white-light observations of the 1991 eclipse Authors: Koutchmy, Serge; Molodenskii, Mikhail M. Bibcode: 1992Natur.360..717K Altcode: THE structure of the solar corona is believed to be governed by the solar magnetic field induced by currents at the surface of the Sun and perhaps within the corona itself1. Inhomogeneities in the corona are well known from radially compensated eclipse images2 in white light or coronal emission lines3. We have used two whitelight images taken about three hours apart by the Multi-station International Coronal Experiment4 during the July 1991 total eclipse in an attempt to deduce directly the three-dimensional structure of the corona. We observed prominent coronal structures, including broad threads, rays and streamers, and used them to calibrate a model based on solid-body rotation and bulk coronal outflow. The errors in the reconstruction method are small enough to give us confidence that quasi-rigid rotation is a reasonable approximation over these timescales. We illustrate the deduced coronal structure by means of a stereogram. Title: Coronal photometry and analysis of the eclipse corona of July 22, 1990 Authors: Koutchmy, S.; Altrock, R. C.; Darvann, T. A.; Dzubenko, N. I.; Henry, T. W.; Kim, I.; Koutchmy, O.; Martinez, P.; Nitschelm, C.; Rubo, G. A. Bibcode: 1992A&AS...96..169K Altcode: Results are presented of aircraft-based observations and ground observations from multiple stations, made during the July 1990 eclipse. The main results of the analysis of the large-scale features of the inner corona concern the measurement of the flattening index of the near-maximum-activity corona; the occurrence of a large coronal hole; and the importance of the line emissions recorded on the broadband white-light pictures, due to the presence of numerous large or faint prominences all around the limb. Title: Photoelectric analysis of the solar granulation in IR Authors: Koutchmy, Serge Bibcode: 1992STIN...9318334K Altcode: Results of both image analysis and statistical analysis of 1D scans the IR granulation observed in the opacity minimum region are briefly presented. The same technique was applied at 600 nm and results partially presented by Koutchmy and Lebecq, 1986, Astron. Astrophys. 169, 323. All observations were collected at the prime focus of the Sac Peak VTT using high signal-to-noise ratio measurements with a specially-designed pinhole PbS spectro-photometer; imaging has been made using both 2D scanning of the telescope and processed video-scans of an IR-vidicon. Images of the IR granulation and of sunspot umbral dots and penumbral filaments are present for the first time. Title: Streamer eclipse observations. Authors: Koutchmy, Serge Bibcode: 1992ESASP.348...73K Altcode: 1992cscl.work...73K During the 1991 eclipse, the large 3.6 m aperture CFH optical telescope was used to analyse time sequences over small coronal fields and to reach the finest structure; results from this experiment are presented including the analysis of the faintest detected feature and small-scale dynamical plasma processes. To prepare the SOHO mission on coronal physics, an overview of what is known on coronal structures from eclipse observations of the past solar cycles is given. The non-potential nature of the coronal magnetic field is well illustrated by the large deviation of streamers from the radial direction as well as by the systematic occurence of tangential discontinuities at edges of streamers. Title: No Evidence of a Circumsolar Dust Ring from Infrared Observations of the 1991 Solar Eclipse Authors: Lamy, P.; Kuhn, J. R.; Lin, H.; Koutchmy, S.; Smartt, R. N. Bibcode: 1992Sci...257.1377L Altcode: During the past 25 years there have been many attempts to detect a possible dust ring around the sun, with contradictory results. Before the 1991 eclipse, infrared eclipse experiments used single-element detectors to scan the corona along the ecliptic for excess surface brightness peaks. The availability of relatively large-format infrared array detectors now provides a considerable observational advantage: two-dimensional mapping of the brightness and polarization of the corona with high photometric precision. The 1991 eclipse path included the high-altitude Mauna Kea Observatory, a further advantage to measure the corona out to large angular distances from the sun. Results are reported from an experiment conducted on Mauna Kea with a HgCdTe-array detector sensitive to wavelengths between 1 and 2.5 micrometers, using broad-band J, H, and K filters. Although the sky conditions were not ideal, the H- and K-band surface brightnesses clearly show the inhomogeneous structure in the K-corona and the elliptical flattening of the F-corona, but no evidence of a circumsolar, local dust component out to 15 solar radii. Title: Coronal Streamers Authors: Koutchmy, Serge; Livshits, Moissei Bibcode: 1992SSRv...61..393K Altcode: The general significance of streamers of the solar corona is discussed in the frame of our knowledge of the solar wind phenomenon and the large-scale solar magnetic structure. Thermodynamical and geometric parameters of streamers observed and measured at total solar eclipses are reviewed. Both the low part (in the form of a helmet with a cusp) and the external part (in the form of a stalk extended at many solar radii) are considered. The modelling of streamers starts with the analysis of effects produced by the solar wind flow on a magnetic structure. Facts and arguments are presented in favor of a model with a current sheet and reconnection processes going on along the axis of the streamer, especially in the non-collisional part of the radially extended streamer. Further development of the Pneuman and Kopp (1971) model is discussed, including difficulties occurring in the interpretation of a stationary solution. An empirical model satisfying observations is presented. Future researchs on streamers were discussed with emphasis on observations to be done with the space-borne coronagraphs on the SOHO spacecraft. Title: Structural changes in the solar corona during the July 1991 eclipse Authors: Zirker, J. B.; Koutchmy, S.; Nitschelm, C.; Stellmacher, G.; Zimmermann, J. P.; Martinez, P.; Kim, I.; Dzyubenko, N.; Kurochka, L.; Makarov, V. Bibcode: 1992A&A...258L...1Z Altcode: Preliminary results of the analysis of radially filtered pictures obtained at several hours interval during the July 11, 1991 total solar eclipse are given. Instrumental parameters and method are outlined. Structural changes are discussed. Title: Evidence of plasmoid ejection in the corona from 1991 eclipse observations with the Canada-France-Hawaii telescope Authors: Vial, J. -C.; Koutchmy, S.; Monnet, G.; Sovka, J.; Clark, C.; Salmon, D.; Purves, N.; Sydserff, P.; Coulder, R.; November, L. Bibcode: 1992ESASP.344...87V Altcode: 1992spai.rept...87V Observations of the solar corona with a large telescope at high altitude was fully exploited with the 3.60 m CFHT (Canada France Hawaii Telescope) in Hawaii, during the 11 Jul. 1991 eclipse, are reported. Different instruments set up for the eclipse and preliminary results are given. The moving feature in the corona is focused upon. Physical conditions in this plasmoid and its origins are discussed. One of the four cameras installed in the primary focus was a video charge coupled device camera with a red filter at 637 nm selecting the red line. The power of the telescope allowed for a good signal in a pixel as small as 0.12 arcsec and a very good time resolution. The spectral resolution as measured at the Moon limb was better than one arcsec. During the three minute long sequence, 6000 video images were obtained. Among the fine structures recorded, a plasmoid about 1500 km wide was seen to ascend and dilute in the corona. Possible emission mechanisms are discussed. It was found that both low and relatively high temperature plasmas can be confined in this ejected plasmoid. Such a small scale phenomenon could be important for the heating of the corona and should be observed in UV emission lines in a wide range of temperatures. The high spatial resolution achieved by Solar Interferometric Mission for Ultrahigh Resolution Imaging and Spectroscopy (SIMURIS) allows to study the shape, stability and the diagnostics of such plasmoids in the corona. Title: Development of Reflecting Coronagraphs Authors: Smartt, R. N.; Koutchmy, S. Bibcode: 1992ASPC...26..660S Altcode: 1992csss....7..660S No abstract at ADS Title: The solar corona of July 11, 1991. Observations in Brazil (MICE). Authors: Dzyubenko, N. I.; Kurochka, L. N.; Rubo, G. A.; Kim, I. S.; Artamonov, B. P.; Boczko, R.; Matsuura, O. T.; Koutchmy, S.; Zimmermann, J. P.; Zirker, J. B. Bibcode: 1992ATsir1552...21D Altcode: No abstract at ADS Title: Eclipse Totale de Soleil du 11 Juillet 1991 Authors: Koutchmy, S. Bibcode: 1992BCFHT..26....2K Altcode: No abstract at ADS Title: Observations of the solar corona on July 22, 1990. The structure and the identification. Authors: Dzyubenko, N. I.; Ivanchuk, V. I.; Rubo, G. A.; Koutchmy, S. Bibcode: 1991BSolD..11...98D Altcode: No abstract at ADS Title: Observations of total solar eclipses in the stratosphere. Authors: Koutchmy, S. Bibcode: 1991ZemVs...5...33K Altcode: No abstract at ADS Title: Multicolor Continuum Analysis of the Solar Granulation in Quiet and Active Regions Authors: Keller, C. U.; Koutchmy, S. Bibcode: 1991ApJ...379..751K Altcode: A set of narrow-band filtergrams of the solar photosphere recorded in three widely separated true continuum windows and in Mg I b1 with a spatial resolution of about 0.5 arcsec is analyzed. The influence of small-scale magnetic fields on the granulation is studied by comparing various statistical parameters in selected active and quiet regions, and the temperature stratification of faculae at the level of continuum formation is investigated. In active regions there exist more points with enhanced continuum intensity as compared with quiet regions, and there is more power at small spatial scales in active regions, whereas more power exists at large scales in quiet regions. Quiet regions near and far away from a large sunspot do not show any significant difference. It is concluded that changes in the granular pattern near sunspots are caused by the small-scale magnetic fields often found near sunspots. Faculae, identified by their brightness in the Mg I b1 wing, show an enhanced continuum intensity and a reduced ratio between the blue and the red continuum, which is consistent with current flux tube models. Title: Study of small scale magnetic flux and the corresponding velocity pattern Authors: Alissandrakis, C. E.; Dara, H. C.; Koutchmy, S. Bibcode: 1991A&A...249..533A Altcode: Two-dimensional maps of the longitudinal magnetic field and the line of sight velocity of two small-scale magnetic regions in the quiet sun, using a one-hour time sequence of filtergrams in the magnetically sensitive lambda 6103 A CaI line (with circular polarization measurements) obtained with the Sacramento Peak Vacuum Tower Telescope and the universal filter, are calculated. After the elimination of the effect of the 5-minute photospheric oscillations, downflows smaller than 300 m/s are found in both magnetic regions. The magnetic field intensity and the velocity are weakly correlated: high values of the magnetic field tend to occur in regions of small negative velocities. The magnetic field intensity increased during the observations, while some magnetic peaks moved with respect to others. The difference of the magnetic field intensity measured in the blue and the red wing indicates a line asymmetry; this asymmetry was found to be independent of the line of sight velocity. Title: Eclipse Plans for NSO/SP Authors: Zirker, J. B.; Koutchmy, S.; Coulter, R. L.; November, L. J.; Smartt, R. N. Bibcode: 1991BAAS...23.1063Z Altcode: No abstract at ADS Title: Small scale magnetic field mapping with high temporal resolution. Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1991sopo.work..257D Altcode: Two dimensional maps of the longitudinal magnetic field can be readily calculated for small-scale magnetic regions. Here the authors use an one-hour time sequence of high spatial resolution (0.75 arc sec) filtergrams, obtained at the Sacramento Peak Vacuum Tower Telescope with the universal filter (UBF) in the wings of the magnetically sensitive λ 6103 Ca I line. The time difference between two magnetic maps is 32 sec. The measurements of the magnetic field in the blue wing are about 40% higher than in the red wing. Title: High spatial resolution V-Stokes polarimetry to measure the Zeeman effect in flux tubes and prominence filament threads. Authors: Koutchmy, S.; Zirker, J. B.; Darvann, T.; Koutchmy, O.; Stauffer, F.; Mann, R.; Coulter, R.; Hegwer, S. Bibcode: 1991sopo.work..263K Altcode: No abstract at ADS Title: Coronal activity. Authors: Koutchmy, Serge; Zirker, Jack B.; Steinolfson, Richard S.; Zhugzhda, Iosif D. Bibcode: 1991sia..book.1044K Altcode: This chapter considers the rather extended, very inhomogeneous and dynamical part of the solar atmosphere called the corona. Coronal structures are first described from the point of view of quasi-static structure in order to consider their thermodynamical gross properties, including heating and magnetic fields. The solar-cycle-related variations of coronal structures are reviewed as well. Solar prominences are a well-observed ingredient of the corona; they form its cool component. Their properties, including magnetic field, thermal and velocity field structures are reviewed before considering the problem of their formation. Coronal mass ejections are the most dramatic phenomena occurring in a short time in the corona and are almost inevitably phenomena occurring in a short time in the corona and are almost inevitably related to a prominence ejection. Their observations are described with reference to several related solar phenomena in order to understand the driving mechanism. Models of coronal mass ejections are described based on numerical simulations including consideration of waves. Finally, the very important and still open question of the waves in the solar corona is briefly discussed from a theoretical point of view, emphasizing the possible role of hydromagnetic waves. Title: Properties of Impulsive Events in a Polar Coronal Hole (With 6 Figures) Authors: Koutchmy, S.; Loucif, M. L. Bibcode: 1991mcch.conf..152K Altcode: No abstract at ADS Title: Future Observations of the F-Corona with the LASCO Coronagraph Space Experiment Authors: Lamy, P. L.; Llebaria, A.; Maucherat, A.; Koutchmy, S.; Giovane, F. Bibcode: 1991ASSL..173..191L Altcode: 1991IAUCo.126..191L; 1991oeid.conf..191L No abstract at ADS Title: High spatial resolution observations of magnetic flux elements. Authors: Koutchmy, S. Bibcode: 1991sopo.work..237K Altcode: The author shortly reviews works done at the VTT of SPO during the last 15 years, on both high spatial resolution spectroscopy using polarization analysis and magnetography with a polarization modulator inside the UBF. Respective merits and noticeable results are discussed. The author stresses the importance of using high-speed measurements to track the magnetic signal and avoid losses due to image motion; the efficiency in improving the resolution using the 2-D Wiener filtering is also demonstrated. Subarcsec resolution magnetic maps are discussed, to show not only the dominant-polarity magnetic-elements, but also the mixed minor-polarity and the weak field outside. Title: Prominence Fine Structure - Part Two - Diagnostics Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1991SoPh..131..107Z Altcode: A random-clustering model of prominence fine-structure has been applied to observations of prominence Hα spectra. The model yields an estimate of the number of unresolved elements that form an individual resolved feature, and sets limits on their velocity and Hα profile dispersions. Title: L'Observatoire Solaire de Sacramento Peak Authors: Koutchmy, S. Bibcode: 1990LAstr.104..395K Altcode: No abstract at ADS Title: Observation de la couronne dans la stratosphére. Authors: Koutchmy, Serge Bibcode: 1990LAstr.104..385K Altcode: Reasons for conducting solar-eclipse observations from the stratosphere are discussed. Stratospheric observations of the total solar eclipse of July 22, 1990 from a specially equipped Falcon 20 are described. A visualization of the corona of the 1990 eclipse is presented. Title: UV solar reflecting coronagraph Authors: Smartt, R. N.; Koutchmy, S.; Vial, J. C. Bibcode: 1990AIPC..207..578S Altcode: 1990am...proc..578S A dual-channel reflecting coronagraph is proposed that would provide observations of Lα corona and chromosphere, upper transition-region phenomena in CIV, and also helioseismology observations in the continuum around 166 nm. Each channel would use a 104×104-UV-sensitive CCD array. The combined velocity and magnetic field data would link events in the chromosphere, the transition region and the corona to an elongation of about 2.5 R0. These data would be used to study both the global-scale and also the fine-scale properties of the corona in terms of the physical processes that deposit energy and momentum in the corona. Specific question to be investigated would be the origin and morphology of CME's and other coronal transients, sources of coronal heating, and the source(s) and dynamics of the coronal wind in the inner coronal region. Title: Erratum: Velocity Pattern of Small Scale Magnetic Fields Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1990SoPh..128..431D Altcode: No abstract at ADS Title: Real-time image processing and data handling for ground-based and spaceborne coronal observations Authors: Koutchmy, S.; Colley, S.; Smartt, R.; Nitschelm, C.; Zimmermann, J. P. Bibcode: 1990SPIE.1235..849K Altcode: Ground-based observations of the solar corona, as well as deep night-time observations close to bright objects, are degraded by highly variable aureole effects produced by the earth's atmosphere, even when the stationary background pattern of both atmospheric and instrumental origin is removed using detectors and special processing techniques. First observations using an objective mirror advanced coronagraph reveal that small particles (both continental and maritime aerosols) imaged on the focal plane as they cross the field of view can dominate the background unter clear-sky conditions, producting a considerable noise background that it is not easily removed. Suggestions are made to reduce to noise of this "dynamical aureole". The authors also discuss the possibility of optically detecting orbital space debris of small size, using either an externally-occulted space-borne mirror coronagraph or a large-aperture ground-based mirror coronagraph, and the corresponding detection system requirements. Title: New technology mirror coronagraph with extended applications Authors: Smartt, Raymond N.; Koutchmy, Serge L.; Colley, Stephen A.; Caron, R.; Schwenn, Rainer; Restaino, Sergio R. Bibcode: 1990SPIE.1236..206S Altcode: General design considerations of objective-mirror coronagraphs are presented. A 1-m-focal-length prototype reflecting coronagraph based on a 5.5-cm aperture spherical superpolished silicon mirror objective is described. The design is simple off-axis reflection from the objective to a conventional coronagraph optical system (occulting disk, field lens, Lyot stop, and imaging system). This instrument has produced the first images of the emission corona using a ground-based reflecting coronagraph. A second prototype instrument based on a 15-cm aperture superpolished fused-silica mirror is also described. Title: The magnetic-field polarity of quiescent prominences Authors: Kim, I. S.; Klepikov, V. Y.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1990PAZh...16..545K Altcode: A statistical analysis of magnetographic data on quiescent solar prominences is presented. The existence of two different magnetic field systems in quiescent prominences is suggested. The first system is oriented opposite to the underlying photospheric field; the angle between the long axis of the filament and the field direction is equal to 15 deg and B-parallel equals 15-18 G. The polarities of the second system and of the underlying photospheric field are the same, B-parallel = 5-7 G. Title: Magnetic Field Polarity of Quiescent Prominences Authors: Kim, I. S.; Klepikov, V. Y.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1990SvAL...16..234K Altcode: No abstract at ADS Title: Prominence Fine Structure Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1990SoPh..127..109Z Altcode: The vertical fine structure in a quiescent prominence was modelled as an assembly of very narrow, optically thin threads. Random clusterings of the threads can account for the observed contrast and Hα line profiles of the fine structures. In this picture, each structure consists of a cluster of 7-20 elementary threads. Title: Velocity pattern of small scale magnetic fields Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1990SoPh..126..403D Altcode: High resolution observations of horizontal proper motions, as well as vertical Doppler velocities measured over two selected regions of small scale magnetic elements show a coherent behaviour. In a region with two opposite polarities, approching with a velocity of 0.4 km s-1, the material in between moves downwards with a velocity of 0.10 to 0.45 km s-1; while in a region with two peaks of the same polarity, moving apart with a velocity of 0.3 km s-1, the material in between moves predominantly upwards, with a velocity of up to 0.3 km s-1. Title: Video Magnetograms with Sub-Arcsecond Resolution Authors: Koutchmy, S.; Stauffer, F.; Zirker, J.; Keil, S.; Mann, R.; Coulter, R.; Hegwer, S. Bibcode: 1990BAAS...22..880K Altcode: No abstract at ADS Title: Coming: 24 hour surveillance of the sun. Authors: Koutchmy, S.; Vial, J. -C. Bibcode: 1990Rech...21...10K Altcode: No abstract at ADS Title: Analysis of the Solar Granulation in the Opacity Minimum Region Authors: Koutchmy, S. Bibcode: 1990IAUS..138...81K Altcode: No abstract at ADS Title: Small Scale Motions Over Concentrated Magnetic Field Regions of the Quiet Sun Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1990IAUS..138..153D Altcode: No abstract at ADS Title: Estimation of the line of sight amplitude of the magnetic field on threads of an active region prominence Authors: Koutchmy, S.; Zirker, J. B. Bibcode: 1990LNP...363..242K Altcode: 1990IAUCo.117..242K; 1990doqp.coll..242K No abstract at ADS Title: On the Spatial Distribution of Prominence Threads Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1990LNP...363..237Z Altcode: 1990doqp.coll..237Z; 1990IAUCo.117..237Z No abstract at ADS Title: A movie of small-scale Doppler velocities in a quiescent prominence Authors: Koutchmy, Serge; Zirker, Jack; Gilliam, Lou B.; Coulter, Roy; Hegwer, Stephen; Mann, Richard; Stauffer, Fritz Bibcode: 1990LNP...363..240K Altcode: 1990doqp.coll..240K; 1990IAUCo.117..240K A movie made of selected H off-band images of a typical Quiescent Prominences has been produced with the optical printer of NSO-S.P. High speed pictures were obtained with the UBF of the VTT on June 21, 1987 during 30 min of very good seeing, at a 20 sec cycling rate. Blue and red wings images are made at plus and minus .040 nm from line center, with a .022 nm passband. Original Pictures were enlarged to give an effective field of view of 100 × 80 arcsec2. Negative to positive superposition allows the mapping of strongly Doppler-shifted features (± 20 km sec-1) on a grey scale. The prominence threads are mostly discrete, allowing accurate measurement of proper motions. Typical transverse velocities of proper motions of small knots moving vertically downward are about 10 km sec-1 The movie also demonstrates the turbulent behaviour of the prominence plasma. Large-scale motions at lower transverse velocities are also clearly present. Title: High Resolution Analysis of Quiescent Prominences at National Solar Observatory / Sacramento Peak Observatory Authors: Darvann, Tron A.; Koutchmy, Serge; Stauffer, Fritz; Zirker, Jack B. Bibcode: 1990LNP...363..239D Altcode: 1990doqp.coll..239D; 1990IAUCo.117..239D We present preliminary results of several experiments carried out at the National Solar Observatory / Sacramento Peak (NSO/SP) Vacuum Tower Telescope (VTT) with the aim to resolve velocities and magnetic fields of the fine scale structures of filaments and prominences. Title: Le Soleil 24 Heures Sur 24 Authors: Koutchmy, S.; Vial, J. Bibcode: 1990Rech..217...10K Altcode: No abstract at ADS Title: High Resolution Observations of Motions and Structure of Prominence Threads Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1990LNP...363..244Z Altcode: 1990doqp.coll..244Z; 1990IAUCo.117..244Z H profiles and filtergrams were obtained of quiescent prominences at the National Solar Observatory, Sunspot, NM, with spatial resolution better than 1.6 arcseconds. The H profiles of individual threads are often Gaussian, but may show marked asymmetries, particularly near the prominence edges. Filtergrams, taken at ± 0.7 Å (± 30 km/sec) in H (with a 0.18 Å passband) show high speed knots and threads at the prominence edges, that persist with no perceptible change for at least 10 minutes. This result implies plasma motions (along essentially horizontal magnetic fields) over distances as large as 18000 km, i.e. much larger than typical thicknesses (5000 km) of H filaments. These motions may be associated with thread formation or decay, but continuous observations of this prominence over 6 hours show that the large-scale form of the prominence remained unchanged. Title: An Automated Procedure for Measurement of Prominence Transverse Velocities Authors: Darvann, Tron Andre; Koutchmy, Serge; Zirker, Jack B. Bibcode: 1990LNP...363..267D Altcode: 1990doqp.coll..267D; 1990IAUCo.117..267D A computer algorithm for measurment of transverse velocities (proper motion) in prominences has been developed. We present the method and examples of computed proper motion maps. The method is a modified version of the local cross correlation technique previously applied to granulation images (November 1986, Title et al 1987, November and Simon 1988, November 1988, Darvann 1988, Brandt et al 1988). Prominence images show much steeper intensity gradients and a wider range of spatial scales of fine structure than granulation images. Due to this we find it necessary to replace the prominence images by an image showing the intensity gradients (derivative of the intensity image). Furthermore, in our algorithm we compute absolute differences instead of correlation coefficients in order to reduce the influence of large scale intensity gradients across a local window (Karud 1988). We have tested the method on datasets obtained at the Vacuum Tower Telescope of NSO/SP. The accuracy of the algorithm is seen to be ±0.3 pixels which, in our data, corresponds to about 1/10 arcsec. Seeing effects are effectively reduced by averaging N cross correlation functions formed from images sampled t apart. We find that t = 120s gives the highest accuracy in the proper motion measurement when applied to our data consisting of quiescent prominences. The correlation coefficient between two interlaced, independent proper motion maps is as high as 0.92 when N=50. The size of the smallest structure for which a proper motion velocity can be measured is limited by the size of the smallest local window that can successfully be applied in the measurement. It needs to be large enough to contain some high contrast structures, typically 4×4 arcsec in our data. Our algorithm is self-adaptive to the data in the sense that the window size is changed automatically depending on the presence of local high contrast structures. We conclude that the method successfully produces prominence proper motion maps in addition to being able to correlation track prominence images. Furthermore the algorithm will be useful for destretching of prominence images before producing Doppler-grams or carrying out oscillation studies at high spatial resolution. Title: Comet P/Halley at a heliocentric preperihelion distance of 2.6 AU - Jet activity and properties of the dust coma Authors: Lamy, P. L.; Malburet, P.; Llebaria, A.; Koutchmy, S. Bibcode: 1989A&A...222..316L Altcode: This paper presents an in-depth analysis of a high-resolution photograph of comet P/Halley obtained on September 12, 1985 when it was a heliocentric distance of 2.6 AU preperihelion. The coma has a diameter of 138,000 km and exhibits structures which are interpreted as three jets, one best seen in the outer part of the coma extending to 29000 km and the two others, in the inner part extending to about 7000 km. The integrated magnitude and radial profiles of the coma are given showing that the comet does not follow the simple steady-state, radial outflow model. By combining the photometric result with nearly simultaneous ultraviolet and infrared observations, it is found that the strong reddening in the ultraviolet gradually levels off in the visible as the color becomes neutral at 2 microns and blue beyond 3 microns. A geometric albedo at zero phase angle of 0.04 is obtained, as well as a dust production rate of 30 to 120 kgs. Title: High resolution photographic Stokes polarimetry of small scale magnetic flux (poster) Authors: Keller, C. U.; Koutchmy, S. Bibcode: 1989hsrs.conf..443K Altcode: No abstract at ADS Title: Optimum filter and frame integration application to granulation pictures Authors: Koutchmy, O.; Koutchmy, S. Bibcode: 1989hsrs.conf..217K Altcode: No abstract at ADS Title: High resolution observations of the solar corona: why and how? Authors: Koutchmy, S.; Smartt, R. N. Bibcode: 1989hsrs.conf..560K Altcode: No abstract at ADS Title: Magnetic fields of solar prominences: strength and latitude distribution. Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1989BSolD..11...98K Altcode: According to the data obtained by a Nikolsky-type magnetograph during 1979 - 1986 there are two maxima in histograms "occurrence-B∥": O - 21 G and 27 - 36 G. The probability of the minimum between these maxima is equal to 82%. The first maximum may be divided into three distributions with peaks at 8, 15 and 20 G. The second maximum refers to active latitude prominences. The major part of the data (80%) belongs to the pre-minimum and minimum epochs. For this period the average latitude of prominence formation is less than 20°. The authors believe that the peak at 15 G characterizes the critical field strength of prominence formation. Title: Ground-Based Mirror Coronograph: First Results Authors: Smartt, R. N.; Koutchmy, S.; Schwenn, R. Bibcode: 1989BAAS...21..848S Altcode: No abstract at ADS Title: New Observations and Analysis of the Helium D3 Shell above the Limb Authors: Avrett, E. H.; Koutchmy, S. Bibcode: 1989BAAS...21..828A Altcode: No abstract at ADS Title: Image processing of coronal pictures Authors: Smartt, Raymond N.; Koutchmy, Olga; Koutchmy, Serge; Nitschelm, Christian; Sykora, Julius Bibcode: 1989STIN...8924252S Altcode: Coronal images contain many complex, superposed, faint, optically-thin structures: rays, loops, curved streamers, etc. The spatial resolution is often limited by the signal/noise ratio in the recording medium while the dynamic range in intensity is severely dominated by the radial gradient. The results obtained with a new simple image processing algorithm are applied to several typical eclipse and coronographic pictures. This 2D filter (second order difference operator in k-direction) shows superior quality by improving the signal/noise ratio, reducing the dynamic range and enhancing faint coronal structures. A comparison with results obtained with more commonly used 2D filters is also presented. The algorithm used here are briefly described, together with discussions of enhanced coronal images of coronal physics interest. Title: On the Spatial Distribution of Prominence Threads Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1989HvaOB..13...41Z Altcode: No abstract at ADS Title: Photoelectric Analysis of the Solar Granulation in the Infrared Authors: Koutchmy, S. Bibcode: 1989ASIC..263..347K Altcode: 1989ssg..conf..347K No abstract at ADS Title: Granulation In and Out of Magnetic Regions Authors: Koutchmy, S. Bibcode: 1989ASIC..263..253K Altcode: 1989ssg..conf..253K No abstract at ADS Title: An Automated Procedure for Measurement of Prominence Transverse Velocities Authors: Darvann, T. A.; Koutchmy, S.; Zirker, J. B. Bibcode: 1989HvaOB..13..243D Altcode: No abstract at ADS Title: Prominence fine structure. Authors: Zirker, J. B.; Koutchmy, S. Bibcode: 1989BAAS...21.1027Z Altcode: No abstract at ADS Title: Solar cycle variations of coronal structures Authors: Loucif, M. L.; Koutchmy, S. Bibcode: 1989A&AS...77...45L Altcode: Using eclipse pictures of the solar corona, properly scaled drawings have been prepared to constitute a short atlas of coronal structures. These drawings have been used to extract 2 parameters which are further considered with respect to the sunspot number and the sunspot cycle: the extension of polar regions free of coronal streamers and the average radial deviation of large streamers. The flattening index deduced from the photometric analysis of a larger number of eclipse pictures is also considered. The out-of-phase behavior of several coronal parameters is confirmed. The results are discussed in the light of the analysis of the green-line activity as observed during 30 years at the Pic du Midi Observatory. The N-S asymmetric behavior of the activity in different solar hemispheres and the occurrence of a powerful secondary maximum of coronal activity are discussed. Title: On variation of prominence heights with the solar cycle. Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1988BSolD...5...77K Altcode: The behaviour of prominence heights with the solar cycle is studied. Prominence pictures taken by the Nikolsky magnetograph in 1979 - 1986 are used. A dependence of the average height with time is analysed. The minimum height took place in the fall of 1984, 2 years before the solar activity minimum. Histograms of "prominence occurrence versus height" were constructed for different phases of the solar cycle. It is pointed out that the behaviour of the average prominence height depends on the variation of the distribution of prominence heights with the solar cycle. The minimum height is due to a relative increase of the number of prominences which is less than 25 arcsec. The occurrence of these prominences has a peak before the minimum of solar activity. Such prominences are predominantly located at the latitudes 0 - 20°. Title: Optical Detection of Space Debris Using a Large Achromatic Coronograph Authors: Koutchmy, S.; Nitschelm, C. Bibcode: 1988Ap&SS.143...45K Altcode: The space debris detectin will become greater and greater in the near future with the space debris enhancing. We introduce a theoretical approach of this problem assuming the using of a new generation large coronograph. We get some interesting — and alarming — results about the great probability to be able to observe space debris with this new ground-based large coronograph. Title: Spectroscopic Coronal Observations Using A High-Sensitivity Camera Authors: Smartt, R. N.; Colley, S. A.; Gilliam, L. B.; Koutchmy, S.; Zirker, J. B. Bibcode: 1988BAAS...20..704S Altcode: No abstract at ADS Title: Space-borne coronagraphy Authors: Koutchmy, Serge Bibcode: 1988SSRv...47...95K Altcode: We consider the main aspects of a rather delicate discipline, space-borne coronagraphy, which is essentially performed with white-light, externally-occulted coronagraphs. Methods of observation and recent results are presented in a scientific section; a short account of historical rocket-borne and balloon-borne experiments is also given. The review concentrates on both the NRL-type coronagraphs and the HAO-type coronagraphs, stressing the essential features and merits of numerous experiments which were flown. A small section is devoted to other designs. A large number of figures, including many drawings, are used to illustrate the growing complexity of experiments. Title: On the distribution of prominence heights. Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1988BSolD1988...75K Altcode: The distribution of prominence heights is studied. Prominence pictures obtained in 1979 - 1986 by the Nikolsky magnetograph are used. Discreteness in the distribution of heights is found. There are two peaks: the first narrow peak at 20 - 25 arc sec and the second one at 35 - 45 arc sec. One finds that the prominences with heights less than 25 arc sec locate mainly at the latitude interval 0 < φ ≤ 20°. During the preminimum and minimum of solar activity the average latitude of the filaments (prominences) formation is 18 - 21°. The most likely height interval for prominence formation is at 20 - 25 arc sec (which is the critical height). Title: Solar cycle variations of coronal neutral lines and polar regions activity. Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S.; Sivaraman, K. R. Bibcode: 1988sscd.conf..362M Altcode: Observations of the corona, of prominences, of polar faculae and of large scale magnetic fields show solar activity over all latitudes, in contrast with sunspot activity, which is limited to mid-latitudes. The global behaviour of the solar activity is considered here thanks to the analysis of chromospheric synoptic maps which include the location of Hα and Ca II K prominences. The process of "migration" of neutral lines during the cycle (supposed to represent the large scale coronal magnetic field) is shown. Title: Image processing of coronal pictures. Authors: Koutchmy, Olga; Koutchmy, Serge; Nitschelm, Christian; Sykora, Julius; Smartt, Raymond N. Bibcode: 1988sscd.conf..256K Altcode: The authors present the results obtained with a new simple image processing algorithm applied to several typical eclipse and coronographic pictures. This 2D filter (second order difference operator in k-direction) shows superior quality by improving the signal/noise ratio, reducing the dynamic range and enhancing faint coronal structures. A comparison with results obtained with more commonly used 2D filters is also presented. The authors describe briefly the algorithm used, together with discussions of enhanced coronal images of coronal physics interest. Title: Small scale coronal structures. Authors: Koutchmy, Serge L. Bibcode: 1988sscd.conf..208K Altcode: The author reviews a few problems connected with the observation and the analysis of fine scale coronal density structures. The inner corona and middle corona are considered. The relations existing between the coronal magnetic fields and the coronal dynamics at small scale, including impulsive events are emphasized. Title: A Study of Disconnection Velocities in the Plasma Tail of P/halley Authors: Caron, R.; Koutchmy, S.; Sarrazin, M. Bibcode: 1988scaa.conf..158C Altcode: 1988IAUCo..98..158C No abstract at ADS Title: Etude de la dynamique du nuage zodiacal par la mesure du décalage Doppler. Authors: Lamy, P.; Koutchmy, S.; Bücher, A.; Robley, R. Bibcode: 1988jopl.conf..227L Altcode: At the Pic-du-Midi Observatory, the authors have started a program to observe the spectrum of the zodiacal light in the region of the b absorption lines of Mg I. They use a 1 m spectrograph with a holographic grating followed by a focal reducer to obtain a 19 Å/mm dispersion over the micro-channel plate camera. Calibrated spectra obtained with an exposure time of 10 minutes systematically show earth atmospheric emission lines attributed to both N I and OH. The temporal variability of these emissions prevents an accurate determination of the line profiles. Title: Observations et propriétés des poussières de la comète de Halley. Authors: Lamy, P.; Perrin, J. M.; Koutchmy, S.; Grün, E.; Llebaria, A.; Malburet, P. Bibcode: 1988jopl.conf..211L Altcode: The authors present the results of various observations and analysis of the dust grains of comet Halley. Title: High Spatial Resolution Coronal Physics: The Need for Larger Coronagraphs Authors: Smartt, R. N.; Koutchmy, S.; Zirker, J. P. Bibcode: 1987BAAS...19Q1122S Altcode: No abstract at ADS Title: Des observations à grand champ et en couleur. Authors: Caron, R.; Koutchmy, S.; Sarrazin, M. Bibcode: 1987LAstr.101..255C Altcode: No abstract at ADS Title: Night sky optical spectrum from a high altitude observatory. Authors: Louistisserand, S.; Bucher, A.; Koutchmy, S.; Lamy, P. Bibcode: 1987A&AS...68..539L Altcode: Night sky spectrum between 380 and 660 nm with effective spectral resolution of 0.2 nm is presented for evaluation of effects produced by the different sources of light including lights of urban origin. Numerous emission lines superposed on a continuum spectrum are identified. Title: Small-scale motions over concentrated magnetic regions of the quiet Sun Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S. Bibcode: 1987SoPh..109...19D Altcode: We have used a 5.5 min time-sequence of spectra in the Fe I lines λ5576 (magnetically insensitive), λ6301.5 and λ6302.5 (magnetically sensitive) to study the association of concentrated magnetic regions and velocity in the quiet Sun. After the elimination of photospheric oscillations we found downflows of 100-300 m s −1, displaced by about 2″ from the peaks of the magnetic field; this velocity is comparable to downflow velocity associated with the granulation and of the same order or smaller than the oscillation amplitude. Quasi-periodic time variations of the vertical component of the magnetic field up to ± 40% were also found with a period near 250 s, close to the values found for the velocity field. Finally we report a possible association of intensity maxima at the line center with peaks of the oscillation amplitude. Title: L'observation des filigrées. Authors: Koutchmy, S. Bibcode: 1987JAF....29...14K Altcode: No abstract at ADS Title: Some Statistical Properties of the Magnetic Field in Prominences Authors: Kim, I.; Koutchmy, S.; Stellmacher, G.; Stepanow, A. I. Bibcode: 1987rfsm.conf..289K Altcode: Magnetic field observations based on the Zeeman effect, measuring the longitudinal component B∥ of the field with an entrance hole of 6.4 arcsec diameter, were obtained for a great number of prominences during 1979 to 1985. Title: Improved measurements of scattered light level behind occulting systems. Authors: Koutchmy, S.; Belmahdi, M. Bibcode: 1987JOpt...18..265K Altcode: 1987JOp....18..265K No abstract at ADS Title: Micrométéorites et débris orbitaux. Authors: Koutchmy, S. Bibcode: 1987LAstr.101..426K Altcode: No abstract at ADS Title: Properties of a Concentrated Magnetic Field Region Authors: Koutchmy, S.; Stellmacher, G. Bibcode: 1987rfsm.conf..103K Altcode: Further results concerning the fine structure of concentrated magnetic field regions or network elements, observed near disk center well outside of active regions, are presented. Title: Ground-Based Large-Scale Monochromatic Images of Comet Halley during the Giotto Flyby Authors: Koutchmy, S.; Lamy, P.; Loucif, M.; Malburet, P. Bibcode: 1986ESASP.250c..79K Altcode: 1986ehc3.conf...79K A wide-field camera (f = 135 mm) equipped with an image-tube was set up at the geophysical observatory of Tamanrasset during the first half of March. Monochromatic images were obtained in CN (390 nm), CO+ (426.3 nm) and in the continuum (582 nm), in March 14.19, a few hours after the Giotto flyby. Title: The Disconnection Events of January 10 and April 8 1986 IN the Plasma Tail of Comet Halley Authors: Caron, R.; Guerin, P.; Koutchmy, S.; Sarrazin, M.; Zimmermann, J. P. Bibcode: 1986ESASP.250c.143C Altcode: A sequence of 6 white-light pictures covering 10 hrs of the Jan. 10, 1986 Halley's comet plasma tail disconnection was analyzed in order to deduce the variation of the relative velocity of the ion tail revealing a sudden acceleration. A second sequence of 8 CO(+) pictures covering 2.5 hr of the April 8, 1986 large disconnection event was obtained and the velocity field was studied. An attempt to trace the origin of this event on early sequence of white light pictures is discussed, as well as the occurrence of sudden accelerations. The images confirm sudden increases or decreases of the velocity, but it is difficult to say whether these changes can be wholly attributed to sudden acceleration. Title: Early resolved structures in the coma of Comet Halley Authors: Dossin, F.; Guerin, P.; Koutchmy, S.; Lamy, P.; Malburet, P. Bibcode: 1986ESASP.250b.173D Altcode: 1986ehc2.conf..173D Three high-resolution photographs of comet Halley were obtained on September 12, 1985 with the Schmidt telescope operated by CNRS and Liège University at the Observatoire de Haute-Provence on hypered Kodak 2415 film and exposure times of 1 hour. The best image (FWHM of 2 arcsec) has been analyzed in order to deduce the 2-dimensional distribution of light presumably scattered by the dust. Two jet-like structures are present in the near nuclear region, one extending outward up to 15 arcsec. The total absolute magnitude has also been determined. Title: Étude de la structure de la couronne solaire grâce aux éclipses totales. Authors: Koutchmy, Serge Bibcode: 1986LAstr.100..499K Altcode: The methods used and results of worldwide photometric imaging of the solar corona during total eclipses are summarized. Combining the observations from different sites enlarges the temporal window of the observations from minutes at a single site to several hours of data. Attention is given to techniques applied to estimate the contributions from light reflected by the coronal plasma and by dust in the interplanetary medium. Sample coronographic images illustrate methods employed to study coronal structures, mainly by tuning the instruments to H-alpha wavelengths. Magnetographic data are also discussed which are used to map the magnetic field around the sun and thereby gain information on the solar dynamo. Title: L'observation des contacts d'une éclipse et son intérêt. Authors: Koutchmy, Serge; Sarrazin, Michel Bibcode: 1986LAstr.100..525K Altcode: Analytical techniques for predicting the occurrence of a total eclipse at a particular location are summarized. Emphasis is placed on the use of two opposing sites on the limb of the moon as the loci for predicting the location and total area of a solar eclipse. The calculations are carried out using astronomical ephemerides and, in the case of observations from an aircraft, consider the magnetic declination of the earth and the flight path of the aircraft. Sample data are presented for measurements of the eclipse area predicted and measured during the flight of an instrumented aircraft. The alterations in the location of the lunar limb due to the coronal light of the sun are noted. Title: The solar granulation. II - Photographic and photoelectric analysis of photospheric intensity fluctuations at the meso-granulation scale Authors: Koutchmy, S.; Lebecq, C. Bibcode: 1986A&A...169..323K Altcode: A statistical analysis of the intensity fluctuations of the solar photosphere, recorded photoelectrically, shows the influence of both seeing effects and especially the 5 min oscillations when intensity fluctuations at scales larger than the scale of the granulation are considered. A one-dimensional photo-electric set of records was time-averaged in order to show the existence of quasi-stationary cells in the range 5arcsec - 50arcsec, with amplitude modulations of up to ±30K. The photographic processing of a 23-min time sequence of excellent granulation pictures also showed the existence of cells of quasi-stationary intensity modulations. The amplitudes and stationary nature are larger for larger sizes, but the existence of cells at the meso-granulation scale is fully confirmed. Title: Dynamical properties of a pre-perihelion comet tail. I. December 6, 1985 observations of P/Halley 82i. Authors: Guerin, P.; Koutchmy, S.; Vial, J. C. Bibcode: 1986A&A...167..395G Altcode: Wide field pictures of comet P/Halley 1982i obtained every hour on December 6, 1985, have been analyzed in order to study the dynamics of low intensity plasma structures in the tail. The deduced radial velocities increase from 50 to 80 km s-1 over distances of 2 to 6×106km. The measured apparent aberration angle is interpreted as a result of a large polarward solar wind velocity component. Title: The 1981 total solar eclipse. III - Photometric study of the prominence remnant in the reversing south polar field Authors: Stellmacher, G.; Koutchmy, S.; Lebecq, C. Bibcode: 1986A&A...162..307S Altcode: High resolution white light colour pictures obtained during the 1981 total solar eclipse were used for a photometric analysis of the S-pole region. A small helmet-like streamer was visible over the S-polar limb overlying a faint polar prominence from the polar crown belt of filament channels that reached 87° latitude at the eclipse date. Typical electron densities deduced are ne ≅ 2×109cm-3 for the activated top of the prominence and ne ≅ 6×108cm-3 for the associated coronal structures. Upward velocities up to 160 km s-1 are obtained for the eruptive prominence parts. The authors found that dynamic processes are controlled by magnetic forces for fields B ≥ 3.5 Gauss, and that the coronal structures are apparently connected with the faintest and most dynamic parts of the prominence. Title: A kinematic analysis of the disconnection of the plasma tail of cometP/Halley, January 10, 1986. Authors: Guerin, P.; Koutchmy, S. Bibcode: 1986CRASB.303..147G Altcode: 1986CRASM.303..147G Photographic images of Halley's Comet tail were analyzed to determine if disconnections of the tail from the comet were due to the crossing of the Comet from one solar magnetic sector to another. The six photographs, taken over a 16 hr period on Jan. 10, 1986, provided detail sufficient for about 1.2753 arcmin accuracy in the Comet ephemerides and the tracks of nodosities at the nucleus and their antisunward movement and separation from the cometary tail. The images depict the simultaneous acceleration of an entire separated tail section region followed by a deceleration of the same section, suggesting that the tail crossed a pre-existing region of interplanetary space. The deceleration to a velocity comparable to the remaining tail took a period of 9 hr. Insufficient data were available for explaining the appearance and behavior of a bar that appeared at the sunward end of the separated nodosity and seemed associated with an influx of solar wind matter as the IMF changed polarity. Title: Periodic Comet Halley (1982i) Authors: Ney, E. P.; Knutson, A. G.; Wootten, Alyn; Loren, R.; Koutchmy, S.; Lamy, P. Bibcode: 1986IAUC.4161....1N Altcode: E. P. Ney and A. G. Knutson, University of Minnesota, report the following infrared magnitudes measured with a 26" diaphragm at the O'Brien Observatory: 1985 Dec. 12.08 UT, K = 6.8, L = 6.1, [8.6 micron] = -0.5, N = -1.8, [12.5 micron] = -1.9, [18 micron] = -3.3; Dec. 14.00, [8.6 micron] = 0.9, N = -0.8, [12.5 micron] = 0.0, [18 micron] = = -2.8; Dec. 25.05, J = 6.8, K = 7.1, L = 5.2, M = 3.1, [8.6 micron] = -0.5, N = -1.6, [12.5 micron] = -1.6, [18 micron] = -3.0; 1986 Jan. 1.0, N = -1.4, [12.5 micron] = -0.9; Jan. 7.9, H = 6.0, K = 6.1, L = 3.9, M = 1.2, [8.6 micron] = -1.5, N = -2.8, [12.5 micron] = -2.6, [18 micron] = -4.0. The silicate feature at 10 micron is ~ 0.5 mag above the continuum. A. Wooten, National Radio Astronomy Observatory, reports: "R. Loren, University of Texas, obtained spectra of P/Halley in the region of the P(2,1) line of protonated water (H3O+) at 307.19241 GHz on Jan. 6 with the 4.9-m telescope of the Millimeter Wave Observatory at Fort Davis. No emission was detected, rms(TR*) = 0.85 placing a preliminary upper limit of 5 x 10**-27 s**-1 for the H3O+ production rate. Receiver tuning was verified through observation of CHEOH at 307.16594 GHz in OMC-1." S. Koutchmy, Institut d'Astrophysique, Paris; and P. Lamy, Laboratoire d'Astronomie Spatiale, Marseilles, telex that 100 image-tube spectra (180 A/mm resolution, range 350-700 nm) were obtained with the Haute Provence Observatory's 0.8-m telescope during 1985 Dec. 10-15. CN emission was detected, extending up to 2 deg away from the sun, but no ions were noted until Dec. 12. From Dec. 13.8 UT onward the N2+ (0,0) line at 391.4 nm was seen in the vicinity of the coma and extending in the antisolar direction up to 2 deg. Observations with the Marly spectrograph (range 326-526 nm, dispersion 80 A/mm, slit width 50 micron, slit length projection 3'7, IIa-O hypered plates) on the 1.20-m f/6 telescope during 1985 Dec. 2.76-2.98 and 3.72-3.97 UT revealed CN, C2 and C3 (all well observed); N2+ (0,0) extending over 16"; CO+ (3,0) lines at 400.18 and 402.4 nm extending over 37" and 14", respectively; CO2+ (0,1) at 367.4 nm was suspected; numerous Fraunhofer absorption lines (including H and K and several Fe lines) were also noted. Photographs (hypered IIIa-J and 2415 emulsions) of the plasma tail with the 0.62-m f/3.5 and 0.30-m f/2 Schmidt telescopes during Dec. 3- 15 revealed an inner part (extending < 1 deg from the head) whose orientation oscillated about the antisolar direction with a maximum deviation of + 5P and a characteristic time of one to two days. Title: Les éclipses totales solaires. Authors: Koutchmy, S. Bibcode: 1986LAstr.100..497K Altcode: No abstract at ADS Title: Relations Between Large Scale Coronal Structure, Chromospheric Filaments and the Solar Cycle Authors: Koutchmy, S.; Loucif, M.; Koutchmy, O. Bibcode: 1986stp..conf...67K Altcode: No abstract at ADS Title: Periodic Comet Halley (1982i) Authors: Jewitt, D.; Meech, K.; Ricker, G.; Lamy, P.; Koutchmy, S.; Vial, J. C. Bibcode: 1985IAUC.4148....1J Altcode: D. Jewitt, K. Meech, and G. Ricker, Massachusetts Institute of Technology, communicate: "Observations from McGraw-Hill Observatory on Kitt Peak over 4 nights show variable structures in the inner coma of P/Halley. Images were taken through broad and narrowband interference filters using the MIT 'MASCOT' CCD camera on the 1.3-m telescope. Jet-like structures were observed in position angles 358 and 313 on Nov. 29 UT. The jets extended 10 000 km in the plane of the sky and had widths comparable to the atmospheric seeing. The jets were visible in both broad and narrowband continuum filters and are probably dust features. The jets showed no variation in position angle or brightness in an observing interval of > 3 hr but were absent on the preceding and following nights." Meech and Jewitt also report: "Observations of P/Halley with the Kitt Peak 0.61-/0.91-m Schmidt telescope (with baked IIIa-J plates and exposure times 30-60 min) show that extensive tail development has occurred within the past month. Observations on Nov. 6-9 showed only a transient, faint anti-solar tail (length 20' on Nov. 6.20) which faded in < 1 day. Observations on Dec. 4-8 show a persistent plasma tail (length > 2.5 deg) displaying a classical streamer morphology. We are able to follow knots, kinks, and streamers in the tail for up to 6 hr. The measured speeds of 3 tail knots are 190, 216, and 240"/hr (39, 45, and 50 +/- 5 km/s along the tail, km/s), considerably less than the solar wind speed but similar to the speeds measured in the tails of other comets. No evidence for acceleration of the features is seen. Two episodes of ray formation have been seen in 25 hr of observation; the rays form in ~ 1 hr and evolve over several hr, but fade in < 18 hr. The tail as a whole shows gross brightness changes from night to night. No dust tail is seen." P. Lamy, Laboratoire d'Astronomie Spatiale, Marseille, and S. Koutchmy, Institut d'Astrophysique, Paris, telex: "Four consecutive 1-hr-exposure IIIa-J hypered plates obtained between Dec. 6.79-6.96 UT by Koutchmy and J. C. Vial with the 0.62-m f/3 Schmidt telescope of Haute Provence Observatory show a disturbed, narrow, plasma tail of length > 2 deg. The tail's inner part deviates southward from the anti-solar direction by 4.8 +/- 0.7 deg; the outer part widens and nears the anti-solar direction. The point of bifurcation seems to move radially outward with time." Title: Measurement of magnetic fields in solar prominences Authors: Nikolskij, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I. Bibcode: 1985AZh....62.1147N Altcode: Measurements of magnetic fields in solar prominences on the basis of the Zeeman effect are described. The circular polarization along the entire line profile is recorded. The spectral scanning is done with a Fabry-Perot interferometer and the modulation is done with a lithium niobate crystal. The influence of the instrumental characteristics on the measurements is discussed. A histogram of the frequency of appearance of longitudinal fields with a spatial resolution of 6-8 arcsec for prominences of 1979-1982 has clear maxima at 8 and 20 G. The peak at 20 G corresponds to prominences of active latitudes (less than + or - 35 deg) for which the angle beta between the long axis of the filament and the line of sight was close to 25 deg. From a comparison with the results measurement of the total field vector (data of Athay et al.) for prominences of the same epoch (1979-1981) the following conclusion is drawn about the field orientation: For prominences of active latitudes B parallel about = B; i.e., the angle between the long axis of a filament and the line of sight is close to the angle between the long axis of the filament and the magnetic field vector. Title: Measurement of Magnetic Fields in Solar Prominences Authors: Nikolskii, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I.; Stellmacher, G. Bibcode: 1985SvA....29..669N Altcode: No abstract at ADS Title: The 1981 total solar eclipse corona. II. Global absolute photometric analysis. Authors: Lebecq, C.; Koutchmy, S.; Stellmacher, G. Bibcode: 1985A&A...152..157L Altcode: Detailed results of the absolute photometry of the solar corona during the July 31, 1981 total eclipse are presented together with a morphological analysis. The basic calibration method uses the detailed photometry of images of stars present on the same coronal picture. Both sky intensity and coronal aureola variations over the field are carefully evaluated. The recent axi-symmetric non-spherical model of the F-corona is introduced and the relevant K-corona intensity variations are derived. The determinations of the Ludendorf index of flattening and the integrated total brightness of the K-corona alone are made and discussed in relation to the phase of the sunspot cycle of activity. Title: Periodic Comet Halley (1982i) Authors: Koutchmy, S.; Lecacheux, J.; Dossin, F. Bibcode: 1985IAUC.4112....2K Altcode: S. Koutchmy and J. Lecacheux, Institut d'Astrophysique, Paris, and Meudon Observatory, report good-resolution, 1-hr exposures on Kodak 2415 hypered film obtained on Sept. 12-14 by F. Dossin and Koutchmy with the 0.62-m f/3 Schmidt telescope of Haute-Provence Observatory; the P/Halley images show a resolved central region with an average FWHM of 5"7 (5"4 north-south, 6"6 east-west) with an overall coma extension from the nucleus of 58" (65" westward). The inner coma near the nucleus was V-shaped with arms 3"5 long at p.a. 30 and 300. An additional faint, jet-like feature at p.a. 30, extending radially up to 15" from the nucleus, is apparent on the picture (free of faint star trails) obtained on Sept. 12.094 UT; magnitudes measured by flux integration in circles of 10" and 120" diameter were V = 15.0 +/- 0.2 and 13.8, respectively. Title: Solar constant variabilities. Authors: de Charentenay, C.; Koutchmy, S. Bibcode: 1985CRASB.301..151D Altcode: 1985CRASM.301..151D The solar-constant variations which were measured from Feb. 16-Nov. 7, 1980 by means of the NASA ACRIM experiment on board the SMM satellite are analyzed. It is shown that if the radiative deficit produced by the passage of sunspots on the solar disk and the radiative flux excess produced by the passage of faculae at the edge of the solar disk are introduced on a weekly basis, the measured variations can be reproduced. Meudon Observatory synoptic maps are used to measure the faculae surfaces. An empirical model which specifies the relation between the activity cycle and the long-term solar-constant variations is presented. A relative decrease of the solar constant at the time of the sunspot activity minimum is predicted. Title: On a possible relation of the law of planetary distances to the 160-minute pulsation of the sun. Authors: Kotov, V. A.; Koutchmy, S. Bibcode: 1985IzKry..72..199K Altcode: The discovery of the global solar pulsation with the period of P0 = 160m enables to introduce characteristic wavelength L = c×P0 = 19.24 A.U. for the solar system, where c is the speed of light. A corresponding analysis of planetary distances reveals the existence of a statistically significant quasi-commensurability between L and 2πai for inner planets and between 2ai and L for outer ones (ai being the major semi-axis of a planetary orbit). It is suggested that this L-commensurability can offer new approach to an explanation of the well-known Titius-Bode law for planetary distances. The physical mechanism enforcing the L-commensurability in the solar system is presumably related with 160m-gravitational waves from some external source of unknown nature. Title: The F-Corona and the Circum-Solar Dust Evidences and Properties (ir) Authors: Koutchmy, S.; Lamy, P. L. Bibcode: 1985ASSL..119...63K Altcode: 1985IAUCo..85...63K; 1985piid.proc...63K This review deals with the main properties of the F-corona. Analysis of its morphology and photometry allows to derive a new axisymmetric, non-spherical model. Polarization, color and infra-red properties are further considered. The authors suggest the existence of a variable "local" component superimposed on a quasi-stationary "far" component. Title: Color photographic photometry of the inner zodiacal light observed from the Salyut 7 orbital station Authors: Koutchmy, S.; Nesmianovich, I. A.; Dzhanibekov, V. A.; Nikolskii, G. M. Bibcode: 1985AbaOB..60..207K Altcode: Photometric data of the inner zodiacal light obtained during the Soviet-French mission aboard Salyut 7 are analyzed. Isophote curves for zodiacal brightness are examined; it is observed that the plane of maximum zodiacal light brightness is close to the orbital plane of Venus. The law governing the brightness intensity is given, and the relation between brightness intensity and elongation is studied. Title: A colorimetric and photometric analysis of the inner zodiacal light observed from the orbiting laboratory "Salyut-7". Authors: Dzhanibekov, V. A.; Koutchmy, S.; Nesmyanovich, I. A.; Nikol'Skij, G. M. Bibcode: 1985AbaOB..60..207D Altcode: The authors present the results of a photographic photometry of the best colour picture of the inner zodiacal light, obtained during the joint Soviet-French mission aboard the Salyut-7 orbiting laboratory. Isophote-map indicates that the plane of maximum zodiacal light brightness is very near the orbital plane of the planet Venus. Intensity in the plane of maximum brightness can be matched using the law BZL ≡ E-2.04 at the elongations 23° ≤ ɛ ≤ 35°, the colorimetric index being bound to be nearly solar. The influence of submicron-sized particles seems to be excluded. Title: The 160-min period in the solar system: solar pulsation and the spin rates of planets and asteroids Authors: Kotov, V. A.; Koutchmy, S. Bibcode: 1985BCrAO..70...37K Altcode: 1985BuCri..70...37K; 1987BCrAO..70...37K No abstract at ADS Title: Magnetic and Velocity Field Analysis of a Quiet Region near the Center of the Sun Authors: Dara-Papamargariti, H.; Koutchmy, S. Bibcode: 1985LNP...233..231D Altcode: 1985hrsp.proc..231D A selected region of the quiet sun near the center of the disc was analyzed in order to deduce parameters concerning regions of highly concentrated magnetic field, including network elements. The present analysis covers a sequence of spectra corresponding to a total time laps of 6 min over the same region. Spectra of both magnetically sensitive and insensitive lines were measured in detail in order to deduce the velocity distribution around magnetic flux tubes. Large amplitude five minute oscillatory components were removed using an averaging over time procedure. Preliminary results are discussed as well as factors which could affect their interpretation. Title: A possible relation between planetary distances and the 160-minute solar pulsation. Authors: Kotov, V. A.; Koutchmy, S. Bibcode: 1985BCrAO..72..171K Altcode: 1985BuCri..72..171K; 1987BCrAO..72..171K No abstract at ADS Title: Doppler Shifts Measurements of the Zodiacal Light at the PIC Midi Observatory Authors: Robley, R.; Buecher, A.; Koutchmy, S.; Lamy, Ph. Bibcode: 1985ASSL..119...85R Altcode: 1985IAUCo..85...85R; 1985piid.proc...85R The authors have started a program to observe the spectrum of the zodiacal light in the region of the b absorption lines of Mg I. They use a 1 meter spectrograph with a holographic grating followed by a focal reducer to obtain a 19 Å/mm dispersion over the micro-channel plate camera. Calibrated spectra obtained with an exposure time of 10 minutes systematically show earth atmospheric emission lines attributed to both N I and OH. The temporal variability of these emissions prevents an accurate determination of the line profiles. The authors best processed measurements of Doppler shifts obtained during five nights do not allow to discriminate between circular and hyperbolic orbits of the interplanetary dust. Title: Facular and Duration of the Solar Cycle Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S. Bibcode: 1985BSolD...8...53M Altcode: No abstract at ADS Title: A magnetograph with scanning along the whole profile of a spectral line. Authors: Nikol'Skij, G. M.; Kim, I. S.; Klepikov, V. Yu.; den, O. E.; Stepanov, A. I.; Koutchmy, S. Bibcode: 1985AbaOB..60..177N Altcode: A magnetograph with scanning along the whole profile of the line is described. This instrument was built for measuring magnetic fields in prominences and in the corona. The study of the Zeeman effect is carried out in different emission lines. Title: Global solar oscillations observed from relative near-IR photosphericbrightness fluctuations. Authors: Kotov, V. A.; Koutchmy, S.; Kononovich, Eh. V.; Ryzhikova, N. N.; Tsap, T. T. Bibcode: 1985BCrAO..73...24K Altcode: 1987BCrAO..73...24K No abstract at ADS Title: Polar faculae and duration of the solar cycle. Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S. Bibcode: 1985BSolD1985...53M Altcode: An analysis of a 20-year series of daily observations of polar faculae has been made. It is shown that for the cycle with a one-fold polarity reversal the solar activity in the polar zone correlates rather well with the sunspot activity in 2.5 cycles, i.e. in 27 - 28 years. In the cycles with a three-fold polarity reversal the shift takes place in about 6 years. A conclusion is made that the global process of solar activity at all the latitudes lasts for about 17 - 18 years. Title: A Coronascanner for a Sun Oriented Space Mission Authors: Koutchmy, S.; Lamy, P. L. Bibcode: 1985ASSL..119..141K Altcode: 1985IAUCo..85..141K; 1985piid.proc..141K No abstract at ADS Title: Photometric calibrations of an MCP space qualified photographic-camera Authors: Koutchmy, S.; Verlhac, A. Bibcode: 1985A&A...142..355K Altcode: The authors describe the methods developed to guarantee quantitative calibrations of a high sensitivity micro-channel plate photo-camera designed to obtain large scale night sky pictures of astronomical and geophysical interest in the optical and near infrared spectral range. In-flight calibrations were obtained with a sensitometer and absolute calibrations were performed in laboratory with a quasi-monochromatic black body source. Results obtained for calibrating the camera are given with emphasis on the comparison of measurements deduced in ground based and orbital condition. Title: Photographic Observations of the Inner Zodiacal Light Aboard Saliout 7 Authors: Nikolskii, G.; Koutchmy, S.; Lamy, P. L.; Nesmianovich, I. A. Bibcode: 1985ASSL..119....7N Altcode: 1985IAUCo..85....7N; 1985piid.proc....7N Color photographs of the inner zodiacal light were obtained aboard Salyut 7 with Kodak Ekta 400. Absolute calibrations were performed in-flight with attenuated sunlight. The photometric analysis was carried out in three colors and corrections were introduced for the O I emission of the F layers. The brightness of the zodiacal light along the ecliptic is found in good agreement with published data while its color is found slightly redder than the sun. Its out-of-ecliptic variation coincides neither with the fan nor the ellipsoidal model; the photometric axis is found near the projection of the orbital plane of Venus. Title: Astrophysical and geophysical observations with piramig/salyut 7 experiment Authors: Levasseur-Regourd, A. C.; Courtes, G.; Herse, M.; Koutchmy, S.; Lamy, P.; Muliarchik, T. M.; Rocca-Volmerange, B.; Savchenko, S. A.; Secher, B.; Tovmassian, H. M.; Beresovoy, A. N.; Chretien, J. L.; Ivanchenkov, A. S.; Djanibekov, V. A.; Lebedev, V. V.; Popov, L. I.; Savitskaya, S. E.; Serebrov, A. A. Bibcode: 1985AdSpR...5c..27L Altcode: 1985AdSpR...5...27L The facility offered by the Salyut 7 vehicle has allowed teams of scientists of 3 CNRS french laboratories to develop an instrument optimized for several disciplines in astrophysics and geophysics. P.I.R.A.M.I.G. (Photography Infra-Red Atmosphere, Interplanetary Medium, Galaxies) is a wide field (10° and 40°) camera devoted to high sensitivity photographic photometry. The spectral range is limited to the visible and near-infrared (400-850 nm), the main advantage being to observe above the absorving and emitting layers of the atmosphere. Title: Global oscillations of the sun according to observations of (relative) fluctuations of photospheric brightness in the near infrared Authors: Koutchmy, S.; Kononovich, E. V.; Ryzhikova, N. N.; Kotov, V. A.; Tsap, T. T. Bibcode: 1985IzKry..73...26K Altcode: The instrument designed for monitoring of relative center-to-limb brightness fluctuations of the photosphere in near IR spectral range (λ = 1.65 μm) is described. Analysis of 67 days of observations carried out in 1981 - 1982 shows clearly the presence of 160-min variations of the differential, center-to-limb intensity with an average amplitude of about 3×10-5 in units of the {average solar} brightness near 1.65 μm or 0.2K in terms of the temperature of the photosphere. Title: G. M. Nikolsky, 1929 - 1982. Authors: Koutchmy, S. Bibcode: 1985ASSL..119D..23K Altcode: No abstract at ADS Title: Empirical model of the solar corona using solar-cycle related parameters. Authors: Koutchmy, S.; Loucif, M. Bibcode: 1984ESASP.220..265K Altcode: 1984ESPM....4..265K Using a set of eclipse pictures, the distribution of stream lines over the outer corona was analyzed. Title: Comparative magnetographic observations in different prominence lines Authors: Nikolsky, G. M.; Kim, I. S.; Koutchmy, S.; Stellmacher, G. Bibcode: 1984A&A...140..112N Altcode: 1984A&A...140..112K Analysis of the longitudinal field strength in prominences obtained by measurements of Zeeman polarization in HeD3, Hα, and Hβ is presented. The measurements were performed with the spectrally scanning magnetograph installed at the 53 cm coronograph of the Kislovodsk high altitude station. The observations allow to correlate the values of the equivalent widths and those of the half widths with magnetographic data. No systematic dependence of field strengths on line widths is found. High field strengths persist for large Doppler shifts and low emissions. In the histogram showing the distribution of observed field strengths two peaks near B∥ ≅ 8 Gauss and B∥ ≅ 20 Gauss appear. The second peak corresponds to prominences mainly related to active regions for latitudes <±35°. A similar distribution is obtained from a set of data deduced from observation of the Hanle effect and corresponding to the same epoch. Title: Éclipse totale du soleil sur un territoire français d'Outre-mer, La Nouvelle-Calédonie, le 23 novembre 1984. Authors: Nitschelm, Ch.; Koutchmy, S. Bibcode: 1984LAstr..98..393N Altcode: No abstract at ADS Title: Photometric analysis of the June 11, 1983 solar corona Authors: Koutchmy, S.; Nitschelm, C. Bibcode: 1984A&A...138..161K Altcode: The solar corona was observed using different photo-cameras during the solar total eclipse on June 11, 1983 under good sky conditions. Pictures were used to perform a detailed morphological analysis of K-corona structures and an isophotometric analysis. Accurate values of the flattening index over 8 earth-radii are deduced. Title: Photographic colour photometry of the inner zodiacal light. Authors: Nikol'Skij, G. M.; Koutchmy, S.; Nesmyanovich, I. A. Bibcode: 1984ATsir1310....3N Altcode: No abstract at ADS Title: A Magnetograph Scanning Along the Whole Profile of the Line Authors: Nikolsky, G. M.; Kim, I. S.; Koutchmy, S.; Klepikov, V. Y.; Den, O. E.; Stepanov, A. I. Bibcode: 1984BSolD...9...88N Altcode: No abstract at ADS Title: The Widefield Coronograph for Observations of Coronal Transient Phenomena Authors: Nikolsky, G. M.; Koutchmy, S.; Fatianov, M. P. Bibcode: 1984BSolD...7...53N Altcode: No abstract at ADS Title: A magnetograph scanning along the whole profile of a line. Authors: Nikol'Skij, G. M.; Kim, N. S.; Koutchmy, S.; Klepikov, V. Yu.; den, O. E.; Stepanov, A. I. Bibcode: 1984BSolD1984...88N Altcode: A magnetograph recording the Zeeman-effect along the whole profile of a line with modulator of a LiNbO crystal and a Fabry-Perot interferometer is described. Title: Wide-field coronograph for observations of coronal transient phenomena. Authors: Nikol'Skij, G. M.; Koutchmy, S.; Fat'yanov, M. P. Bibcode: 1984BSolD1984...53N Altcode: A small Lyot coronograph is described. The results of the trial observations are discussed. Title: Periodic Comet Crommelin (1983n) Authors: Koutchmy, S.; Laques, P.; Lecacheux, J. Bibcode: 1983IAUC.3876....2K Altcode: The following three precise positions, obtained using a micro-channel device on the 2-m reflector at Pic du Midi, have been selected from 21 made on the same night by S. Koutchmy, P. Laques and J. Lecacheux. The positions are geocentric. 1983 UT R.A. (1950.0) Decl. Sept. 4.94350 20 07 26.92 +22 13 55.5 4.96399 20 07 25.44 +22 13 46.8 4.97875 20 07 24.52 +22 13 40.3 P/Crommelin has been selected by the International Halley Watch for a dry run to test out the procedures planned for observations of P/Halley. This test will mainly be during the week 1984 Mar. 25-31, at which time P/Crommelin will probably not be fainter than mag 17.5 (although it may not be all that much brighter). Title: Photospheric faculae-III-intensity, and magnetic field mapping of a typical element of the photospheric network Authors: Dara-Papamargaritis, H.; Koutchmy, S. Bibcode: 1983A&A...125..280D Altcode: The authors studied a typical quiet sun magnetic network element. Without introducing any correction, high spatial resolution spectra (=0arcsec.75) of two iron lines, simultaneous Ca II K and white-light slit-jaw pictures as well as spectroheliograms in H&alpha; and Mgb1 - 0.4 Å of a typical quiet region of the solar photosphere were analyzed in order: 1. to map the intensity, the velocity field and the magnetic field of a typical element of this region; 2. to study the underlying solar granulation, which seems to have a lower contrast; 3. to get from H&alpha; filtergrams the fibril structure around the rosette. Finally the authors give an estimate of the magnetic flux of a large region of the quiet sun. Title: Photometric analysis of sunspot umbral dots. III Spectrophotometry and preliminary model of a 2-component umbra Authors: Adjabshirzadeh, A.; Koutchmy, S. Bibcode: 1983A&A...122....1A Altcode: An empirical two-component model of the solar sunspot core based on the results of a two-dimensional photometrical analysis of quasi-statistical nature is presented. Spectrophotometrical line profile measurements of a highly selected observation are also used. The core of a sunspot is considered to be composed of a more or less homogeneous dark and cold background occupying 95 percent of the area of the core, with many tiny, very bright umbral dots embedded inside. The average radiative flux corresponding to the dots amounts to 37 pecent of the total flux of the core at 6000 A. With a calculated distribution of temperature and pressure of the proposed hydrostatic two-component model, it is demonstrated that the essential results given by the most recent homogeneous models can be easily retrieved when the hot and cold components of the present model are adequately mixed. Title: Exploration du ciel nocturne par photographie à partir de la station orbitale Saliout. Authors: Belmahdi, M.; Koutchmy, S. Bibcode: 1983LAstr..97..263B Altcode: The photography equipment and procedures, and examples of ionospheric and sky surveys performed from the Salyut space station during the visit by the French astronaut Chretien are described. Space-based viewing is unencumbered by skyglow from cities, the appearance of false sources near the terminator line, and interferences from the ionospheric F region. Standard astronomical and photographic equipment were used, including cross-hair sights, filters, objectives, and cassette loaded films. Once an object was sighted and the cameras pointed the entire station was placed into an inertial navigation mode to provide up to 40 sec stability for photography. Samples from studies of the ionospheric D region, the zodiacal cloud, and terrestrial limb are provided. Title: Short period coronal oscillations - Observation and interpretation Authors: Koutchmy, S.; Zhugzhda, Ia. D.; Locans, V. Bibcode: 1983A&A...120..185K Altcode: The result of an experiment devoted to the search of short period coronal waves using the green coronal line 5303 Å of Fe XIV are analyzed. After the subtraction of sky aureola fluctuations, 2 time series of measurements performed at a 40arcsec height over a faint facular area and small changing chromospheric features show power spectra with evidence of Doppler velocity oscillations with periods near 300 s, 80 s, and especially 43 s. However, no prominent intensity fluctuations appeared. The observed waves are considered as good candidates for being resonant Alfvén oscillations viewed at a low level through several legs of coronal arches, with a typical distance between feet being equal to the autocorrelation distance of the network and with foot-points inserted in the photosphere. A model of such an arch is subsequently computed and seems to fit quite well the observed periods and velocity amplitudes. In addition the energy flux balance is evaluated and the role of such waves in the heating mechanism of coronal arches is discussed. Title: Les éclipses totales et l'environnement solaire. Authors: Koutchmy, S. Bibcode: 1983LAstr..97..177K Altcode: The solar corona, which becomes highly visible during an eclipse, was first characterized as belonging to the sun in 1868, and the ionized state of the plasma was recognized in 1941. Coronal jets, i.e., particle streaming, were recognized in the 20th century. Modern era measurements include spectroscopic and radioastronomical data, gathered during the transit of the moon across the solar disk, with 'slices' taken of different sections of the solar image. Spectroscopy and monochromatic photometry have disclosed the limb structures of the chromosphere and coronal bursts. The ability to photograph the coronal features in totality during an eclipse is emphasized, as is photography of the stellar field around the sun. Comparisons are then made with photographs taken six months later. Additionaly, total field photography allows for examinations of the solar magnetic field lines and the plasma flow, which is the origin of the solar wind. Title: The electron density of faint prominences observed during the solar eclipse of July 31, 1981 Authors: Koutchmy, S.; Lebecq, C.; Stellmacher, G. Bibcode: 1983A&A...119..261K Altcode: Prominences visible on the narrow band filtergrams of the eclipsed Sun, July 3t, 1981, are analysed. The ratio of the Hβ line intensity to the continuum intensity at λ=6073 Å is used to derive the electron density ne as a function of electron temperature Te. The prominences present on that day were of low brightness: Eβ,max ≃ 0.2 104 [erg cm-2 s-1 sterad-1]. An electron density ne = 5.7 109 [cm-3] at Te = 10,000° is obtained, being typical for prominence edges. Title: Observation of global 160-min infrared (differential) intensity variation of the Sun Authors: Kotov, V. A.; Koutchmy, S.; Koutchmy, O. Bibcode: 1983SoPh...82...21K Altcode: 1983IAUCo..66...21K The method developed and the instrument designed for detecting variations of the solar limb darkening at the atmospheric transparency window of the solar opacity minimum region of λ 1.65 μ are described. This differential technique proved to be successful in rejecting undesirable low frequency noises due to the atmosphere and to the instrument. Analysis of observations made in 1977, 1978, and 1981 indicates the persistance of global fluctuations of the IR differential, center-to-limb intensity at the wellknown 160 min period with an average amplitude of about ± 2 × 10-4 in units of the `average Sun' intensity near 1.65 μm. Title: Relative distribution of colour of the solar corona on June 30, 1973. Authors: Nikol'Skij, G. M.; Koutchmy, S.; Nesmyanovich, I. A. Bibcode: 1983BSolD1983...67N Altcode: A more precise photometric analysis of a colour picture obtained during the June 30, 1973 total solar eclipse showed that the F-corona is slightly redder than the K-corona. Title: Relative Distribution of Color of the 1973JUN30 Solar Corona Authors: Nikolsky, G. M.; Koutchmy, S.; Nesmyanovich, I. A. Bibcode: 1983BSolD...4...67N Altcode: No abstract at ADS Title: Measurement of magnetic fields in solar prominences. Authors: Nikol'Skij, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I. Bibcode: 1983ppsf.conf...52N Altcode: No abstract at ADS Title: Night Sky from Salyut Authors: Koutchmy, S.; Nikolskii, G. M. Bibcode: 1983S&T....65...23K Altcode: The equipment and astronomical observations on the Salyuts 6 and 7 space stations are described. Noting that only one and a half hours of night sky viewing are available during each orbit, observations become either well-planned or innovative, with the presence of a crew in space an asset to taking advantage of opportunities as they arise. Human movement on board the stations is restricted while viewing is being performed. The station can be inertially stabilized for up to 40 sec. The results of photography of the F layer are presented, together with twilight photography and a reproduction of the inner zodiacal cloud. Other sessions have recorded the internal structure of noctiluminescent clouds, the 6300 A emissions of the F layer, and auroral structures. Title: Eclipse Totale de Soleil du 11 Juin 1983 Propositions D'observations Astrophysiques pour L'equipe de la S. a. F. Authors: Koutchmy, S. Bibcode: 1982O&T.....2....3K Altcode: No abstract at ADS Title: Measurements of the Magnetic Field in Solar Prominences with a Spectrally Scanning Magnetograph Authors: Nikolskii, G. M.; Kim, I. S.; Koutchmy, S. Bibcode: 1982SoPh...81...81N Altcode: We describe observations with a new magnetograph capable of recording the whole profile of emission lines in prominences. Two recordings are used simultaneously to study the Zeeman effect in circularly polarized light. The spectral scan is produced by the action of piezo ceramics of a Perot-Fabry inter ferometer combined with a narrow band interference filter. Title: Magnetic field in solar prominences measured with a new spectrally scanning magnetograph Authors: Kim, I. S.; Nikolsky, G. M.; Koutchmy, S.; Stellmacher, G. Bibcode: 1982A&A...114..347K Altcode: Observations of the longitudinal field strength in quiescent prominences obtained with the new redesigned spectrally scanning magnetograph installed in the Coude focus of the 53 cm coronograph of the Kislovodsk station are presented. With the instrument one can obtain magnetographic data as well as central intensities, equivalent widths, line widths, and shifts of the analyzed prominence lines. A first discussion, correlating magnetographic and spectroscopic data, is given Title: Large-scale Photographic Observations, Photometry, Colorimetry and Polarimetry of Cometary Tails Authors: Lamy, P. L.; Koutchmy, S. Bibcode: 1982ncgb.conf..243L Altcode: 1982gbhc.work..243L The use of large-scale photographic observations to characterize the dust tails of comets is discussed, with emphasis on plans being developed for observing Halley's Comet in 1986. The techniques used to investigate the geometric structure of the dust tail and its evolution (including detached structures, bursts, striae, and large-scale extensions), the integrated magnitude from blue to far IR, and color and polarization parameters are reviewed and illustrated with data and images from recent studies of other comets. The requirements for a network of identical cameras for Halley observations are examined: minimum 30-deg field of view, spectral coverage and filter separation, polarizers, calibration, color emulsions, and data-reduction schemes. Many of the problems inherent in ground observations programs could be avoided by using a space instrument such as the very-wide-field camera flown on the first Spacelab mission; this device is briefly described. Title: About the Foreshortening Effect on Sunspot Umbral Dots Authors: Adjabshirzadeh, A.; Koutchmy, S. Bibcode: 1982SoPh...75...71A Altcode: Using high-resolution pictures of the core of a unipolar sunspot observed with several cos θ values, we studied the center limb effect on the form of the bright umbral dots. The ratio of the apparent sizes in radial and tangential direction do not show the foreshortening effect typically observed in granular structures. Title: Study of the Interplanetary Dust at High Ecliptic Latitudes: Doppler-Fizeau Shifts Authors: Robley, R.; Bucher, A.; Koutchmy, S. Bibcode: 1982ASSL...96..255R Altcode: 1982spls.meet..255R No abstract at ADS Title: Soviet-French observations of the total solar eclipse. Authors: Koutchmy, S.; Nikol'Skij, G. M. Bibcode: 1982ZemVs...1...65K Altcode: No abstract at ADS Title: A Search of Short-Period Coronal Waves Authors: Koutchmy, Serge Bibcode: 1981SSRv...29..375K Altcode: In 1973, during the total solar eclipse, we flew an experiment aboard the Concorde supersonic airliner in order to investigate the possible presence of white-light coronal waves. Our experiment failed to detect any significant effects, so it became clear that such waves should be searched for by use of finer, i.e., spectroscopic methods. Title: An Opportunity for the Observations of Comets with Widefield Cameras Aboard the Salyut Space Station Authors: Lamy, P. L.; Koutchmy, S. Bibcode: 1981motc.conf..190L Altcode: No abstract at ADS Title: Soviet-French joint study of the solar corona. III - The structure and certain dynamic features of the corona of June 30, 1973 Authors: Vsekhsvyatsky, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Shtelmacher, G. Bibcode: 1981AZh....58..810V Altcode: The overall, as well as the detailed and fine, structure of the corona extending to approximately 3.0-4.0 solar radii is studied. The structure is compared with formations on the solar surface, and certain changes in the structure are traced for periods of 80-90 min. The structure of the rays in the outer corona is studied out to 12 solar radii by reproducing computer-enhanced negatives from a short-focus camera. New phenomena are detected, namely, quasi-continuous dynamic disturbances occurring in and near coronal holes (rifts); they appear to be hydromagnetic in the same way as coronal transients. Data are obtained on the fine-filament structure of the corona, on the relationship between this structure and the magnetic fields and current layers, on the spatial arrangement of large helmet-like rays, on the width of the visibility zone, and on the relationship between the overall structure of the corona and the N-S asymmetry of the activity of the 20th cycle. Title: Joint Soviet - French Investigations of the Solar Corona - Part Three - Structure and Some Dynamic Features of the Solar Corona of 1973JUN30 Authors: Vsekhsvyatskii, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Stellmacher, G. Bibcode: 1981SvA....25..463V Altcode: No abstract at ADS Title: Photometric Analysis of the Sunspot Umbral Dots - Part Two - Size Shape and Temperature Authors: Koutchmy, S.; Adjabshirzadeh, A. Bibcode: 1981A&A....99..111K Altcode: We use several selected very high resolution pictures obtained at 4680 Å and 6000 Å at the prime focus of the Sacramento Peak Vacuum Telescope to study the sizes, shape, and typical brightness temperatures of the umbral bright dots observed well inside the core of a unipolar sunspot. A two-dimensional photometric analysis was performed. Results are consistent with the picture of a core composed of a cool background atmosphere at a constant level with many extremely bright embedded dots. The average diameter of dots is 190 km and their brightness temperature, 6185 °K. Sizes of dots as well as their rounded shape are approximately constant whatever the values of cos θ are; conversely, their intensities show a decrease with increasingly center limb distances. Title: Sensitometry during Orbital Missions Aboard the Salyut Space Station Authors: Koutchmy, S. Bibcode: 1981asph.conf...11K Altcode: No abstract at ADS Title: Joint Soviet / French Investigations of the Solar Corona - Part Two - Photometry of the Solar Corona of 1973JUN30 Authors: Vsekhsvyatskii, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Stellmacher, G. Bibcode: 1981SvA....25..211V Altcode: No abstract at ADS Title: Measurement of the Continuum Background of Solar Prominences Using a Large Coronagraph Authors: Koutchmy, S.; Nikolskij, G. M. Bibcode: 1981PAZh....7..183K Altcode: No abstract at ADS Title: Joint Soviet-French studies of the solar corona. II - Photometry of the solar corona on June 30, 1973 Authors: Vsekhsvyatsky, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Shtelmacher, G. Bibcode: 1981AZh....58..376V Altcode: Results are presented of a study of negatives obtained on June 30, 1973 during the total solar eclipse in Africa; the study was part of a joint Soviet-French experiment on white corona dynamics, carried out by expeditions of Kiev University (Atar, Mauritania) and the Paris Astrophysical Institute (Moussoro, Chad). The distribution of total corona brightness up to 4.5 solar radii and its K and F corona components for east and north directions were found on the basis of novel methods of photometry and colorimetry using star images up to 8.5m as the photometry standards. Neither the color effect nor flattening is found in the inner part (less than 2.5 solar radii) of the F corona. Integral corona brightness in the standard zone of 1.03-6.00 solar radii was found to be 0.64 x 10 to the -6th solar-E. Title: Infrared Imaging and Speckle Observations with a TV Camera Authors: Lamy, P.; Koutchmy, S. Bibcode: 1981Msngr..23....5L Altcode: The lack of suitable two-dimensional detectors has been a major problem for infrared imaging in astronomy, and most results so far have been obtained by scanning the object with a single detector (e. g., Terrile and Westphal,lcarus, 30, 730, 1977). The relative merit of both techniques was thoroughly investigated by Hall (Applied Optics, 10, 838, 1971) who concluded that, below about 2.5 ~lm, camera tubes should be preferred to scanners. Besides, sufficiently long times required by the scanning technique are not always available for some astronomical applications. These considerations led us to acquire a standard television camera equipped with an infrared vidicon tube N156 manufactured by Hamamatsu Co. (Japan). Title: Measurements of the Background Continuum of Prominences with a Large Coronagraph Authors: Koutchmy, S.; Nikolskii, G. M. Bibcode: 1981SvAL....7..102K Altcode: No abstract at ADS Title: On TV Observations of Polarization of Green Coronal Line at the Eclipse Time of 1981JUL31 Authors: Popov, O. S.; Ivchenko, V. N.; Lapchuk, V. P.; Milinevsky, G. P.; Osminkina, K. I.; Koutchmy, S.; Begot, J.; Lebeq, C.; Stellmacher, G. Bibcode: 1981ATsir1202....1P Altcode: 1981ATsir1202Q...1P No abstract at ADS Title: Spectrophotométrie de fond du ciel et dynamique du nuage zodiacal Authors: Koutchmy, S.; Bucher, A.; Robley, R. Bibcode: 1981hrse.conf...39K Altcode: No abstract at ADS Title: Detection of 160 min solar intensity variations: sampling effects. Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V. A. Bibcode: 1980A&A....90..372K Altcode: The theory that the 2 h 40 min period in the Crimean and Stanford global solar velocity oscillation measurements may have resulted partly by 1-day sampling is verified using the IR center-limb intensity variations measurements. It was shown that (1) the power spectrum of these data has a peak near the 2 h 40 min period, and (2) the power spectra of the series with the observing windows 'filled' with a constant do not manifest a significant peak at the 9th harmonic of the day. It was concluded that the analysis of the really observed data is not biased by the influence of data windows and 1-day sampling regularity of observations. Title: Photometric analysis of the sunspot umbral dots. I - Dynamical and structural behaviour Authors: Adjabshirzadeh, A.; Koutchmy, S. Bibcode: 1980A&A....89...88A Altcode: A sequence of selected high resolution white light pictures of a unipolar sunspot was studied in order to measure the main characteristics of umbral dots size, contrast value, and lifetime. Using a statistical analysis, the behavior of a typical dot was deduced. The large effect of smearing on the values of umbral intensities and sizes of umbral dots is discussed. This study considers the computed values of radiative flux, as obtained from measured sizes and contrasts; this parameter is presumably free of instrumental effects. An analytic function is proposed to describe the time variation of some of the umbral dots. Title: The solar granulation. I - Two dimensional power-spectrum analysis using optical data processing methods Authors: Koutchmy, S.; Legait, A. Bibcode: 1980A&A....88..345K Altcode: Optical data processing methods are used to analyze a good time sequence of selected high resolution solar granulation pictures obtained at the Vacuum solar telescope of Sacramento Peak Observatory. Several two-dimensional power spectra were composited and averaged by rotation to deduce a statistically significant distribution. No regularities appear on the deduced spectra. The speckles of partly instrumental origin seen on individual two-dimensional power spectra are stable, their characteristic life time being up to 7 min, indicating a similar lifetime for solar granulation. Title: The effect of the equation of time on the 160-min solar oscillation Authors: Kozov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T. Bibcode: 1980PAZh....6..421K Altcode: If the Crimean and Stanford experiments to measure the sun's pulsations of 160.010 m period (approximately 1/9 day) have actually recorded not a solar oscillation but the ninth harmonic of a diurnal wave in the terrestrial atmosphere, then the power spectrum and the exact value of the period should depend on the equation of time (the difference between true solar time and mean solar time). However, analysis of the Crimean Doppler-shift measurements for 1974-1979 reveals no such relationship, thereby supporting a solar interpretation of the 160.010 m period. Title: The Effect of the Equation of Time on the 160-MINUTE Solar 0SCILLATION Authors: Kotov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T. Bibcode: 1980SvAL....6..233K Altcode: No abstract at ADS Title: Two-Dimensional Photographic Photometry of the Zodiacal Light from Spatial Observations Authors: Lamy, P. L.; Llebaria, A.; Koutchmy, S. Bibcode: 1980IAUS...90...37L Altcode: No abstract at ADS Title: 2-D observations of IR-stellar speckles. Authors: Lamy, P.; Koutchmy, S. Bibcode: 1979JOpt...10..331L Altcode: 1979JOp....10..331L The first observations of speckle images of Alpha Orionis as obtained at the Cassegrain focus of the 193-cm Telescope of the Haute Provence Observatory using an IR-TV camera are discussed. The specific nature of the 2-micron images is outlined. Title: Astronomical applications of infrared television imaging. Authors: Lamy, P. L.; Nguyen-Trong, T.; Adjabschirzadeh, A.; Koutchmy, S. Bibcode: 1979A&A....77..257L Altcode: Infrared imaging between 1 and 2.4 microns was realized with a television camera operated at the conventional video rate. A M2 star of visual magnitude 5.6 was detected at 1.2 and 1.6 microns. Alpha Ori was further observed at 2 microns and the corresponding smearing function was found to improve with increasing wavelength. The image structure (speckle) of Alpha Ori was visualized in the infrared and is briefly characterized as compared to the visible. Solar observations at 1.6 microns included direct imagery of sunspots and simultaneous spectrography of the photosphere and sunspot umbra. The Zeeman splitting of the 1.5648 microns Fe I line was observed and measurements are shown to be possible on processed CRT pictures. Title: Comet West 1975n. I. Observations near and after perihelion passage. Authors: Koutchmy, S.; Coupiac, P.; Elmore, D.; Lamy, P.; Sevre, F. Bibcode: 1979A&A....72...45K Altcode: Photographic observations of Comet West 1975n from a high altitude site are reported. A small value of the absolute magnitude of the Comet 1.5 d after perihelion passage is deduced. Morphological characteristics of the strongly structured dust tail are obtained, using a statistical analysis based on the optical data processing of a transparency. The deduced two-dimensional power spectrum is considered. The temporal behavior of the main features of the tail is discussed using several selected pictures. Title: Comet West 1975n part II: study of the striated tail. Authors: Lamy, P. L.; Koutchmy, S. Bibcode: 1979A&A....72...50L Altcode: The dynamical evolution of the striae in the tails of comet West 1975n is investigated. A synchrone-syndyne analysis of the overall tail structure is attempted, but it is found that the classical synchrone-syndyne description does not apply to the dynamical evolution of the striae. A subsequent examination of the main properties of the stria structure strongly suggests that all striae within a given tail appear to originate from a synchronic edge. A scenario for the formation of striae is proposed, according to which the bulk of the dust constituting a tail is released at or around perihelion and subsequently swept out under the influence of some unknown interaction that organizes the dust into narrow streaks, or striae. It is concluded that the unknown interaction involves the solar wind and a convected magnetic field. Title: Salyut-6: a new look at the ionosphere. Authors: Koutchmy, S. Bibcode: 1979Rech...10...63K Altcode: No abstract at ADS Title: Observatoires en URSS: Description de quelques instruments nouveaux Authors: Koutchmy, S. Bibcode: 1978LAstr..92..433K Altcode: No abstract at ADS Title: Photometrical analysis of the June 30, 1973 solar corona. Authors: Koutchmy, S.; Stellmacher, G.; Koutchmy, O.; Dzubenko, N. I.; Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Vsekhsviatskii, S. K.; Lamy, P. Bibcode: 1978A&A....69...35K Altcode: In order to deduce reliable values of the K and F coronal, a method of photographic photometry has been applied to study compensated high-resolution pictures obtained during the June 30, 1973, solar total eclipse, including a color one. The correctly exposed images of calibration stars are used to obtain intensities in units of the mean brightness of the sun. An account is made, in both the blue and the red spectral ranges, for the sky background as well as for the coronal aureola effects. The N-polar and E-equatorial regions are shown to be relatively homogeneous; their intensities are especially studied in the radial direction and compared with published values of the K and F coronae. No flattening and no color effect are found in the inner part (distance less than 2.5 solar radii) of the F corona. Title: Bright points in sunspot umbrae: morphology, intensities. Authors: Adjabshirzadeh, A.; Koutchmy, S. Bibcode: 1978CRASB.286..335A Altcode: The bright point distribution in a sunspot umbra was determined by applying precise photographic photometry to three photographic plates obtained at time intervals of several minutes. The size and intensity distribution along two orthogonal axes is examined. The distance between bright points seems to be about 0.40 arcsec or about 300 km, but if a correction is applied, the distance might be approximately 40 km. While the asymmetric distribution of the bright points seems to indicate that the points have an elongated form, it is suggested that the elongations are composed of a series of more or less circular points which lie close together. Title: Propagating inhomogeneities in the dust tail of comet West 1975 Authors: Koutchmy, S.; Lamy, P. Bibcode: 1978Natur.273..522K Altcode: COMET West has displayed some remarkable properties. Sekanina1 has studied the multiple splitting of its nucleus and also discussed the strange structure of its dust tail. This tail is characterised by a system of bright bands which do not correspond to the true synchronous band2 and which are shown by very few comets. We call these striae (striated tail) and to study them we have examined numerous original and duplicate pictures, and selected four observations (Table 1) which reveal that the morphology was relatively well conserved during the evolution of the dust tail over a period of more than 4 days. We have identified three striae (Fig. 1) which seem to propagate in space while retaining their basic form. This phenomenon is not unusual in plasmas, such as gas tails of comets3 or streamers in the solar K-corona4,5. However, this is apparently the first time that it has been observed in dust `clouds'. These striae, which we describe here, are made of dust grains which can be readily demonstrated by the wide-field colour photographs made by comet observers: the gas tail (type I) appears distinctly blue because of CN emission and is directly in the anti-solar direction as well as being well separated from the large dust tail (type II) which has a neutral colour. Title: Photospheric faculae. II. Line profiles and magnetic field in the bright network of the quiet sun. Authors: Koutchmy, S.; Stellmacher, G. Bibcode: 1978A&A....67...93K Altcode: Smnmary. Spatially high resolution spectra ( 0"75) of the three iron lines. Fe 5576 A (non split), Fe 6301.5 A and Fe 6302.5 A (triplet) observed in maguetic regions (network) of the quiet Sun, were analysed. For the model computations, recent values of filigree continuum contrast and diameter were used [1f/1P -18, 4) -0"24 (174 km), =6000 A]. High values of the maguetic field strength (10001500 Gauss) are found for the quiet network regions. A fit of the observed profiles with the calculated proffles can be obtained only when a strong maguetic field is also assumed in the intergranular regions that surround the filigrees; the dimension of the magnetic field patch is found to be structured and larger than that of the proper line gap (ffligree). For the model calculations, a good fit is obtained when the filigree width r is assumed to increase with height h as r =0.12 h+87 [km]. Key words: Sun - photo sphere - filigrees - facularpoints - gap-profiles - concentrated magnetic fields Title: Workshop on cometary missions. ESOC Darmstadt, 17 - 19 April 1978. Chairmen's summaries and extended abstracts of invited contributions. Authors: Arpigny, C.; Bertaux, J. L.; Bodechtel, J.; Dalmann, B. -K.; Fechtig, H.; Festou, M.; Giese, R. H.; Grün, E.; Haser, L.; Hughes, D. W.; Ip, W. -H.; Jockers, K.; Keller, H. U.; Keppler, E.; Kissel, J.; Koutchmy, S.; Krankowsky, D.; Lämmerzahl, P.; Lamy, P. L.; Levasseur-Regourd, A. -C.; Lukoshhus, D.; Malaise, D.; Mariani, F.; Michel, K. W.; Neukum, G.; Orfei, R.; Rosenbauer, H.; Röser, S.; Schlude, F.; Schmidt, H. U.; Schubart, J.; Schwehm, G. H.; Sieber, A.; Wänke, H.; Wallis, M. K.; Zerull, R. H. Bibcode: 1978wocm.book.....A Altcode: No abstract at ADS Title: Super Granulation in the Deep Photosphere Authors: Koutchmy, S. Bibcode: 1978pfsl.conf..155K Altcode: 1978ESPM....2..155K No abstract at ADS Title: Practical work on colour emulsions using filtered duplicates Authors: Koutchmy, S. Bibcode: 1978mtap.conf..225K Altcode: No abstract at ADS Title: Photospheric faculae: the contrasts at the center of the solar disk using filigree pictures. Authors: Koutchmy, S. Bibcode: 1977A&A....61..397K Altcode: Summary. Fine structure of photo spheric faculae embedded in intergranular lanes has been observed at the continuum level. 2-dimensional restoration of the best filigree pictures obtained by R. B. Dunn was tentatively achieved, using a Quasi-conventional method of deconvolution and assuming largest values of the modulation transfer function. The restored pictures show a typical filigree contrast of 100 %, but we think that this limited restoration gives only a lower limit to the actual constrast. Key words: solar filigree - faculae - intergranular lanes - granulation two-dimensional deconvolution - image processing - restoration Title: Etude polarimétrique de la couronne solaire observe a l'èclipse totale du 30 juin 1973 à l'aide d'un filtre neutre radial. Authors: Koutchmy, S.; Picat, J. P.; Dantel, M. Bibcode: 1977A&A....59..349K Altcode: Photographs of the white-light solar corona were obtained during the total solar eclipse of June 30, 1973 in two orthogonal components of polarization. The total intensity and fraction of polarization of the white-light corona were determined by means of a photographic method and also by a numerical method of reduction of the plates with a computer-controlled microdensitometer. The simple and quick photographic method provided results which were in very good agreement with the numerical ones. A procedure is described which permits the total intensity and fraction of polarization of the K corona alone to be computed and mapped, and a model for the transpolar coronal hole is deduced. Title: Measurements of the solar limb-darkening in the 1 - 4 µm range. Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V. Bibcode: 1977A&A....59..189K Altcode: Radial scans in selected spectral regions near the opacity minimum, in both equatorial and polar directions, have been performed for the purpose of obtaining improved values for the limb darkening of the very undisturbed quiet solar atmosphere. Equipment and correction procedures are described. The new data are compared with earlier values, and the HSRA model is found to be inadequate for predicting values near the opacity minimum. The data are more in accord with the new model M of Vernazza et al. (1976) and also with the BCA model. No pole-equator difference of limb darkening due to the presence of faint faculae was found. Title: Study of the June 30, 1973 trans-polar coronal hole. Authors: Koutchmy, S. Bibcode: 1977SoPh...51..399K Altcode: Radially and tangentially polarized pictures of the solar corona obtained near 4500 Å during the 30 June, 1973 solar total eclipse have been used to derive a model of a trans-polar coronal hole. The hole is identified by using OSO-7 EUV spectroheliograms. The line of sight coincides with the privileged plan of the hole over the N-polar region. A new method of absolute calibration is used. The Saito (1970) method is applied to determine the electron densities. Extrapolated values of densities down to the surface are lower than have ever been observed although derived hydrostatic temperatures are certainly not: Ne × 107 cm−3 and T = 2 × 106 K. The morphological peculiarities of polar regions are considered. Title: The Contrast of Solar Filigrees Authors: Koutchmy, S.; Stellmacher, G. Bibcode: 1977MitAG..42..142K Altcode: No abstract at ADS Title: Solar Corona Authors: Koutchmy, S. Bibcode: 1977ASSL...69...39K Altcode: 1977igss.conf...39K White-Light Corona Ellipticity or Flattening Coronal Streamers Polar Plumes Coronal Cavity Rifts Coronal Condensation and Enhancement E-Corona or Emission Line Corona Coronal Loops EUV and X-Ray Corona Magnetic Arcades Coronal Holes Coronal Bright Points Coronal Events or Coronal Transients T-Corona Lyot-Coronagraph Externally Occulted Coronagraph Title: Photometric study of chromospheric and coronal spikes observed during the total solar eclipse of 30 June 1973. Authors: Koutchmy, S.; Stellmacher, G. Bibcode: 1976SoPh...49..253K Altcode: A photometric and colorimetric analysis of a color picture of the very inner solar corona, near the South pole region, is performed. Dimensions and average electron densities of both chromospheric and very fine resolved coronal spikes are deduced. For the coronal spike a half width of 1″.67 is measured, the estimate of electron density yields ne = 1010 cm−3. Some conclusions are attempted on the light of a simultaneously observed spectrum of the same region which appeared to be a "disappearing coronal hole." The observations seem to support the concept of a "striated" corona. Title: Comet West (1975n) Authors: Sinvhal, S. D.; Babu, G.; Ketelsen, D. A.; Neff, J. S.; Young, J.; Bortle, J.; Sekanina, Z.; Farrell, J. A.; Willmarth, D.; Elmore, D.; Koutchmy, S.; Mayo, M. J.; Truxton, J.; Apeldoorn, B.; Cosmovici, C.; Geyer, E. H.; Hoffmann, M.; Boyd, R.; O'Meara, S. Bibcode: 1976IAUC.2924....3S Altcode: S. D. Sinvhal, Uttar Pradesh State Observatory, reports that observations by G. Babu on Mar. 6.00 UT showed very strong Na emission, strong Swan bands and detectable CN 3883 A and 4214 A and C3 4050 A; on Mar. 7.00 all emissions except the Swan bands had considerably weakened. D. A. Ketelsen and J. S. Neff, University of Iowa, report that observations of the nuclear region (resolution 16 A) on Mar. 7.5 showed a strong continuum, strong emission features due to CN and C2 and rather weaker emissions due to Na and C3. J. Young, Table Mountain Observatory, reports the following visual tail lengths: Mar. 2.58 UT, > 10o; 6.54, 25o; 7.55; 28o; 8.55, 30o. J. Bortle, Brooks Observatory, reports the following observations of tail structure: Mar. 7.41 UT, 5o.5 long in p.a. 295o (a pair of gas tails); 8o.5 in 305o and 11o.5 in 310o and 19o in 330o (dust); 8.40, 8o.5 in 298o (gas), 11o in 307o and 16o in 310o and 25o in 320o (dust). Corrigendum: on IAUC 2919, the p.a. for the Feb. 29.47 observation should read 340o. Z. Sekanina, Center for Astrophysics, comments on photographic observations of the tail: "On photographs (4.5-cm f/4 camera, Royal Pan emulsion) taken on Mar. 5.51 and 6.50 UT J. A. Farrell, Los Alamos, New Mexico, noted a broad, dust tail composed of a number of 'synchronic bands', similar to those observed in comet 1957 V; the breadth of the tail had increased by the latter date, while the bands showed a systematic translational motion of about 1o.6 per day and rotated at about 13o per day relative to the faint plasma tail; Farrell also detected two streamers superimposed on the dust tail, one of them essentially coinciding with its southern border. On a print (f = 135 mm camera, IIIa-J emulsion) obtained on Mar. 5.50 UT by D. Willmarth, Mount Hopkins Observatory, I find the main body of the tail to be between p.a. 310o and 357o, but a fainter glow can also be detected in the north-northeast, apparently terminating in p.a. 40o; the bright section of the dust tail consists of as many as 20 'synchronic bands', those nearest the nucleus being directed toward p.a. 320o, the farthest ones toward p.a. 330o; the most distant bands reach to at least 19o from the nucleus, but traces of the dust tail extend out to some 25o. This bright section of the dust tail consists of postperihelion particle emissions, while the faint northeast section, which can be followed for a few degrees, is made up of somewhat heavier particles emitted during the week before perihelion. Willmarth's print also shows a plasma tail > 15o long in the form of a 15o sector centered on p.a. 300o." D. Elmore and S. Koutchmy, Sacramento Peak Observatory, report that daylight photographic measurements on Feb. 26.81 UT at an effective wavelength of 8750 A (passband 800 A) give an integrated magnitude of -3.65 +/- 0.40 (30' field). Selected recent total visual magnitude estimates: Mar. 2.56 UT, 0 (M. J. Mayo and J. Truxton, Agoura, California, 7 x 50 binoculars); 3.23, 0 to -0.5 (B. Apeldoorn et al., Hoeven, The Netherlands, naked eye); 4.2, 0 (C. Cosmovici, Lecce, Italy, naked eye); 5.55, < 1.0 (Mayo and Truxton); 6.56, 1.2 (Mayo and Truxton); 7.41, 1.3 (Bortle, 10 x 50 binoculars); 7.56, 1.4 (Mayo and Truxton); 8.40, 1.8 (Bortle). Visual observations of secondary nuclei: Mar. 5.23 UT, separation 3", p.a. 50o, magnitude difference 0.5 (E. H. Geyer and M. Hoffmann, Hoher List Observatory, 36-cm refractor, 250 x); 7.46, -, 120o, 0 (R. Boyd, Miami, Florida, 20-cm reflector, 210 x); 7.55, 4" 1 (Young, 61-cm reflector, 500 x); 8.40, < 5", 340o, 1 (Bortle, 32-cm reflector, 100 x); 8.42, 1".5, 350o, 0.5 (S. O'Meara, Harvard Observatory, 23-cm refractor, 300 x); 8.55, 2", -, - (Young). Title: JointSoviet-French studies of the solar corona. I. Structural properties and photometry of solar corona of July 10, 1972 Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.; Popov, O. S.; Koutchmy, S. Bibcode: 1976SvA....19..477V Altcode: No abstract at ADS Title: Study of the Anti-Tail of Comet Kohoutek from an Observation on 17 January 1974 Authors: Lamy, Ph. L.; Koutchmy, S. Bibcode: 1976LNP....48..343L Altcode: 1976IAUCo..31..343L As part of our program of observation of Comet Kohoutek at Pic-du-Midi observatory, we obtained, on January 17.8 UT, 1974 a photograph in polarized light showing dramatically the (dust) antitail extending for almost 1° from the Comet's head (reported in Sky and Telescope, June 1974); indeed the comet is visible in polarized light further away than in total light as noticed by Weinberg and Beeson (IAU Colloquium No. 25, 1974) for Comet Ikeya-Seki. A photometric and polarimetric study was performed (Bücher, A., Robley, R., and Koutchmy, S., 1975, Astron. Astrophys. 39, 289) showing that the anti-tail is strongly polarized (up to 50 %). These large degrees of polarization are of the same order of magnitude as those reported for the tail of Comet Ikeya-Seki by Matjagin Sabitov and Kharitonov (1967, Astron. Zh. 44, 1075) and by Weinberg and Beeson (op. cit.). As discussed by these latter authors, particle alignment is precluded as a significant contributor to polarization in the tail of comets. Polarization by large spheres as obtained from the Fresnel reflection coefficients applies only in the case of perfect surface, a circumstance very unlikely in interplanetary space; the scattering is in fact controlled by the surface microstructures (Van de Hulst, private communication). Therefore we hypothesized that submicronic grains should play an important role in the anti-tail. The classical method of Finson and Probstein (1968, Astrophys. J. 154, 327, 353) was used to draw the sky plane view of the syndynes for the day of observation. Since the ratio β of the radiation pressure force to the gravitational attraction is proportional to the third power of the grains' radius s for ≲z 0.1 μ, submicronic grains with typical radii of 0.02 μ may indeed be present in the anti-tail and provide a straight-forward explanation of the observed polarization. This size is of the same order of magnitude as that inferred for interstellar grains which may well be embedded in the comet's nucleus as well as meteorites for which there exists good evidence. Our conclusion does not rule out the presence of millimeter-size grains as proposed by Sekanina and Gary and O'Dell in their preliminary investigations (1974, Icarus 23, 502, 519) which did not take into account the polarimetric result; such grains may well coexist with the submicronic ones. Finally, the line of maximum intensity is close to a synchrone corresponding to a time of emission 100 days before perihelion passage. This supports the synchronic formation of anomalous tails and possibly of tails as proposed by Vsekhsvyatsky (1932, Astron. Zh. 9, 166). Title: JointSoviet-French studies of the solar corona. I. Structural properties and photometry of solar corona of July 10, 1972 Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.; Popov, O. S.; Koutchmy, S. Bibcode: 1975AZh....52..785V Altcode: No abstract at ADS Title: Study of the Inner Satellites of Saturn by Photographic Photometry Authors: Koutchmy, S.; Lamy, P. L. Bibcode: 1975Icar...25..459K Altcode: Good photographs of Saturn and its five inner satellites were obtained on January 2, 1974 with the 105 cm telescope at Pic du Midi Observatory with exposure times of 45 sec. The spread function is constant over the field, and isotropic. The true photometric profiles of the satellites are obtained after deriving a model for the stray light coming from the rings. The magnitudes, computed by integration, are in good agreement with published values except for Mimas, which is nearly one magnitude fainter then previously believed. Title: Saturn's Rings: A Photometric Study of Ring C Authors: Koutchmy, S. Bibcode: 1975Icar...25..131K Altcode: A simple computational procedure is proposed for determining the true photometric profile of ring C using the spread function obtained from the satellite Dione and also slightly overexposed photographs of Saturn. No trace of a faint additional ring between ring C and the disk was found. The decreasing part, toward the planet, of the recorded photometric profile of ring C exhibits a slight depression tentatively attributed to a new division. Title: L'étude de la couronne blanche à bord de Concorde 001 au cours de l'éclipse totale de Soleil du 30 juin 1973 Authors: Koutchmy, S. Bibcode: 1975LAstr..89..149K Altcode: Preliminary preparations, essential results, and a narrative account of the high-resolution coronal photography experiment conducted aboard the Concorde 001 during the recent African solar eclipse are presented. Scientific and other objectives of the study are considered, the camera used is described, and the performance of the camera is evaluated. Title: Dynamic processes in the solar corona of June 30, 1973 Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.; Rubo, G. A.; Koutchmy, S. Bibcode: 1975DoSSR.218..787V Altcode: High-resolution photographs of the solar corona obtained during a solar eclipse at two widely spaced points (time difference of 80 to 90 min between the photographs) are analyzed. It is shown that following processes can occur during one hour in a solar corona whose global structural characteristics are maintained during this period: the formation and decay (or pronounced brightness variations) of such medium-scale formations as polar rays, coronal jets, etc.; formation and decay of distinct interfaces in the coronal structure; pronounced shifts of coronal structures at speeds of several kilometers per second; and separation of solar plasma concentrations, and their ejection from the sun. Title: Photometric, Colorimetric and Polarimetric Study of Comet Kohoutek 1973F, on January 17 and 18, 1974 Authors: Bucher, A.; Robley, R.; Koutchmy, S. Bibcode: 1975A&A....39..289B Altcode: Summary. The photoelectric and photographic observations performed on 17 and 18 January 1974 of the external parts of the comet Kohoutek (1973 f) show that the color of the tail is much the same as the solar color, and that the degree of polarization in the tail and anti-tail is very strong. Observations of the anti-tail suggest similarity in the properties with the zodiacal cloud dust. Key words: comet Kohoutek 1973 F zodiacal light - photometry - polarimetry colorimetry interplanetary dust Title: Investigation of dynamical processes in the solar corona on 30th June, 1973. Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.; Rubo, G. A.; Koutchmy, S. Bibcode: 1974DoSSR.218..787V Altcode: High-resolution photographs of the solar corona obtained during a solar eclipse at two widely spaced points (time difference of 80 to 90 min between the photographs) are analyzed. It is shown that following processes can occur during one hour in a solar corona whose global structural characteristics are maintained during this period: the formation and decay (or pronounced brightness variations) of such medium-scale formations as polar rays, coronal jets, etc.; formation and decay of distinct interfaces in the coronal structure; pronounced shifts of coronal structures at speeds of several kilometers per second; and separation of solar plasma concentrations, and their ejection from the sun. Title: Study of low dispersion eclipse spectra: observation of weak low excitation emission lines in the corona. Authors: Stellmacher, G.; Koutchmy, S. Bibcode: 1974A&A....35...43S Altcode: Summary. A spectroscopic experiment, set up to observe simultaneously the electronic, emission line and F-corona, near the equator between 0.1 and 0.8 R0 above the sun's limb, was carried out successfully during the total solar eclipse on June 30, 1973 in the Republic of Tchad. The low excitation line emission in Ca+, H and K, H , H , H is observed superimposed over the entire spectrum, including the lunar background. No radial dependence is observed for the equivalent width of these lines. The emission is interpreted in terms of double scattered light of chromospheric origin in the earth's atmosphere. The color dependence of the double scattered light is correctly reproduced by a quasi quantitative model confirming the parasitic origin of these lines. Key words: sun - total solar eclipse chromospheric emission lines double scattered parasitic light atmospheric optics Title: Infrared Photometry of the Outer Corona. Authors: Lamy, Ph. L.; Koutchmy, S. Bibcode: 1974BAAS....6..311L Altcode: No abstract at ADS Title: Observations photographiques de la comète Kohoutek Authors: Koutchmy, S. Bibcode: 1974LAstr..88..172K Altcode: No abstract at ADS Title: Photométrie photographique de la couronne solaire. Observée au cours de l'éclipse totale du 10 juillet 1972 Authors: Koutchmy, S.; Dzubenko, N. I.; Nesmjanovich, A. T.; Vsekhsvjatsky, S. K. Bibcode: 1974SoPh...35..369K Altcode: No abstract at ADS Title: The coronal aureola in the time of total solar eclipse Authors: Koutchmy, O.; Koutchmy, S. Bibcode: 1974A&AS...13..295K Altcode: We propose a computational method allowing to obtain the intensity of the coronal aureola from the measures of the solar aureola. The method is applied to 2 very different observations performed at the solar eclipses at Sept. 22, 1968 and March 7, 1970. In addition, a scattering function is given for some typical cases observed (clear sky) showing a large variety in values. We suggest to use this type of function in order to describe the scattered light superimposed on the lunar earthshine and the sky background. For good observing conditions, we show that the coronal aureola is everywhere one order of magnitude less than the but becomes higher than the minimum electronic corona, for r >2,5. When the sky background is important, especially because of the low value of the eclipse magnitude, the intensity of coronal aureola may be compared to the intensity. Key words: solar corona - total solar eclipse - aureola effect - coronal model Title: Sur les premiers signes de la reprise de l'activité solaire. Authors: Koutchmy, S.; Bareau, C.; Stellmacher, G. Bibcode: 1974CRASB.278..873K Altcode: No abstract at ADS Title: Comet Kohoutek, 1973f. Authors: Koutchmy, S.; Chernykh, N. S.; Kastel', G. R.; Pavlenko, P. P. Bibcode: 1974KomTs.169.....K Altcode: No abstract at ADS Title: On the Observation of the F Corona in the Vicinity of the Solar Limb Authors: Koutchmy, S.; Magnant, F. Bibcode: 1973ApJ...186..671K Altcode: Theoretical calculations led Calbert and Beard to predict a much lower intensity of the F corona near the solar limb than the one generally accepted. We show that this does not agree with recent observations, especially airborne ones obtained far above the lower atmosphere. The measurements made on the ground during the eclipse of 1970 March 7 confirm the classical models. We suggest that new observations should be made in order to allow a choice between the apparently inconsistent interpretations of the measurements concerning the external F corona. Subject heading: corona, solar Title: Rapid Variations Observed during the Total Eclipse of the Sun on June 30, 1973 Authors: Koutchmy, S.; Fagot, J. Bibcode: 1973Natur.246..414K Altcode: FOR nearly a century the solar corona has been considered responsible for the interplanetary corpuscular radiation and in particular large streamers have been thought to be the main source of this radiation. Title: French Eclipse Studies Authors: Koutchmy, S. Bibcode: 1973S&T....46..215K Altcode: No abstract at ADS Title: Etude photometrique d'un Renforcement Diffus observé dans la Lumière Zodiacale, à une distance de 100 Rsun du Soleil Authors: Banos, C.; Koutchmy, S. Bibcode: 1973Icar...20...32B Altcode: A photograph of the zodiacal light obtained at the Pic du Midi Observatory is studied in order to measure, in absolute units, the brightness of the reinforcement, observed 15° above the ecliptic plan and in a distance of 100R⊙ from the Sun. The obtained brightnesses are compared to the brightness of the zodiacal light given by other authors for the elongations ɛ ɛ [23°, 40°]. The calibration of the image was made using the stars in the field of the image and isophotes corrected for extinction were obtained, by the method of isodensities. A discussion of the obtained results is made and the origin of the reinforcement is investigated. The mass evaluation of the interplanetary particles producing this reinforcement has been estimated and permits to us to conclude that it may be due to particles evaporated from the circumsolar region. The mechanism of transfer of momentum to the particles in orbit around the Sun by a convecting ma magnetic field is not elucidated. Title: On the origin and the dynamics of interplanetary dust. Authors: Koutchmy, S. L. Bibcode: 1973pcp..conf...28K Altcode: No abstract at ADS Title: Joint Soviet-French observations of the total solar eclipse on July 10, 1972. Authors: Vsekhsvyatskij, S. K.; Koutchmy, S. L.; Nesmyanovich, A. T.; Dzyubenko, N. I.; Ivanchuk, V. I.; Rubo, G. A. Bibcode: 1973ATsir.789....1V Altcode: No abstract at ADS Title: Observations of the total solar eclipse of June 30, 1973 according to the Soviet-French cooperation programme. Authors: Vsekhsvyatskij, S. K.; Dzyubenko, N. I.; Nesmyanovich, A. T.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Bareau, C.; Begot, J.; Fagot, J. Bibcode: 1973ATsir.800....1V Altcode: No abstract at ADS Title: Étude hydrodynamique du grand jet coronal ne onserv&eacute à I'éclipse du 7 Mars 1970 Authors: Koutchmy, S. Bibcode: 1972SoPh...24..373K Altcode: No abstract at ADS Title: Photometry of a Sunspot at ~ = 3.75 ~s Authors: Coupiac, P.; Koutchmy, S. Bibcode: 1972A&A....16..272C Altcode: Photometry of a Sunspot at = 3.75 A sunspot with an umbra of 16" (fig. 2) was observed in the N0 11145 MacMath plage during Feb. 1971. The ccelostat of the Pic-du-Midi Observatory with an aperture of 50 cm was used in the infra-red range. Good photometric scans were obtained by spatial cancellation techniques using a modulation frequency of 330 Hz and amplitudes <4" with a 0.34 band pass filter and InSb detector at a wavelength of 3.75 the spatial derivates of the photometric sunspot profiles were calibrated by scanning the extreme limb profile (Fig. 1). This technique offers the advantage of permetting a very effective filtering of low frequency noise of atmospheric origin. In this range a 0.60 + 0.03 (uncorrected for the seeing) umbra photosphere contrast was obtained, this giving an umbral temperature of 4200 + 120 K. This value is in agreement with the computed predictions of the recent models of H6noux (1969) and of Stellmacher and Wiehr (1970). We have used Bode (1965) diagrams to deduce T (5000). Key words: Sun - sunspot - infrared photometry - solar physic - spatial cancellation technique. Title: Contribution à l'étude de la couronne solaire en expansion. Authors: Koutchmy, S. Bibcode: 1972PhDT........98K Altcode: No abstract at ADS Title: Diffuise External Reinforcements in the Solar Corona from the March 7 Solar Eclipse Plates Authors: Koutchmy, S. Bibcode: 1972A&A....16..103K Altcode: Observations of diffuse external reinforcements (renforcements externes diffus or R.E.D.) during March 7th total eclipse are reported. The reality of the R.E.D. is demonstrated by the agreement between the results obtained using different methods and by different authors, all these being shown in Table I. The morphology (Fig. 1) and brightness distribution (Fig. 2) are studied. The visible light of the R.E.D. seems to be either unpolarized or slightly polarized in a different way than that, that would be predicted from Thompson scattering. Their position angles appear well correlated with those of active regions (Fig. 3). Two effects are proposed to explain the R.E.D.'s: a)wind or magnetic field effects on circum-solar dust. b)ejection of neutral gas similar to that of the "disparitions brusques" of the prominences. The physical process giving the observed radiation from R.E.D. `s is not elucidated. Many arguinents are given showing that the classical K and F corona concept is insufficient to explain these observations, i.e. the morphology, the relation with solar activity, polarization, the lack of correlation with large coronal streamers, etc. Key words: Sun-solar corona - circum-solar dust - gaz ejection - solar eclipse - streamers Title: Observation in the Wing of the Hα Line and Identification of the Spicular Structure near the Solar Limb Authors: Koutchmy, S.; Macris, C. Bibcode: 1971SoPh...20..295K Altcode: No abstract at ADS Title: Three Dimensional Model of a Large Coronal Streamer with Active Region Enhancement Authors: Koutchmy, S. Bibcode: 1971A&A....13...79K Altcode: A large streamer (Fig. 1) has been studied photometrically (Fig. 8) using some weighted plates obtained at the total eclipse of the 220d September 1968 in Siberia. The synoptic map as well as the green coronal line observations are used (Figs. 4, 6a, 6b) for identification with chromospheric structure. At the center, a coronal enhancement rises above a well defined active region (Figs. 2, 3), around which a 650000 km diameter chain of quiescent prominances has been identified, the streamer rising above the latter. This streamer is composed of two parts: the bulb and "stalks". The proffles (Figs. 5, 7) show the characteristic edge brightening and discontinuity (Fig. 17). A model of the enhancement (Fig. 10) is given; typical value of electronic density is 5- 108 at r = 1.15, in good agreement with radio observations. The quasi-cylindrical edges of the large streamer form the bulb and the measured photometrical proffles (Fig. 9) are well described by electronic density distribution obtained by the formula: fle( r) = n0(r) exp cc (P- )1 H( - , where cc-parameters take values given in Table land the Heaviside function corresponds to the discontinuity; the "stalks" are assumed to have a gaussian density distribution perpendicular to their axis. The values of the edges density (Fig. 14) are not so much higher than the double value of the Newkirk (1961) active region coronal model; the streamer thickness at hall-height of density distribution curve (Fig. 16) is about 30000 km at r = 1.5 and decreases to the sun surface. The differential edge brightening is explained (Fig. 13); this confirming the validity of the model and assumed geometry. The discontinulty is separately studied (Section 4) with a model of linear decrease. Original results concerning the lower limit of transversal gradient density are shown (Table 2); at r = 1.5 this gradient is in the order of 0.25 e-- , that is to say more than 300 times the value of the radial gradient; interpretation is proposed as a tangential discontinuity and a 0.8 Gauss longitudinal magnetic field is found for r = 1.5; its decrease is stronger than the sun center localized dipolar field. The life time of the discontinuity is estimated (4-19) and the obtained values suggest that this thickness can be considerably lower than the measured value, i.e. 4000 km at r = 1.5. Hydrostatic temperature for streamer's edges are lower than the average whereas "stalks" give higher values (Fig. 15); in the central area, above the enhancement, the density is lower, but temperature seems abnormally high; this suggests a model of coronal streamer in expansion with a heating source (Fig. 18) probably constituted by the enhancement; the discontinnity shape confirms this model as well as the application of the continuity equation (Fig. 19). Corpuscular emission associated with the large streamer appeared clearly more efficient than the spherical coronal models' one. The main results are the identification of the large streamer and the enhancement with underlying chromospheric fflaments and plages respectively (Section 2) the model of the streamer for which the lower part (bulb) has a completely different structure compared with those of the models rewiewed (Section 1) previously; the demonstration of the existence of a tangential discontinuity (Section 4) and large magnetic fields in the midcorona, and finally the confirmation of the dominant role of the large streamer as a contributor to corpuscular emission (solar wind). Key words: solar corona - streamers - enhancement - eclipse - corpuscular emission - solar activity - solar wind Title: Observations and Discussions Concerning `High' Polarization Features in the Solar Corona Authors: Koutchmy, Serge; Schatten, Kenneth H. Bibcode: 1971SoPh...17..117K Altcode: Photographic observations were obtained of the radial and tangential polarization of the solar corona for the 1970, March 7, solar eclipse. The corona was photographed using a neutral density filter and rotating linear polaroid sectors to allow the polarization structure to be seen from 1 to 6 solar radii. Anomalously high polarizations were found for structures with the E-tangential intensity being predominantly larger than the E-radial intensity. These structures are generally filamentary in nature and radial in direction. One case with a high radial polarization was also found. The photographs were calibrated accurately against the Earth shine from the Moon. Possible source mechanisms are discussed that may explain this new component in the solar corona. Most sources may be ruled out on physical grounds. One possibility appears to be synchrotron radiation from 10 GeV electrons in a 0.4 G field. The existence of these electrons, however, is unlikely in that spacecraft observations at 1 AU do not confirm their presence. Title: More March 7th eclipse results. Authors: Lilliequist, C.; Schmahl, E.; Laffineur, M.; Koutchmy, S.; Kanno, M.; Sinzi, A. M.; Saito, K. Bibcode: 1970S&T....40...77L Altcode: No abstract at ADS Title: Photometric Study of the Solar Corona Authors: Koutchmy, S.; Laffineur, M. Bibcode: 1970Natur.226.1141K Altcode: No abstract at ADS Title: Study of the Solar Continuum in the Intermediate Infra-Red Spectral Range 3.5-24.4 4u Authors: Koutchmy, S.; Peyturaux, R. Bibcode: 1970A&A.....5..470K Altcode: No abstract at ADS Title: Observation de la lumière cendrée au cours d'une éclipse totale. Authors: Koutchmy, S. Bibcode: 1970CRASB.271..259K Altcode: No abstract at ADS Title: Weighted Observation of the Corona during the Total Solar Eclipse of September 22, 1968 Authors: Laffineur, M.; Burnichon, M. -L.; Koutchmy, S. Bibcode: 1969Natur.222..461L Altcode: WE compare here the prediction of the coronal features made by Schatten1 with the photographic observation made by us in Yurgamish, Siberia. Title: The radio telescope for millimetre waves at the Simeis Observatory. Authors: Laffineur, M.; Koutchmy, S. Bibcode: 1969LOEle..49..246L Altcode: No abstract at ADS Title: Sur un type nouveau de jet coronal associé à des éruptions chromosphériques et à des "bulbes coronaux". Authors: Burnichon, M. -L.; Koutchmy, S.; Laffineur, M. Bibcode: 1969CRASB.269..139B Altcode: No abstract at ADS Title: Some Morphological Particularities of the Solar Corona on 22 September 1968 Authors: Koutchmy, S. Bibcode: 1969ApL.....4..215K Altcode: No abstract at ADS