smartt

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Author name code: smartt
ADS astronomy entries on 2022-09-14
author:"Smartt, Raymond N."

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Title: Detection of opposite polarities in a sunspot light bridge:
evidence of low-altitude magnetic reconnection
Authors: Bharti, Lokesh; Rimmele, Thomas; Jain, Rajmal; Jaaffrey,
S. N. A.; Smartt, R. N.
2007MNRAS.376.1291B Altcode: 2007astro.ph..1674B; 2007MNRAS.tmp..160B
A multiwavelength photometric analysis was performed in order to study
the sub-structure of a sunspot light bridge in the photosphere and
the chromosphere. Active region NOAA 8350 was observed on 1998 October
8. The data consist of a 100 min time series of 2D spectral scans of
the lines FeI 5576 Å, Hα 6563 Å, FeI 6302.5 Å, and continuum images
at 5571 Å. We recorded line-of-sight magnetograms in 6302.5 Å. The
observations were taken at the Dunn Solar Telescope at US National Solar
Observatory, Sacramento Peak. We find evidence for plasma ejection
from a light bridge followed by Ellerman bombs. Magnetograms of the
same region reveal opposite polarity in light bridge with respect to
the umbra. These facts support the notion that low-altitude magnetic
reconnection can result in the magnetic cancellation as observed in
the photosphere.

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Title: Properties of Galactic B supergiants
Authors: Crowther, P. A.; Lennon, D. J.; Walborn, N. R.; Smartt,
2006astro.ph..6717C Altcode:
Physical and wind properties of Galactic B supergiants are presented
based upon non-LTE line blanketed model atmospheres, including
Sher 25 toward the NGC 3603 cluster. We compare Halpha derived wind
densities with recent results for SMC B supergiants and generally
confirm theoretical expectations for stronger winds amongst Galactic
supergiants. Mid B supergiant winds are substantially weaker than
predictions from current radiatively driven wind theory, a problem
which is exacerbated if winds are already clumped in the Halpha line
forming region. We find that the so-called `bistability jump' at B1
(Teff ~ 21kK) from Lamers et al. is rather a more gradual downward
trend. CNO elemental abundances, including Sher 25, reveal partially
processed material at their surfaces. In general, these are in good
agreement with evolutionary predictions for blue supergiants evolving
redward accounting for rotational mixing. A few cases, including HD
152236 (zeta^1 Sco), exhibit strongly processed material which is more
typical of Luminous Blue Variables. Our derived photospheric [N/O] ratio
for Sher~25 agrees with that for its ejecta nebula, although a higher
degree of CNO processing would be expected if the nebula originated
during a red supergiant phase, as is suspected for the ring nebula
ejected by the B supergiant progenitor of SN 1987A, Sk-69 202. Sher
25 has an inferred age of ~5Myr in contrast with ~2Myr for HD 97950,
the ionizing cluster of NGC 3603. Sher 25 may be a foreground object
or close binary evolution could be responsible for its unusual location
in the H-R diagram.

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Title: Interpretation of Localized Deficits in Coronal Emission
Authors: Zhang, Z.; Smartt, R. N.; Landman, D. A.
2002SoPh..207...63Z Altcode:
Coronal images recorded above the limb in Fe xiv (530.3 nm) and Fe x
(637.5 nm) sometimes have localized regions of anomalously low emission,
with the appearance of an abrupt gap in the background corona. These
`dark spaces' have been previously described in the literature in
the case of the 530.3 nm line and tentatively explained by reduced
coronal plasma density and/or a decrease in the line intensity due
to temperatures above or below the optimal ionization temperature
for Fe xiv. However, loops are sometimes observed spanning gaps,
with diminished loop brightness over the region of the gap. It is
concluded that at least some of these regions of reduced brightness are
caused by absorption of the coronal emission. An analysis reveals that
absorption by coronal ions is inadequate as a mechanism to explain the
phenomenon. Absorption by neutral hydrogen is, however, consistent with
the observations in terms of the reduced brightness of the gaps. The
concentration of cool material in the coronal environment associated
with large magnetic fields on the disk could explain the gaps. Hence,
neutral hydrogen continuum absorption appears to provide a plausible
interpretation of, at least, some coronal gaps. Based on this result and
from measured intensities, the electron density in the region of a gap
is derived and found to be consistent with estimates derived elsewhere.

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Title: Results from a revisit to the K2V bright points
Authors: Sivaraman, K. R.; Gupta, S. S.; Livingston, W. C.; Damé,
L.; Kalkofen, W.; Keller, C. U.; Smartt, R.; Hasan, S. S.
2000A&A...363..279S Altcode:
We have used pairs of temporally simultaneous CaII K-line
spectroheliograms and magnetic area scans to search for spatial
correlation between the CaII K2V bright points in the
interior of the network and corresponding magnetic elements. We find
that about 60% of the K2V bright points spatially coincide
with magnetic elements of flux density &gt; 4 Mx cm-2. About
25% of the K2V bright points with equally enhanced emission
lie over bipole elements where the fields are &gt; 4 Mx cm-2
for both polarity elements which merge and presumably cancel and
result in low fields. The rest, 15%, of the bright points coincide
with areas of fields &lt; 4 Mx cm-2 which is the noise
level set by us for the magnetic scans. When magnetic elements of
opposite polarity merge and form bipoles, the associated K2V
bright points show excess emission. Although such excess emission is a
magnetic-field-driven phenomenon, the measured value of the field at the
site of the bipole is typically low, and these cases would therefore be
excluded in the count of coincidences of excess emission with excess
magnetic fields. In our opinion, these cases of excess emission at
the sites of the bipoles, as well as at the sites of fields &gt;
4 Mx cm-2, are both instances of magnetic-field-related
emissions. If the former are not taken into account as coincidences,
the correlation will drop down and this might be interpreted as not an
obvious correlation. Our present results, taking into account the low
fields of merging bipoles, establish the association of K2V
bright points with magnetic elements.

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Title: Multi-wavelength observations of the 1998 September 27
flare spray
Authors: Gallagher, Peter T.; Williams, David R.; Phillips, Kenneth
J. H.; Mathioudakis, Mihalis; Smartt, Raymond N.; Keenan, Francis P.
2000SoPh..195..367G Altcode:
We report on observations of a large eruptive event associated with a
flare that occurred on 27 September 1998 made with the Richard B. Dunn
Solar Telescope at Sacramento Peak Observatory (several wave bands
including off-line-center Hα), in soft and hard X-rays (GOES and
BATSE), and in several TRACE wave bands (including Fe ix/x 171 Å,
Fe xii 195 Å, and C iv 1550 Å). The flare initiation is signaled by
two Hα foot-point brightenings which are closely followed by a hard
X-ray burst and a subsequent gradual increase in other wavelengths. The
flare light curves show a complicated, three-component structure which
includes two minor maxima before the main GOES class C5.2 peak after
which there is a characteristic exponential decline. During the initial
stages, a large spray event is observed within seconds of the hard
X-ray burst which can be directly associated with a two-ribbon flare
in Hα. The emission returns to pre-flare levels after about 35 min,
by which time a set of bright post-flare loops have begun to form at
temperatures of about 1.0-1.5 MK. Part of the flare plasma also intrudes
into the penumbra of a large sunspot, generally a characteristic of
very powerful flares, but the flare importance in GOES soft X-rays is in
fact relatively modest. Much of the energy appears to be in the form of
a second ejection which is observed in optical and ultraviolet bands,
traveling out via several magnetic flux tubes from the main flare site
(about 60° from Sun center) to beyond the limb.

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Title: SECIS: The Solar Eclipse Coronal Eclipse Imaging System
Authors: Phillips, K. J. H.; Read, P. D.; Gallagher, P. T.; Keenan,
F. P.; Rudawy, P.; Rompolt, B.; Berlicki, A.; Buczylko, A.; Diego,
F.; Barnsley, R.; Smartt, R. N.; Pasachoff, J. M.; Babcock, B. A.
2000SoPh..193..259P Altcode:
The Solar Eclipse Coronal Imaging System (SECIS) is an instrument
designed to search for short-period modulations in the solar corona
seen either during a total eclipse or with a coronagraph. The CCD
cameras used in SECIS have the capability of imaging the corona at a
rate of up to 70 frames a second, with the intensities in each pixel
digitised in 12-bit levels. The data are captured and stored on a
modified PC. With suitable optics it is thus possible to search for
fast changes or short-period wave motions in the corona that will
have important implications for the coronal heating mechanism. The
equipment has been successfully tested using the Evans Solar Facility
coronagraph at National Solar Observatory/Sacramento Peak and during
the 11 August 1999 eclipse at a site in north-eastern Bulgaria. The
instrument is described and preliminary results are outlined.

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Title: Obituary John Wainwright Evans, Jr.
Authors: Dunn, Richard B.; Smartt, Raymond N.; Zirker, Jack B.
2000PhT....53c..94D Altcode:
No abstract at ADS

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Title: John W. Evans died 31 October 1999.
Authors: Dunn, R. B.; Simon, G. W.; Smartt, R. N.; Zirker, J. B.
2000SoPh..191..227D Altcode:
No abstract at ADS

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Title: Obituary: John Wainwright Evans, 1909-1999
Authors: Dunn, Richard B.; Simon, George W.; Smartt, Raymond N.;
Zirker, Jack B.
2000BAAS...32.1663D Altcode:
No abstract at ADS

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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.
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.

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Title: The Solar Corona
Authors: Golub, Leon; Pasachoff, Jay M.; Smartt, Raymond N.
1999AmJPh..67..263G Altcode:
No abstract at ADS

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Title: Fine-Scale Structure of Coronal Loops and Consequences for
Coronal Loop Interactions
Authors: Kaghashvili, E.; Smartt, R.
1999ASPC..183..397K Altcode: 1999hrsp.conf..397K
No abstract at ADS

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Title: SOPHIE: a solar EUV multilayer reflecting coronagraph
Authors: Hassler, Donald M.; Slater, David C.; Smartt, Raymond N.;
Koutchmy, Serge L.
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.

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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.
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.

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Title: Advances in ground-based and space-based reflecting coronagraph
designs
Authors: Smartt, Raymond N.; Koutchmy, Serge L.
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.

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Title: Recurrent solar wind streams
Authors: Kim, I. S.; Krussanova, N. L.; Alekseeva, I. V.; Smartt, R. N.
1998R&QE...41...94K Altcode:
A new approach to investigating the statistical relationship between
certain solar features and recurrent wind streams is presented. This
approach is based, on a comparative analysis of the distributions
of lifetimes of a set of solar features, recurrent geomagnetic
disturbances, and geomagnetic “calms.” Correlation coefficients
of 0.81, 0.85, 0.79, and 0.77 are found for the distributions of
several solar features—filaments, large-scale magnetic fields,
coronal features, and coronal holes, respectively—and recurrent
geomagnetic disturbances. A correlation factor of 0.97 between
the distributions of geomagnetic “calms” and active regions is
found. The combined evidence indicates that no specific type of solar
feature is responsible for the recurrent stream activity. Rather, the
configuration of the large-scale magnetic field of the Sun appears
to control the permanently existing corpuscular activity. Since
prominences trace polarity division lines of the large-scale magnetic
field structure of the Sun, they have been checked as a possible general
predictor of recurrent corpuscular activity; their parameters could
present the most reliable indices that relate closely with trends in
geomagnetic disturbances. A comparative analysis of cyclic variations of
sunspot numbers, the total number of prominences, the relative number of
low-height (&lt;-20″) prominences, and recurrent geomagnetic storms is
made for solar cycle N16. The relative number of low-height prominences
is found to correlate broadly (0.83) with recurrent wind streams.

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Title: Coronal loop crossings and associated Hα activity
Authors: Smartt, R. N.; Zhang, Z.; Kim, I. S.; Kaghashvili, E. Kh.
1998ESASP.421..333S Altcode: 1998sjcp.conf..333S
No abstract at ADS

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Title: Observations of the Association of Prominences and the
Surrounding Corona
Authors: Smartt, R. N.; Zhang, Z.; Airapetian, V. S.; Kim, I. S.
1998ASPC..150...37S Altcode: 1998IAUCo.167...37S; 1998npsp.conf...37S
No abstract at ADS

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Title: Analysis of the cross-sectional form of coronal loops:
properties and temporal behavior.
Authors: Kaghashvili, E. Kh.; Smartt, R. N.
1998joso.proc..110K Altcode:
Observations of EUV lines provide evidence of the radial temperature
dependence of coronal loops, with the highest temperature at the outer
part of a loop. Here the authors investigate the cross-sectional
properties of the temperature for both hot and cool loops. It is
found that the radial dependence of the temperature for both types
of loops has the same general characteristics, and this enables to
draw some general conclusions about the thermodynamic quantities that
characterize these loops. From this general picture for an idealized
loop, the authors investigate its evolution for different levels of
energy input, which is considered to be derived from photospheric
motions of the feet of the loop. Based on this, a common scenario
for coronal loop temporal behavior is described. It provides an
interpretation of the difference in lifetimes of hot and cool loops
and of the gradual fading of post flare coronal loops in time.

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Title: New missions for space-based observations of the moon, planets,
and planetary systems with new all-reflecting coronagraph optics
Authors: Morgan, Thomas H.; Slater, David C.; Smartt, Raymond N.
1997SPIE.3116...27M Altcode:
Creative new optical designs for coronagraphs which use only reflecting
elements are extremely well suited for planetary studies which usually
require detection of large, faint, tenuous sources about bright central
planets (themselves worthy of study). These new coronagraphic designs
not only allow the observation of extended atmospheres and coronae,
they also allow critical observations of the central planet at the
same time with instruments optimized for different wavelengths. The
new coronagraphic systems can be more easily accommodated within
the envelope of launch vehicle capabilities available today than
can older, slower systems, and they permit simple spacecraft designs
which reduce weight, power, and cost. They possess inherently higher
end-to-end optical efficiencies. The very modest fluxes associated
with many extended sources in the solar system, however, require
state-of-the-art fabrication techniques, and place new demands on
focal plane instrumentation. We focus here on an instrument designed to
observe the lunar atmosphere. Also considered are several archetypical
problems, including the study of the neutral cloud an ionized torus
associated with Jupiter's moon Io and of comets.

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Title: Imaging Coronal Emission Lines under High Sky-Background
Conditions
Authors: Keller, C. U.; Smartt, R. N.
1996SoPh..166..311K Altcode:
We have obtained images in solar coronal emission lines under high
sky-background conditions by making precise differential measurements
between the coronal emission line and the near-by continuum, which is
primarily due to scattered light from the solar disk. Chopping between
the two wavelengths was performed at 100 kHz to avoid artifacts from
fast-flying dust particles and other aerosols, and also from seeing
effects. The differential signal was detected with a novel CCD camera
that demodulates signals up to 100 kHz. These preliminary observations
show coronal emission at the 0.2% level of the scattered-light
background and pave the way to efficient and precise imaging of coronal
emission features under less than ideal `coronal-sky' conditions.

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Title: Solar drivers of the interplanetary and terrestrial
disturbances
Authors: Balasubramaniam, K. S.; Keil, Stephen L.; Smartt, Raymond N.
1996ASPC...95.....B Altcode: 1996sdit.conf.....B
No abstract at ADS

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Title: White-Light Reflecting Corona graph for the SWATH Mission
Authors: Smartt, Raymond N.; Dunn, Richard B.; Carmichael, Roger
B.; Gregory, B. Scott; Plum, Douglas W.; Neidig, Donald F.; Golub,
Leon; Bookbinder, Jay A.; Koutchmy, George U.; Nystrom, Serge L.;
Zimmermann, Jean-Paul
1996ASPC...95..531S Altcode: 1996sdit.conf..531S
No abstract at ADS

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Title: Coronal Loop Interactions Observed in Optical Emission Lines
Authors: Smartt, R. N.; Airapetian, V. S.; Zhang, Z.
1996mpsa.conf..531S Altcode: 1996IAUCo.153..531S
No abstract at ADS

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Title: Optical Diagnostics of Coronal Loop Interactions
Authors: Airapetian, Vladimir S.; Smartt, Raymond N.
1995ApJ...445..489A Altcode:
Coronal loop interactions (CLIs) are commonly observed in images of
postflare loop systems recorded in the 5303 A (Fe XIV) and 6374.5 A
(Fe X) lines. The CLIs appear as occasional transient brightenings
at the projected intersections of adjacent loops. Observational
parameters of a CLI of 1981 December 7 are used to determine values
of key plasma quantities that characterize these events, leading to
optical diagnostics. On the basis of this analysis, the likelihood of
detecting CLIs at other coronal-line wavelengths is estimated. Finally,
the possible contribution of CLIs to coronal heating is investigated in
terms of the estimated frequency of binary loop-loop collisions in the
solar corona and their dependence on available photospheric magnetic
flux, within and outside active regions. Possible implications for
heating of coronae of dMe stars are discussed.

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Title: Magnetic Reconnection Model for X-Ray Flare Loop Interaction
Authors: Zhang, Zhen-Da; Li, Xiao-Qing; Smartt, R. N.
1995Ap&SS.226...31Z Altcode:
The subtle interactions between the magnetohydrodynamics (MHD) and
transverse plasmons are investigated. It is shown that there is a
resistive instability by the plasmon's soliton in a current sheet,
which eventually turns into an eruptive instability at the magnetic
field reconnection. In the case of ion-acoustic turbulence, the high
temperature current sheet model must adopt the aromalous conductivity
instead of the Coulomb conductivity. The numerical results are
consistent with the observations obtained by Hanaoka (1994). Thus the
flare caused by X-ray loop coalescence can be basically interpreted by
this model of magnetic field reconnection driven by ponderomotive force.

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Title: CLEAR : A Concept for a "Coronagraph and Low Emissivity
Astronomical Reflector" for Solar and Nighttime Observations
Authors: Beckers, J. M.; Kuhn, J.; Neidig, D.; Rabin, R.; Rimmele,
T.; Smartt, R. N.
1995SPD....26..722B Altcode: 1995BAAS...27..971B
No abstract at ADS

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Title: Emission-Line Signatures of Coronal Loop Interactions
Authors: Airapetian, V. S.; Smartt, R. N.
1995itsa.conf...31A Altcode:
No abstract at ADS

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Title: Near-Infrared Coronagraphic Detection of Space Debris
Authors: Neidig, D. F.; Smartt, R. N.; Kim, I. S.; Koutchmy, S.
1995itsa.conf..253N Altcode:
No abstract at ADS

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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.
1995itsa.conf..239K Altcode:
No abstract at ADS

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Title: Reflecting Coronagraphs: Prospects
Authors: Smartt, R. N.; Koutchmy, S.
1995itsa.conf..163S Altcode:
No abstract at ADS

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Title: Comments on Doppler shifts deduced by the Fabry-Perot technique
Authors: Kim, I. S.; Alexeeva, Irina V.; Smartt, Raymond N.
1994ESASP.373...71K Altcode: 1994soho....3...71K
No abstract at ADS

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Title: Photometric imaging observations of the emission corona
Authors: Altrock, R. C.; Smartt, R. N.
1994ESASP.373..425A Altcode: 1994soho....3..425A
No abstract at ADS

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Title: Progress in dynamic research of solar flare magnetic loops.
Authors: Zhang, Zhenda; Smartt, R. N.
1994PABei..12..287Z Altcode:
No abstract at ADS

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Title: Role of loop-loop encounters in coronal heating
Authors: Airapetian, V. S.; Smartt, R. N.
1994ESASP.373...29A Altcode: 1994soho....3...29A
No abstract at ADS

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Title: Magnetic reconnection theory for coronal loop interaction.
Authors: Li, X. -Q.; Zhang, Z.; Smartt, R. N.
1994A&A...290..963L Altcode:
Images of post-flare loop systems recorded in coronal green- and
red-line emissions display occasional transient enhancements at
the intersection of some loops where they come into contact. Such
enhancements are investigated in terms of the likely plasma processes
involved in these dynamic events. For this, the interaction between
magnetohydrodynamic and high frequency plasma waves, and the instability
associated with an electromagnetic solitary wave in a current sheet,
are studied. It is shown that there is a resistive instability, which
eventually turns into an eruptive instability at the onset of magnetic
field reconnection. The numerical results are consistent with the
observations. Thus the phenomenon of occasional enhancements in the
vicinity of the projected intersection of two loops may be basically
interpreted by this theory of magnetic field reconnection driven by
ponderomotive force.

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Title: Moon-based UV reflecting coronagraph
Authors: Vial, J. C.; Koutchmy, S.; Smartt, R. N.
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.

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Title: Analysis of loop interaction in the visible emission corona
Authors: Zhang, Z.; Li, X. -Q.; Smartt, R. N.
1994AdSpR..14d..41Z Altcode: 1994AdSpR..14...41Z
Images of coronal post-flare loop systems in the two coronal lines,
5303Å(Fe XIV) and 6374Å(FeX), show occasional brightenings
at projected points of intersection of overlapping loops. Such
brightenings are interpreted as an interaction between two loops coming
into localized contact due to motion of loop footpoints or when one
loop grows more rapidly than a higher loop. The observations indicate
that partial magnetic reconnection occurs, with associated heating
and subsequent cooling of the plasma in the interaction region. The
phenomenon is commonly observed in post-flare loop systems. Low-energy
events apparently occur also, with less frequency, in quiet coronal
loop systems. An analysis suggests that these events can, as observed,
be described by an initial resistive instability in the region of
the enhancement, which eventually turns into an eruptive instability
at the onset of reconnection. The energy contribution of these small
events to the overall coronal environment is estimated.

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Title: Coronal Loop Interaction Observed at Visible Wavelengths
Authors: Smartt, R. N.; Zhang, Z.; Kim, I. S.; Reardon, K. P.
1994scs..conf..219S Altcode: 1994IAUCo.144..219S
Brightening is observed to occur in regions where two loops come
into contact, with resultant heating of the common plasma volume,
and subsequent cooling. The observations show systematically that a
brightness maximum in the cooler (634 Å) line lags that of the hotter
(5303 Å) line. Coalescence is evident in that the brightness can extend
away from the overlapping region along the adjacent parts of the loops.

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Title: Near-IR Solar Coronal Observations with New-Technology
Reflecting Coronagraplis
Authors: Smartt, R. N.; Koutchmy, S.; Noens, J. -C.
1994IAUS..154..603S Altcode:
No abstract at ADS

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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.
1994IAUS..154..185K Altcode:
No abstract at ADS

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Title: On the Eclipse E-Corona Observations by the Fabry-Perot
Technique
Authors: Kim, I. S.; Smartt, R. N.
1994scs..conf..549K Altcode: 1994IAUCo.144..549K
Interpretations of the eclipse Fabry-Perot interferograms obtained
by different authors are compared particularly in point of view
of velocity measurements. Advantages and disadvantages of the
instrumentation consisting of a Fabry-Perot etalon and a narrow band
interference filter are discussed when a coronal emission is imposed on
steep gradient coronal continuum. A list of optical and near infrared
emission coronal lines is analyzed and a recommendation for employment
of the Fe XIV (5303 Å) and Fe XI (7892 Å) is given.

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Title: The SWATH Satellite Program
Authors: Bookbinder, J.; Golub, L.; Deluca, E.; Smartt, R.
1993AAS...183.0810B Altcode: 1993BAAS...25R1302B
No abstract at ADS

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Title: Post-Flare Coronal Loop Interaction
Authors: Smartt, R. N.; Zhang, Z.; Smutko, M. F.
1993SoPh..148..139S Altcode:
High-resolution images of post-flare loop systems in FeXIV (5303 å)
and FeX (6374 å) display occasional transient enhancements at the
projected intersection of some loops. The brightness of a green-line
enhancement gradually increases to a marked maximum and then fades with
a lifetime of the order of thirty minutes. The red-line image at the
same location, although fainter, shows the same overall characteristics,
its maximum following that of the green-line on average by 8.6 min. Hα
then becomes more evident and reaches a maximum in extent on average
9.3 min after the red-line maximum. The phenomenon is interpreted as
a process of localized loop coalescence involving partial magnetic
reconnection. Estimates of the electron density are derived from
the cooling time following the initial heating of the plasma in the
immediate vicinity of the X-point of interaction. Similar estimates for
the energy dissipated, equivalent to a very small flare, are derived
by two independent methods.

---------------------------------------------------------
Title: Coronal Loop Interaction
Authors: Smartt, R. N.; Zhang, Z.
1993ASSL..183..183S Altcode: 1993pssc.symp..183S
No abstract at ADS

---------------------------------------------------------
Title: Morphology of coronal loop interactions.
Authors: Smartt, Raymond N.; Zhang, Zhenda
1992ESASP.348..185S Altcode: 1992cscl.work..185S
Localized transient brightenings appear occasionally in images of
post-flare coronal loop systems, as recorded in the 5303 Å (Fe XIV)
and 6374 Å (Fe X) lines. Such brightenings occur apparently also in
quiet coronal loop systems, but only in the lower range of energies
that characterize these events. Brightenings result when two loops
come into contact at some point, the enhancement typically extending
partially along the loops away from the point of intersection. The
observations show systematically that a brightness maximum in the cooler
(6374 Å) line lags that of the hotter (5303 Å) line by about 9 min,
on average, while Hα material appears about 9 min later, the sequence
revealing cooling of the plasma following initial heating. Since an
enhancement does not appear in the red line prior to a corresponding
maximum occurring in the green line, it appears that the plasma is
heated rapidly during initial coalescence. Hence, on this basis it is
inferred that such events should be observable in higher-temperature
lines prior to a maximum appearing in the green line. Hα material
is seen to stream down to the surface from the site of interaction,
but there is some evidence also of material moving up from the surface
to the region of interaction. The typical morphology of these events
is discussed.

---------------------------------------------------------
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.
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: Development of Reflecting Coronagraphs
Authors: Smartt, R. N.; Koutchmy, S.
1992ASPC...26..660S Altcode: 1992csss....7..660S
No abstract at ADS

---------------------------------------------------------
Title: Some considerations for instrumentation for a lunar-based
solar observatory
Authors: Smartt, Raymond N.
1992ecos.proc.1890S Altcode:
Outstanding problems in solar physics and observational trends and
directions of instrumental development in solar astronomy are discussed
briefly. These lead to the specification of observational opportunities
and corresponding instrumentation for lunar-based solar observing
facilities. First and second phases for a lunar-based solar observatory
are considered. For phase I, an automated, compact Lyman-alpha/CIV
telescope/coronagraph used principally to monitor flare activity on the
solar disk as well as coronal disturbances is proposed. For phase II,
three facilities are proposed: an array of medium-aperture, extremely
low-instrumental-scatter telescopes operating from EUV through IR
wavelengths; X-ray, XUV telescopes of high-angular resolution; and
a hard X-ray, gamma-ray facility. Dual-purpose (daytime/nighttime)
operation is emphasized.

---------------------------------------------------------
Title: Interpretation of Coronal Loop Interactions
Authors: Smartt, R. N.; Li, X. -Q.; Zhang, Z.
1992AAS...179.3806S Altcode: 1992BAAS...24..681S
No abstract at ADS

---------------------------------------------------------
Title: Interaction of Coronal Loops
Authors: Zhang, Z.; Smartt, R. N.
1992AcASn..32..233Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The morphological characteristics and cooling mechanisms of
the post-flare loop system of April 28, 1980
Authors: Lin, J.; Zhang, Z.; Wang, Z.; Smartt, R. N.
1992A&A...253..557L Altcode:
The paper describes the morphology and evolution of the postflare
loop system of April 28, 1980, which were obtained with the 40-cm
coronograph at NSO/Sacramento Peak (USA). It was found that this flare
loop system is still in variation during the stage of main phase; mass
and energy in the loops are in dynamic equilibrium. The cooling time
for a single loop was estimated on the basis of losses due to radiation,
thermal conduction, and adiabatic expansion of plasma in the loop. The
results show that radiative cooling dominates conductive and expansion
cooling in the cool (T about 10 exp 4 K) flare loops. The nature of
the likely resources which permit the loops to stay bright for a long
time is discussed.

---------------------------------------------------------
Title: Interaction of coronal loops
Authors: Zhang, Zhen-Da; Smartt, R. N.
1991AcASn..32..233Z Altcode:
In this paper the occasional transient enhancement at the interaction
regions of some loops as recorded in coronal images of FeXIV
(5303A) and FeX (6374A), and the associated images in H alpha have
been analyzed. The brightness of a green line enhancement gradually
increases to a maximum and then fades with a typical lifetime of about
20-30 minutes. The maximum of the red line enhancement at the same
location follows that of the green line on average by 8.6 minutes,
and H alpha then reaches a maximum in extent on average 9.3 minutes
after the red line maximum. This phenomenon is interpreted as a process
of localized magnetic reconnection. Estimates of the electron density
are derived from the cooling time, and the values of dissipated energy
are obtained by two separate methods.

---------------------------------------------------------
Title: Eclipse Plans for NSO/SP
Authors: Zirker, J. B.; Koutchmy, S.; Coulter, R. L.; November, L. J.;
Smartt, R. N.
1991BAAS...23.1063Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Dark Gaps in Emission Corona Images
Authors: Smartt, R. N.; Zhang, Z.; Landman, D. A.
1991BAAS...23Q1045S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: High resolution telescopes at the National Solar Observatory
Authors: Dunn, R. B.; Smartt, R. N.
1991AdSpR..11e.139D Altcode: 1991AdSpR..11..139D
The principal high-resolution telescopes of the National Solar
Observatory are its two evacuated telescopes of 61-cm aperture (Kitt
Peak) and 75-cm aperture (Sac Peak). The 61-cm telescope is used for
making full-disk magnetograms, spectromagnetograms and λ10830 maps
that show coronal holes, and is dedicated to synoptic programs. We
describe the 75-cm telescope at Sac Peak. Upgrades that are underway
include an adaptive mirror and fast mirror system that will feed
several focal-plane instruments including the Universal Spectrograph,
a new spectrograph whose detectors are CCD cameras, the Universal
Birefringent Filter, a Fabry-Perot Interferometer and an Advanced
Stokes Polarimeter (ASP), is being constructed at the High Altitude
Observatory. Additional equipment planned for this telescope includes
an improved temperature control subsystem for the entrance window, an
instrument that continually measures Fried's parameter, r0,
and integrating more advanced data collection systems into a computer
network. The observatory is also pursuing a mirror coronagraph, which
should have high resolution and which could be built in apertures
larger than a meter. Operated by the Association of Universities
for Research in Astronomy, Inc. (AURA) under cooperative agreement
with the National Science Foundation.

---------------------------------------------------------
Title: Interpretation of polarization measurements of coronal Fe XIII
(10747 Å) emission.
Authors: Smartt, R. N.; Querfeld, C. W.
1991sopo.work..326S Altcode:
Measurements of the linear polarization of Fe XIII (10747 Å) coronal
emission are discussed. Polarization maps appear to be consistent with
the general form of the expected magnetic field distribution in the
corona as projected in the plane of the sky. Well-defined, large-scale
coronal structures are found to be mapped well by corresponding
polarization measurements.

---------------------------------------------------------
Title: The Morphology Evolution of the Cool Post-Flare Loop System
of April 28, 1980
Authors: Lin, J.; Zhang, Z.; Wang, Z.; Smartt, R. N.
1990AcASn..31..313L Altcode: 1990AcASn..31..317L
No abstract at ADS

---------------------------------------------------------
Title: UV solar reflecting coronagraph
Authors: Smartt, R. N.; Koutchmy, S.; Vial, J. C.
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: 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.
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.
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: Interacting Coronal Loops
Authors: Smartt, R. N.; Zhang, Z.
1990BAAS...22R.870S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coronal Loop Interaction
Authors: Smartt, R. N.; Zhang, Z.
1990IAUS..142..350S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Measurement of telescope system aberrations
Authors: Smartt, R. N.
1989hsrs.conf..232S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: High resolution observations of the solar corona: why and how?
Authors: Koutchmy, S.; Smartt, R. N.
1989hsrs.conf..560K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Ground-Based Mirror Coronograph: First Results
Authors: Smartt, R. N.; Koutchmy, S.; Schwenn, R.
1989BAAS...21..848S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Image processing of coronal pictures
Authors: Smartt, Raymond N.; Koutchmy, Olga; Koutchmy, Serge;
Nitschelm, Christian; Sykora, Julius
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: The Plasma Property of Cool Flare Loops of 1980APR28
Authors: Lin, J.; Wang, Z. Y.; Zhang, Z. D.; Smartt, R. N.
1989AcASn..30...52L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Lithium niobate double channel Fabry-Perot interferometer
for solar corona uses
Authors: Bonaccini, Domenico; Smartt, Raymond N.
1988ApOpt..27.5095B Altcode:
The use of a tunnable etalon in the measurement of spectral profiles
of solar corona emission lines is investigated. The etalon is a y-cut
plate of lithium niobate. A suitable tunning range for the line is +
or - 1 A corresponding to an applied voltage of + or - 1000 V for
a thickness of 0.1 mm. A passband of 0.2 A can realistically be
obtained with an appropriate free spectral range of 6 A. Thermal
analysis shows that a temperature excursion of 0.05 C corresponds to
a spectral drift of less than 0.05 FWHM. An emission line profile is
obtained by scanning an ordinary-ray passband through the emission line,
while measuring the difference between this signal and that from and
adjacent extraordinary-ray passband. Using polarization chopping, the
scattered-light component due to the sky and instrument is efficiently
removed. The extraordinary-ray (reference) passband is insensitive
to the applied voltage; hence the reference signal is substantially
unaffectted by the spectral modulation in the scattered light due to
the solar absorption spectrum.

---------------------------------------------------------
Title: The GONG instrument.
Authors: Harvey, J.; Abdel-Gawad, K.; Ball, W.; Boxum, B.; Bull,
F.; Cole, J.; Cole, L.; Colley, S.; Dowdney, K.; Drake, R.; Dunn,
R.; Duvall, T.; Farris, D.; Green, A.; Hartlmeier, R.; Harvey, J.;
Hubbard, R.; Jackson, P.; Kucera, D.; Miller, C.; Miller, D.; Petri,
A.; Poczulp, G.; Schwitters, J.; Simmons, J.; Smartt, R.; Streander,
G.; Vaughn, F.; Wiborg, P.; GONG Instrument Development Team
1988ESASP.286..203H Altcode: 1988ssls.rept..203H
An instrument is being developed to provide high-quality Doppler
oscillation measurements for the Global Oscillation Network Group
(GONG) project. This instrument uses the Fourier tachometer principle of
sweeping a squared-cosine transmission function across a limited region
of the solar spectrum centered on the Ni I line at 676.8 nm. Doppler
shift is detected as a phase shift between the modulated solar signal
and a simultaneously modulated signal from a stabilized laser. The solar
signal is measured with an array of about 250 by 250 pixels covering
the full disk. Design goals include a short-term noise level at a single
pixel of about 10 m/s per integration interval of 60 s and a long-term
stability of better than one m/s. A "breadboard" model has been in
operation since early 1988 and a prototype is under construction. Most
of the observations as of August 1988 have been of the Doppler shift
of the entire sun imaged onto a single detector. These observations
easily show the global p-mode oscillations with good short-term
signal-to-noise ratio but have revealed a number of interesting
problems. Imaging measurements have started with promising results.

---------------------------------------------------------
Title: Spectroscopic Coronal Observations Using A High-Sensitivity
Camera
Authors: Smartt, R. N.; Colley, S. A.; Gilliam, L. B.; Koutchmy, S.;
Zirker, J. B.
1988BAAS...20..704S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Image processing of coronal pictures.
Authors: Koutchmy, Olga; Koutchmy, Serge; Nitschelm, Christian;
Sykora, Julius; Smartt, Raymond N.
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: Coronal emission-line polarization.
Authors: Smartt, Raymond N.; Arnaud, Jean
1988sscd.conf..451S Altcode:
Polarization measurements from two large data sets are discussed. The
first set consists of measurements obtained in the 5303 Å line of
Fe XIV with the Pic du Midi Coronameter, at heights ranging from 1.1
Rsun to 2.0 Rsun from disk center. The second
set consists of similar observations in the 10747 Å line obtained with
the HAO/SPO Coronal Emission-Line Polarimeter, from 1.1 Rsun
to 1.8 Rsun. Both of the polarization vectors are close to
radial with a mean magnitude of 0.016 and 0.12, respectively. Comparison
of these data with NSO/SP coronal images in the 5303 Å line confirms
that the vectors trace out the coronal loop systems in cases where such
systems are well-defined. For both sets of observations, the magnitude
of the measured polarization is much less than that predicted from
simple scattering theory. The discrepancy is discussed in terms of
the various mechanisms and special geometries that can account for it.

---------------------------------------------------------
Title: Day-time seeing statistics at Sacramento Peak Observatory
Authors: Brandt, P. N.; Mauter, H. A.; Smartt, R.
1987A&A...188..163B Altcode:
A method for the photoelectric measurement of angle-of-arrival
fluctuations at the solar limb is described, from which Fried's
seeing parameter r0 can be determined. From a set of
2092 measurements, each of 10 s duration, performed on 146 observing
days in the period from June 84 to September 86 at the solar vacuum
tower telescope of the Sacramento Peak Observatory, a log-normal
distribution of the r0 values gave a median r0
= 8.7 cm (measured at λ = 510 nm), with a standard deviation σ =
0.25 in logarithmic units. The results are compared with atmospheric
sounding experiment data and longterm day- and night-time seeing
statistics obtained at other observatories.

---------------------------------------------------------
Title: High Spatial Resolution Coronal Physics: The Need for Larger
Coronagraphs
Authors: Smartt, R. N.; Koutchmy, S.; Zirker, J. P.
1987BAAS...19Q1122S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Loop interaction in the visible emission corona - morphological
details.
Authors: Smartt, Raymond N.; Zhang, Zhenda
1987NASCP2483..129S Altcode: 1987tphr.conf..129S
Coronagraph observations of two post-flare loop systems, recorded
photographically in the emissions of Fe XIV (5303 Å) and Fe X
(6374 Å), show occasional enhancements at the intersections of some
loops. The brightness of such enhancements in the green-line gradually
increases to a maximum value several times greater than that of the
legs of the loops and then declines with a typical lifetime ≡30 -
60 minutes. In red-line emission the loop systems are usually very
faint, but show the same overall type of enhancement, with a lag
in maximum brightness relative to that of the green line ≡10
minutes. The electron density, derived from the cooling times, is
≡1012cm-3.

---------------------------------------------------------
Title: Near-Infrared Measurements of the Radiance of the Solar Corona
Authors: Smartt, R.
1987BAAS...19..924S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Flare Associated Coronal Loop Systems in Fexiv 5303A Fex 6374
and Hα Morphological Details and Derived Parameters
Authors: Jain, R.; Smartt, R. N.; Zhaug, Z.
1987BASI...15...19J Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Day-time seeing statistics at Sacramento Peak Observatory.
Authors: Brandt, P. N.; Mauter, H. A.; Smartt, R.
1987LFTR...26...41B Altcode:
The results of the extended series of day-time seeing measurements
performed at the vacuum tower telescope of Sacramento Peak show that
the median r0 value of 8.7 cm is about a factor of 2 higher
than measured at other mountain sites during day-time. Even without
correction for zenith distance this median value ranks among the highest
measured in longterm night-time tests at observatories like Kitt Peak,
Flagstaff, Chile, Calar Alto (Spain), Roque de los Muchachos (Canary
Islands) and others - although one should be cautious when comparing
results obtained with different measuring techniques.

---------------------------------------------------------
Title: Mass Estimate of an Erupting Loop Prominence
Authors: Smartt, R. N.
1986BAAS...18..899S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Electric Field Measurements in Solar Flares
Authors: Zhang, Z.; Smartt, R. N.
1986SoPh..105..355Z Altcode:
Meaurements of solar flare spectra have allowed the electric field
strengths in two flares to be determined, using the Inglis-Teller
formula. Further, an independently estimated value for the
electron density has allowed the two components of this field,
that is, the interionic component and the external component that
arises, for example, through plasma instabilities, to be separately
extracted. External electric field strengths ∼0.5 kV cm−1
for a limb flare and ∼1.3 kV cm−1 for a white-light
flare are found. Estimates of electric fields strengths generated by the
resistive magnetic tearing instability indicate that this process could
account for a significant part of the electric field if pre-existing
magnetic field strengths in the flaring regions are characterized by
a few kilogauss. Other plasma processes probably contribute measurably
as well.

---------------------------------------------------------
Title: Coronal Loop Interaction in the Post-Flare Phase
Authors: Smartt, R. N.; Zhang, Z.
1986BAAS...18..699S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Zone-plate Radial-shear Interferometers a Study of Possible
Configurations
Authors: Smartt, R. N.; Hariharan, P.
1985AcOpt..32.1475S Altcode: 1985JMOp...32.1475S
No abstract at ADS

---------------------------------------------------------
Title: Point-diffraction interference microscopy
Authors: Smartt, Raymond N.; Steel, W. H.
1985ApOpt..24.1402S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Vector Magnetic Fields in Prominences - Part Two Hei d3 Stokes
Profiles Analysis for Two Quiescent Prominences
Authors: Querfeld, C. W.; Smartt, R. N.; Bommier, V.; Landi
Degl'Innocenti, E.; House, L. L.
1985SoPh...96..277Q Altcode:
The Stokes components of He I D3 emission in two quiescent
prominences, using full spectral profile measurements, are analyzed to
derive vector magnetic fields. Two independently developed schemes,
based on the Hanle effect, are used for interpretation. They involve
solutions of the statistical equilibrium equations for the He I
D3 multiplet, including the effect of coherency and full
level crossing, which predict the magnetic field dependence of the
observed polarization. Derived magnetic field vector solutions for
each pair of linear polarization Stokes profiles corresponding to
an observational point in the prominence are, intrinsically, not
uniquely determined, and a set of possible solutions is usually
obtained. However, mutual consistency of these solutions with
those independently predicted by the form of the circular polarized
component, allow, in almost all cases, rejection of all solutions of a
set except one symmetrical pair. Of such a pair, a unique solution can
be determined with a high confidence level by reference to independent
potential field information. Field vectors are found usually to be
close to horizontal and normal to the prominence surface, but extreme
exceptions are found. Field values range from 6 G to 60 G. The derived
vectorfield configurations and their magnitudes are briefly discussed
relative to these prominences and to different quiescent prominence
models.

---------------------------------------------------------
Title: Detailed Morphology of Flare-Associated Coronal Loops
Authors: Smartt, R. N.; Jain, R.
1985BAAS...17Q.645S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Comparison of Coronal Emission Line Structure and Polarization
Authors: Querfeld, C. W.; Smartt, R. N.
1984SoPh...91..299Q Altcode:
Simultaneous observations obtained with the HAO/SPO coronal
emission-line polarimeter and the new SPO emission-line coronagraph
are compared. The polarimeter data are measured in the FeXIII (10747
Å) line and the coronagraph observations are recorded in the FeXIV
(5303 Å) line. The polarimeter field-of-view is relatively coarse
compared with the resolution limit of the coronagraph. Therefore,
the observed coronal polarization cannot be related directly to the
detailed loop structures that characterize the localized coronal
distribution, but it is found that large-scale emission features
have corresponding polarization signatures. Since the measured
linear polarization vectors describe the projected magnetic field
direction, as shown theoretically, it follows that the form of the
large-scale coronal distribution describes corresponding magnetic
field structures. Measured polarization values are consistent with
those predicted theoretically. Interpretation of these data to obtain
corresponding magnetic field directions suggests that the value usually
accepted for iron abundance in the corona might be too large.

---------------------------------------------------------
Title: Visible Coronal Emission Associated with a Quiescent Prominence
Authors: Smartt, R. N.; Zhang, Z.
1984SoPh...90..315S Altcode:
Emission-line coronagraph images of a high-latitude, nominally quiescent
prominence, recorded at wavelengths of Hα, 6374 Å (Fex) and 5303 Å
(Fe XIV), are analyzed. Over a two-day period, the coronal images,
which are found to arise predominantly from coronal emission, evolve
such that the emission becomes concentrated at locations corresponding
to the outer regions of the prominence. This edge enhancement has
similar characteristics to results inferred from EUV prominence
observations. It is postulated that this coronal emission associated
with the prominence results from MHD wave dissipation. Dissipation
lengths for slow-mode, fast-mode and Alfvén waves are estimated for
different prominence conditions. Of these, fast-mode waves appear
to be the most physically realistic heating source if the prominence
magnetic field is along the length of the prominence.

---------------------------------------------------------
Title: Vector Magnetic Fields in Prominences: Observations and
Analysis
Authors: Smartt, R. N.; House, L. L.
1984KodOB...4...35S Altcode:
Stokes polarimeter spectral profiles of He I D3, representing
many observational points within a quiescent prominence, are interpreted
using a detailed quantum-mechanical theory of resonance polarization
for the D3 multiplet. The multiple set of solutions obtained
when the linear polarization information alone is used can be reduced,
generally to a symmetric pair, when the full, generalized theory is
applied that interprets also the weak circular polarization Stokes
profile. In most cases a unique solution can be found through additional
information available from disk field polarity.

---------------------------------------------------------
Title: New observations of the Solar Emission Corona in Fe X and
Fe XIV
Authors: Smartt, R. N.; Zirker, J. B.
1984stp..conf..269S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Vector Magnetic Fields in Prominences - Part Three - Hei d3
Stokes Profile Analysis for Quiescent and Eruptive Prominences
Authors: Athay, R. G.; Querfeld, C. W.; Smartt, R. N.; Landi
Degl'Innocenti, E.; Bommier, V.
1983SoPh...89....3A Altcode:
Observations of linear polarization in two resolved components of HeI
D3 are interpreted using the Hanle effect to determine vector
magnetic fields in thirteen prominences. As in all vector magnetic
field measurements, there is a two-fold ambiguity in field direction
that is symmetric to a 180° rotation about the line-of-sight. The
polar angles of the fields show a pronounced preference to be close to
90° from the local solar radius, i.e., the field direction is close
to horizontal. Azimuth angles show internal consistency from point to
point in a given prominences, but because of the rotational symmetry,
the fields may be interpreted, in most cases, as crossing the prominence
either in the same sense as the underlying photospheric fields or in
the opposite sense.

---------------------------------------------------------
Title: A White-Light / Fex / Hα Coronal Transient Observation to
10-SOLAR-RADII
Authors: Wagner, W. J.; Illing, R. M. E.; Sawyer, C. B.; House, L. L.;
Sheeley, N. R., Jr.; Howard, R. A.; Koomen, M. J.; Michels, D. J.;
Smartt, R. N.; Dryer, M.
1983SoPh...83..153W Altcode:
Multi-telescope observations of the coronal transient of 15-16
April, 1980 provide simultaneous data from the Solar Maximum Mission
Coronagraph/Polarimeter, the Solwind Coronagraph, and the new Emission
Line Coronagraph of the Sacramento Peak Observatory. An eruptive
prominence-associated white light transient is for the first time
seen as an unusual wave or brightening in Fe Xgl6374 (but not in
Fe XIVgl5303). Several interpretations of this fleeting enhancement
are offered.

---------------------------------------------------------
Title: Test of vacuum vs helium in a solar telescope.
Authors: Engvold, O.; Dunn, R. B.; Livingston, W. C.; Smartt, R. N.
1983ApOpt..22...10E Altcode:
The consequences of filling a solar telescope with helium, a gas with an
exceptionally low index of refraction and a high thermal conductivity,
are reported. All the tests are conducted with the solar beam present to
provide normal heating. Internal seeing of the telescope is evaluated by
viewing the image of an He-Ne laser beam in autocollimation reflected
from the entrance window for different pressures of air or helium. The
total path of the laser beam through the tank (six times) becomes
about 100 m. Quantitative measurements of the wave front distortions
are derived by inserting a point-diffraction interferometer near the
focused image of the laser beam. Excursions of the fringe pattern yield
direct measures of the wave front errors in units of the 0.633-micron
laser wavelength. It is concluded that a helium-filled telescope is a
realistic alternative to a vacuum telescope for solar observations. The
barely detectable tank seeing with helium near atmospheric pressure
could possibly be rectified either by a high reflectivity coating of
the mirrors, which reduces the heat load, or by a forced circulation
of the helium in the tank.

---------------------------------------------------------
Title: Precision Tuning and Improved Stability of a Universal
Birefringent Filter
Authors: Stauffer, F. R.; Smith, G. H.; Streander, G. W.; Wilkins,
L. M.; November, L. J.; Smartt, R. N.
1983SPIE..380...77S Altcode:
Basic modifications of the Sacramento Peak Observatory Universal
Birefringent Filter system and resultant major improvements in its
performance are described. Spectral tuning is accomplished by rotating
the nine birefringent elements that comprise the filter. For this,
stepper motors are used under computer control, where one step is
equivalent to a precision of 0.0025 Å (at 7000 A) for the narrowest
bandpass element. The element angles are accurately set for an arbitrary
wavelength by an algorithm derived from known tune solutions. Absolute
wavelength calibration is provided by a He-Ne laser source, while
an integrated monochromator can be used for the same purpose, though
less accurately, throughout the 4100 A to 7000 A spectral range of the
filter. The filter is maintained in a thermally stable environment
controlled to a precision of 0.05° C; any incremental temperature
change in the filter itself can be detected and its effects compensated
by means of a laser calibration. In operation, the filter can typically
be tuned to a selected wavelength in less than is with a precision of
1 mÅ.

---------------------------------------------------------
Title: Solar corona photoelectric photometer using mica etalons
Authors: Smartt, R. N.
1982SPIE..331..442S Altcode:
A solar corona photoelectric photometer has been constructed that
operates at the three coronal lines, Fe XIV (5302.9 A), Ca XV (5694.5 A)
and Fe X (6374.5 A), using mica etalons and narrow-band interference
filters. The photometer is used with a 40-cm coronagraph feed. In each
case, the corona is discriminated from the sky background, by means
of polarization-chopping between the line passband and a reference
continuum passband. A mica etalon allows the reference passband to
be arbitrarily located in the vicinity of the spectral line. Also,
the width of the etalon passbands can be matched to that of the
coronal line width, and the transmittance can be high if extremely
transparent mica is used. A photomultiplier detects the two signals,
their difference being proportional to coronal radiance. The photometer
performance is illustrated by radiance plots derived from observations
obtained at a fixed height in the corona at equally-incremented field
points around the limb.

---------------------------------------------------------
Title: Vector Magnetic Fields in Prominences - Part One - Preliminary
Discussion of Polarimeter Observations in he i D3
Authors: House, L. L.; Smartt, R. N.
1982SoPh...80...53H Altcode:
A preliminary discussion is presented of measurements of the
polarization of the He I D3 multiplet in a quiescent
prominence, observed with a wavelength-scanning Stokes polarimeter. For
a series of 43 observations in the same prominence, the linear
polarization of the major component of D3 lies primarily
in the range 1 to 2% and of the wing component, the range 2 to 5%;
the polarization vector angle lies primarily in the range 10-25°
for the major component, and 25-35° for the other component. From a
more limited data set, the polarization of both components is found
to first increase as a function of height in the prominence, and
then to decrease; the polarization angles of the major component
vary in a random-like way with height, while the wing component
shows a systematic change. The amount of polarization and the angle
of polarization are governed by the Hanle effect. The collective
effect of the group of lines at the peak of D3 evidently
has a different sensitivity to the Hanle effect than does the wing
component, thus yielding at least four independent measurements -
two polarizations and two angles. With some redundancy, the vector
magnetic field can then be established using the detailed theory
of the Hanle effect. Since the wing component of D3 is a
simple triplet, an initial estimate of the magnetic field strength
and its horizontal orientation, 0, relative to the line of sight,
is simply obtained. Examples of such calculations are presented.

---------------------------------------------------------
Title: Coronal Emission Associated with a Quiescent Prominence
Authors: Smartt, R. N.; Zhang, Z.
1982BAAS...14Q.623S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Interferometric eclipse observations of the Fe XIV inner
corona.
Authors: Smartt, R. N.; Zirker, J. B.; Mauter, H. A.
1982PINSA..48..102S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Interferometric Eclipse Observations of the Fe XIV Inner Corona
Authors: Smartt, R. N.; Zirker, J. B.; Mauter, H. A.
1982PIAS...48..102S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Design and performance of a new emission-line coronograph.
Authors: Smartt, R. N.; Dunn, R. B.; Fisher, R. R.
1981SPIE..288..395S Altcode:
A new emission-line solar coronagraph is described that photographically
records coro-nal emission of the Fe XIV (5303 Å) and Fe X (6374 Å)
lines, and prominences and the solar disk in Hα (6563
Å). The basic optical system consists of a 20-cm aperture, f/11
aspheric singlet objective and four secondary optical systems--one
for each image channel--that are sequentially switched into the
beam. Interference filters and a specially-designed Lyot birefringent
filter isolate spectral bands ≍ 1 Å at the three wavelengths. The
efficiency of this filtering and special constructional features
result in an exceptionally small amount of scattered light reaching
the film plane. Coronal images can be recorded in skies some 2.5
times brighter than is typical for earlier designs of emission-line
corona-graphs. Features of the data obtained so far, including high
contrast and high spatial resolution images and the detection of
extremely rapid coronal changes, are discussed.

---------------------------------------------------------
Title: Eclipse observations of coronal Fe XIV emission.
Authors: Smartt, R. N.; Zirker, J. B.; Mauter, H. A.
1981otse.conf...36S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Quiescent Prominence Vector Magnetic Fields Inferred from He
I D3 Polarization
Authors: Querfeld, C. W.; Smartt, R. N.; Bommier, V.; Landi
Degl'Innocenti, E.
1980BAAS...12..792Q Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Vector Magnetic Fields Inferred from He I D3
Polarization in the August 5, 1980 Eruptive Prominence
Authors: Querfeld, C. W.; Smartt, R. N.; Bommier, V.; Landi
Degl'Innocenti, E.
1980BAAS...12..913Q Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Comparison of Coronal Emission-Line Structure and Observed
Polarization
Authors: Smartt, R. N.; Querfeld, C. W.
1980BAAS...12..793S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Three-Coronagraph Record from 1 to 10 RO of the
Energetics of a Coronal Transient
Authors: Wagner, W. J.; Sawyer, C.; Illing, R. M. E.; House, L. L.;
Querfeld, C. W.; Sheeley, N. R., Jr.; Howard, R. A.; Koomen, M. J.;
Michels, D. J.; Smartt, R. N.
1980BAAS...12Q.902W Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Interferometric Eclipse Observations of Coronal Fexiv Emission
Authors: Smartt, R. N.; Zirker, J. B.; Mauter, H. A.
1980BASI....8...59S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar corona spectra observations in active, quiescent and
hole regions.
Authors: Gilliam, L. B.; Smartt, R. N.; Zirker, J. B.
1980BAAS...12..751G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Polarization Measurements of Prominences - Characteristics
of Stokes Profiles
Authors: Smartt, R. N.; House, L. L.
1979BAAS...11..409S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Point-Diffraction Interference Microscopy
Authors: Smartt, R. N.; Steel, W. H.
1979JOSA...69.1455S Altcode: 1979OSAJ...69.1455S
No abstract at ADS

---------------------------------------------------------
Title: Scattered-light measurements of optical surfaces
Authors: Smartt, R. N.
1979SPIE..190...58S Altcode:
Measurements of the angular distribution of scattered light produced
by specially-polished optical components are reported. The components
were six 12-cm aperture coronagraph objective mirrors and two
20-cm coronograph objective lenses. For each test the component was
illuminated with white light and the magnitude of the scattered flux
measured at several field points. It was not feasible to separate
surface and body scattering of the lenses, so that these measurements
represent the combined contributions. Successive recoatings and tests
of the mirrors has led to the conclusion that the residual roughness
of the substrate polish is the dominant parameter that determines
the magnitude of the scattered flux. Dark ground and phase contrast
measurements qualitatively support this conclusion. The fractional
contributions of integrated scattered light of the lenses and mirrors
are found to be of the same order, although the functional relationships
are significantly different over the angular range measured.

---------------------------------------------------------
Title: Special applications of the point-diffraction interferometer
Authors: Smartt, R. N.
1979SPIE..192...35S Altcode:
Characteristics and applications of the point-diffraction interferometer
(PDI) are discussed, including the effects of moving the aperture
in various directions. The test of an astronomical telescope using a
stellar source emphasized the benefits to an accurate error analysis
of excellent atmospheric seeing conditions. Also considered are
a test of a telescope with an He-Ne laser source at a distance of
2.3 km and a test of the universal birefringent filter system. It
is concluded that the PDI is an extremely convenient device to test
complex optical systems in situ, on- and off-axis, especially in cases
where a double-pass configuration is not practicable, where vibration
sources are not negligible and where a direct, rapid measure of the
wavefront aberration is desirable.

---------------------------------------------------------
Title: Discussion
Authors: Landi Degl'Innocenti, M.; Kundu, M. R.; Landman, D. A.;
Smartt, R. N.; Stenflo, J.
1979phsp.coll...85L Altcode: 1979IAUCo..44...85D; 1979phsp.coll...85D
No abstract at ADS

---------------------------------------------------------
Title: Stokes Polarimetry of Quiescent Prominences in HeI
D3.
Authors: House, L. L.; Smartt, R. N.
1979phsp.coll...81H Altcode: 1979IAUCo..44...81H; 1979phsp.conf...81H
No abstract at ADS

---------------------------------------------------------
Title: Stokes Polarimetry of Quiescent Prominences in He I
D3
Authors: House, L. L.; Smartt, R. N.
1978BAAS...10..672H Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Zone-Plate Radial-Shear Interferometer
Authors: Smartt, R. N.
1978JOSA...68.1391S Altcode: 1978OSAJ...68.1391S
No abstract at ADS

---------------------------------------------------------
Title: Scattering Properties of Coronagraph Objective Lenses and
Mirrors.
Authors: Smartt, R. N.
1977BAAS....9..370S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Absolute measurements of optical flats (A)
Authors: Smartt, Raymond N.
1976JOSA...66.1104S Altcode: 1976OSAJ...66.1104S
No abstract at ADS

---------------------------------------------------------
Title: Observations of the near-infrared solar corona and a new
interferometric telescope test
Authors: Smartt, Raymond Newton
1976PhDT.......366S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observations of the Near-Infrared Solar Corona and a New
Interferometric Telescope Test.
Authors: Smartt, R. N.
1976PhDT.........3S Altcode:
Observations of the infrared outer solar corona were carried out,
two with a balloon-borne infrared scanning coronagraph during balloon
flights on October, 1973, and the other, ground-based at the June 30,
1973, total solar eclipse. The performance of the 6-detector coronagraph
was evaluated, particularly with regard to its novel dual reflective
optical systems. The coronagraph balloon flight radiance data,
derived from coronal scans spanning elongations of approximately 3-13
solar radii, and a wavelength range of 2-4 microns, is presented. The
eclipse data represents the coronal elongation radiance distribution
parallel to the ecliptic, over a range of approximately 2-9 solar
radii, at a wavelength of 1 micron. A new two-beam interferometer and
its application to the testing of telescopes are also described. The
interferometer is positioned at the image of a point source, and forms
a spherical reference wavefront by diffraction of part of the incident
light. Field tests using both star and laser sources were successful.

---------------------------------------------------------
Title: Theory and Application of Point-Diffraction Interferometers
Authors: Smartt, R. N.; Steel, W. H.
1975JaJAP..14...14S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Simple unequal-path interferometer configurations (A)
Authors: Smartt, Raymond N.
1975JOSA...65.1210S Altcode: 1975OSAJ...65.1210S
No abstract at ADS

---------------------------------------------------------
Title: Zone plate interferometer
Authors: Smartt, Raymond N.
1974ApOpt..13.1093S Altcode: 1974ApOpt..13..109S
Available from <A
href="http://www.opticsInfoBase.org/abstract.cfm?id=18526;">http://www.opticsInfoBase.org/abstract.cfm?id=18526;</A>

---------------------------------------------------------
Title: Point-Diffraction Interferometer
Authors: Smartt, R. N.; Strong, J.
1974OptEn..13.G198S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Point-Diffraction Interferometer
Authors: Smartt, R. N.; Strong, J.
1974JOSA...62..737S Altcode: 1974OSAJ...62..737S
No abstract at ADS

---------------------------------------------------------
Title: Telescope Test using the Point-Diffraction Interferometer
Authors: Smartt, R. N.
1974JOSA...64..558S Altcode: 1974OSAJ...64..558S
No abstract at ADS

---------------------------------------------------------
Title: Coronagraph Mirrors for the Near Infrared
Authors: Smartt, R. N.; Dalton, W. S.
1971JOSA...61..665S Altcode: 1971OSAJ...61..665S
No abstract at ADS

---------------------------------------------------------
Title: A Variable Transmittance Beam Splitter
Authors: Smartt, R. N.
1970ApOpt...9..970S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Fresnel Zone Plate Interferometer
Authors: Smartt, R. N.; Givens, M. P.
1969JOSA...59.1522S Altcode: 1969OSAJ...59.1522S
No abstract at ADS

---------------------------------------------------------
Title: Mica Polarizing Prism
Authors: Dumont, F. J.; Smartt, R. N.
1969JOSA...59.1541D Altcode: 1969OSAJ...59.1541D
No abstract at ADS

---------------------------------------------------------
Title: A Tunable Birefringent Fabry-Perot Interferometer
Authors: Ramsay, J. V.; Smartt, R. N.
1966ApOpt...5.1341R Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Production and Use of the Optical-Contact Bond
Authors: Smartt, R. N.; Ramsay, J. V.
1964JPhE...41..514S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A 1/8 A Birefringent Filter for Solar Research
Authors: Steel, W. H.; Smartt, R. N.; Giovanelli, R. G.
1961AuJPh..14..201S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Production of High-Quality Optical Surfaces on Calcite
Authors: Smartt, R. N.
1961JPhE...38..165S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Birefringence of quartz and calcite
Authors: Smartt, R. N.; Steel, W. H.
1959JOSA...49..710S Altcode: 1959OSAJ...49..710S
No abstract at ADS