Author name code: makita ADS astronomy entries on 2022-09-14 author:"Makita, Mitsugu" ------------------------------------------------------------------------ Title: Demonstration of an x-ray Raman spectroscopy setup to study warm dense carbon at the high energy density instrument of European XFEL Authors: Voigt, K.; Zhang, M.; Ramakrishna, K.; Amouretti, A.; Appel, K.; Brambrink, E.; Cerantola, V.; Chekrygina, D.; Döppner, T.; Falcone, R. W.; Falk, K.; Fletcher, L. B.; Gericke, D. O.; Göde, S.; Harmand, M.; Hartley, N. J.; Hau-Riege, S. P.; Huang, L. G.; Humphries, O. S.; Lokamani, M.; Makita, M.; Pelka, A.; Prescher, C.; Schuster, A. K.; Šmíd, M.; Toncian, T.; Vorberger, J.; Zastrau, U.; Preston, T. R.; Kraus, D. Bibcode: 2021PhPl...28h2701V Altcode: We present a proof-of-principle study demonstrating x-ray Raman Spectroscopy (XRS) from carbon samples at ambient conditions in conjunction with other common diagnostics to study warm dense matter, performed at the high energy density scientific instrument of the European x-ray Free Electron Laser (European XFEL). We obtain sufficient spectral resolution to identify the local structure and chemical bonding of diamond and graphite samples, using highly annealed pyrolytic graphite spectrometers. Due to the high crystal reflectivity and XFEL brightness, we obtain signal strengths that will enable accurate XRS measurements in upcoming pump-probe experiments with a high repetition-rate, where the samples will be pumped with high-power lasers. Molecular dynamics simulations based on density functional theory together with XRS simulations demonstrate the potential of this technique and show predictions for high-energy-density conditions. Our setup allows simultaneous implementation of several different diagnostic methods to reduce ambiguities in the analysis of the experimental results, which, for warm dense matter, often relies on simplifying model assumptions. The promising capabilities demonstrated here provide unprecedented insights into chemical and structural dynamics in warm dense matter states of light elements, including conditions similar to the interiors of planets, low-mass stars, and other celestial bodies. Title: Laboratory measurements of resistivity in warm dense plasmas relevant to the microphysics of brown dwarfs Authors: Booth, N.; Robinson, A. P. L.; Hakel, P.; Clarke, R. J.; Dance, R. J.; Doria, D.; Gizzi, L. A.; Gregori, G.; Koester, P.; Labate, L.; Levato, T.; Li, B.; Makita, M.; Mancini, R. C.; Pasley, J.; Rajeev, P. P.; Riley, D.; Wagenaars, E.; Waugh, J. N.; Woolsey, N. C. Bibcode: 2015NatCo...6.8742B Altcode: 2015NatCo...6E8742B Since the observation of the first brown dwarf in 1995, numerous studies have led to a better understanding of the structures of these objects. Here we present a method for studying material resistivity in warm dense plasmas in the laboratory, which we relate to the microphysics of brown dwarfs through viscosity and electron collisions. Here we use X-ray polarimetry to determine the resistivity of a sulphur-doped plastic target heated to Brown Dwarf conditions by an ultra-intense laser. The resistivity is determined by matching the plasma physics model to the atomic physics calculations of the measured large, positive, polarization. The inferred resistivity is larger than predicted using standard resistivity models, suggesting that these commonly used models will not adequately describe the resistivity of warm dense plasma related to the viscosity of brown dwarfs. Title: The energy spectrum of the light components (P+He) at the knee obtained by the Tibet air shower core detector Authors: Katayose, Y.; Amenomori, M.; Ayabe, S.; Chen, D.; Cui, S. W.; Danzengluobu; Ding, L. K.; Ding, X. H.; Feng, C. F.; Feng, Z. Y.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Haibing, Hu; Hu, H. B.; Huang, J.; Huang, Q.; Jia, H. Y.; Kajino, F.; Kasahara, K.; Kato, C.; Kawata, K.; Labaciren; Le, G. M.; Li, J. Y.; Lu, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nishizawa, M.; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Sakata, M.; Sasaki, T.; Shibata, M.; Shiomi, A.; Shirai, T.; Sugimoto, H.; Makita, M.; Tan, Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wang, X.; Wang, Y. G.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yan, C. T.; Yang, X. C.; Yasue, S.; Ye, Z. H.; Yu, G. C.; Yuan, A. F.; Yuda, T.; Zhang, H. M.; Zhang, J. L.; Zhang, N. J.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhaxisangzhu; Zhou, X. X. Bibcode: 2005ICRC....6..185A Altcode: 2005ICRC...29f.185A No abstract at ADS Title: Calibration of the instrumental polarization of the Domeless Solar Telescope at the Hida Observatory Authors: Kiyohara, Junko; Ueno, Satoru; Kitai, Reizaburo; Kurokawa, Hiroki; Makita, Mitsugu; Ichimoto, Kiyoshi Bibcode: 2004SPIE.5492.1778K Altcode: A new spectropolarimeter is developed at the Domeless Solar Telescope (DST) in Hida Observatory. It consists of a rotating waveplate, Wollaston prisms, and a high-dispersion spectrograph which is vertically installed at the focus of the DST. In order to realize a high-precision measurement, it is inevitable to compensate the instrumental polarization due to the DST. We observed the quiet region of the Sun, which is considered to be highly unpolarized, with and without a sheet linear polarizer or circular polarizer set at the entrance window of the telescope. The theoretical model which represents the total instrumental polarization of the DST with some characteristic parameters was calculated and compared with the observation. The model that two flat mirrors have different properties can explain the observation in 0.5% accuracy for the unpolarized light, and in 7% for the polarized light. Title: On the nature of the suspected dwarf nova, HP Andromedae Authors: Nogami, D.; Ishioka, R.; Makita, M.; Kato, T.; Yamaoka, H.; Uemura, M.; Mineshige, S. Bibcode: 2003IBVS.5416....1N Altcode: The object having been identified with HP And is not a dwarf nova. Title: Chromospheric structure derived from flash spectra of the total solar eclipse Authors: Makita, Mitsugu Bibcode: 2003PNAOJ...7....1M Altcode: A chromosphere model for the analysis of emission lines in a flash spectrum is constructed. Emission gradients of metallic and Balmer lines in flash spectra give height distributions of the total hydrogen and the product of electron and proton density in the high chromosphere, respectively. The derived distributions imply the presence of "spicule" structure which has a filling factor of 0.05 at 4,000 km above the base of the chromosphere. They explain the averaged eclipse curves of Ca II H and K, and Hɛ line profiles observed in a 1958 flash spectrum and the Balmer and Sr II emissions observed in a 1962 flash spectrum. Their excitation and ionization seem to match the radiation field of the chromosphere. They are applied to 24 Ca II H and K spicules in the higher chromosphere observed during the 1958 eclipse. The analysis shows that they have a turbulence of 22 km/s on the average and 19 of them are thinner than 2,000 km. The Ca II H and K, and Hɛ emissions of the active region observed during the 1958 eclipse are enhanced mainly by the increase of their source functions due to an increase in their excitation temperatures. Title: Emission line eclipse mapping of velocity fields in dwarf nova accretion discs Authors: Makita, M.; Mineshige, S. Bibcode: 2002ASPC..261..501M Altcode: 2002pcvr.conf..501M We propose a new method, emission-line eclipse mapping, to map the velocity fields in an accretion disc. We apply the usual eclipse mapping technique to the light curves at each of 12-24 wavelengths across the line center to map the region with same line-of-sight velocity, from which we are able to plot the rotational velocity as a function of radius on the assumption of axisymmetric disc. We calculate time changes of the emission line profiles, assuming Keplerian rotation fields (vvarphi propto r-1/2) and the emissivity distribution of j propto r-3/2, and reconstruct emissivity profiles. The results show typically a `two-eye' pattern for high line-of-sight velocities and we can recover the relation, vvarphi propto d-1/2, where d is the separation of two lq eyes.' Title: Numerical Simulation of Interaction between an L1 Stream and an Accretion Disk in a Close Binary System Authors: Fujiwara, H.; Makita, M.; Nagae, T.; Takuya Bibcode: 2001PThPh.106..729F Altcode: 2001astro.ph..9238F Numerical simulation of the hydrodynamic behavior of an accretion disk in a close binary system is reported. Calculations were carried out for a region including a compact star and its gas-supplying companion. The equation of state is that of an ideal gas characterized by a specific heat ratio γ. Two cases, with γ=1.01 and γ=1.2, are studied. Our calculations show that the gas, flowing from the companion via a Lagrangian L1 point towards the accretion disk, forms a fine gas beam (L1 stream), which penetrates into the disk. Thus, no hot spot forms in these calculations. Another result is that the gas rotating with the disk forms ---upon collision with the L1 stream--- a bow shock wave, which we call an `L1 shock'. The disk becomes hot because the L1 shock heats the disk gas in the outer parts of the disk, so that the spiral shocks wind loosely, even with γ=1.01. The L1 shock enhances axial asymmetry of the density distribution in the disk, and therefore angular momentum is transferred through the tidal torque more effectively. The maximum value of the effective α becomes ~ 0.3. A `hot spot' is not formed in our simulations, but our results suggest the formation of a `hot line', which is the L1 shock elongated along the penetrating L1 stream. Title: WZ Sagittae. Authors: Baba, H.; Sadakane, K.; Norimoto, Y.; Nogami, D.; Matsumoto, K.; Makita, M.; Kato, T. Bibcode: 2001IAUC.7678....2B Altcode: No abstract at ADS Title: WZ Sagittae Authors: Kato, T.; Ohashi, H.; Ishioka, R.; Uemura, M.; Matsumoto, K.; Masi, G.; Starkey, D.; Pietz, J.; Martin, B.; Baba, H.; Sadakane, K.; Norimoto, Y.; Nogami, D.; Makita, M. Bibcode: 2001IAUC.7678....1K Altcode: 2001IAUC.7678A...1K T. Kato, H. Ohashi, R. Ishioka, M. Uemura and K. Matsumoto, Kyoto University; G. Masi, Ceccano, Italy; D. Starkey, Auburn, Indiana; J. Pietz, Erftstadt, Germany; and B. Martin, The King's University College, Edmonton, Alberta, on behalf of the VSNET collaboration team, report: "Our time-resolved CCD photometry revealed that WZ Sge started to show a different type of prominent modulations (amplitude 0.10 mag) on Aug. 4.53 UT. Between Aug. 4.44 and 5.08 the oscillations had an initial period of 0.057143 +/- 0.000046 day, which is 0.8 percent longer than the orbital period (0.05669 day). Earlier observations, starting on Aug. 4.163, also showed a suggestion of the growing signal. Later observations, between Aug. 5.166 and 6.074, have shown further development of superhumps up to 0.23 mag and give a mean period of 0.058876 +/- 0.000025 day. The sharply defined profile and the period excess qualify the present variations as genuine superhumps. The superhumps developed from the secondary hump structure of the early superhumps (IAUC 7672). The 12-day delay of superhump evolution since the start of the outburst is the longest one measured among all known SU UMa-type dwarf novae. The observed delay is consistent with the earliest time of detection of a similar, but less distinct, signal during the 1978 outburst (Heiser and Henry, IBVS 1559)." H. Baba, National Astronomical Observatory of Japan; K. Sadakane, Osaka-Kyoiku University; Y. Norimoto, Okayama Astrophysical Observatory (OAO); and D. Nogami, K. Matsumoto, M. Makita and T. Kato, Kyoto University, report: "We constructed Doppler tomograms of WZ Sge using time-resolved spectra (resolution about 3000) covering two binary orbits between July 24.576 and 24.701 UT with the OAO 0.91-m telescope (IAUC 7672). The He II (468.6 nm) map shows that the emitting region on the accretion disk is elongated along the ballistic stream, which constitutes an asymmetric 'boomerang-like' one-armed spiral structure. The present observation shows the earliest detection of presence of the spiral structure of the emission line. Since Steeghs et al. (IAUC 7675) reported that the He II and C III emission lines were dominated by a two-armed spiral pattern four days after the maximum, there must have been a dramatic change in the emission pattern between our earlier observation and theirs. Such a totally unprecedented, unexpected change may be responsible for the growth of early superhumps." Title: Spiral Shocks in an Inviscid Simulation of Accretion Flow in a Close Binary System Authors: Makita, M.; Fujiwara, H.; Matsuda, T.; Boffin, H. M. J. Bibcode: 2001LNP...573...88M Altcode: 2001astr.conf...88M We perform 2D and 3D numerical simulations of an accretion disc in a close binary with a mass ratio of 0.5, corresponding to the dwarf nova IP Pegasi. We do not include artificial nor α-viscosity and supply gas from the inner L1 point. We construct Doppler maps and artificial trailed spectrograms. In the 2D calculation, the results agree very well with those observed in IP Peg. In the 3D calculations, the stream from the L1 point penetrates into the accretion disc. The resulting flow pattern, therefore, is different from the 2D results. Title: Eclipse Curves of Ca H, K, and Hɛ Structures Authors: Makita, M. Bibcode: 2000ASPC..205...97M Altcode: 2000ltse.conf...97M Eclipse curves of Ca H, K, and Hɛ structures are obtained from the 1958 flash spectrum. Under the active region, Ca and Hɛ lines are enhanced by 0.2 and 0.3 in logarithmic scale, respectively. Ca line ratio K/H is greater than 1 and seems not to reach 2. 58% of Ca line profiles below 2500 km do not show central dips but single peaks. Width difference of Ca and Hɛ lines may give kinetic temperature of 9000circ K for isolated structures. Title: 3D numerical simulation of accretion disc Authors: Matsuda, T.; Fujiwara, H.; Makita, M.; Nagae, T.; Oka, K.; Boffin, H. Bibcode: 2000NewAR..44P..21M Altcode: No abstract at ADS Title: Spiral Structure in IP Peg: Confronting Theory and ObservationsCD Authors: Matsuda, T.; Makita, M.; Yukawa, H.; Boffin, H. M. J. Bibcode: 1999ASSL..240..207M Altcode: 1998astro.ph..7239M; 1999numa.conf..207M The first convincing piece of evidence of spiral structure in the accretion disc in IP Pegasi was found by Steeghs et al. (1997). We performed two kinds of 2D hydrodynamic simulations, a SFS finite volume scheme and a SPH scheme, with a mass ratio of 0.5. Both results agreed well with each other. We constructed Doppler maps and line flux-binary phase relations based on density distributions, the results agreeing well with those obtained by observation. Title: 3D Simulations of the Spiral Structure Authors: Matsuda, T.; Makita, M.; Boffin, H. M. J. Bibcode: 1999dicb.conf..129M Altcode: No abstract at ADS Title: 3D Finite Volume Simulation of Accretion Discs with Spiral ShocksCD Authors: Makita, M.; Matsuda, T. Bibcode: 1999ASSL..240..227M Altcode: 1999numa.conf..227M; 1998astro.ph..7237M We perform 2D and 3D numerical simulations of an accretion disc in a close binary system using the Simplified Flux vector Splitting (SFS) finite volume method. In our calculations, gas is assumed to be the ideal one, and we calculate the cases with gamma=1.01, 1.05, 1.1 and 1.2. The mass ratio of the mass losing star to the mass accreting star is unity. Our results show that spiral shocks are formed on the accretion disc in all cases. In 2D calculations we find that the smaller gamma is, the more tightly the spiral winds. We observe this trend in 3D calculations as well in somewhat weaker sense. Title: Spiral Shocks in Accretion Discs: Comparing models with observations Authors: Makita, M.; Yukawa, H.; Matsuda, T.; Boffin, H. M. J. Bibcode: 1999dicb.conf..147M Altcode: No abstract at ADS Title: The Proper Motion of Individual Sunspots Authors: Herdiwijaya, Dhani; Makita, Mitsugu; Anwar, Bachtiar Bibcode: 1997PASJ...49..235H Altcode: The proper motions of 276 individual sunspots were observed with a triple-exposures method, and then analyzed. Their linear drifts give the mean motions (degree day(-1) ), which, depending on the heliographic latitude B, are the differential rotation, omega (B) = 14.5 - 2.5sin (2B) , and the equatorward meridional flow, v_B =-0.05sin 2B. The deviations of the linear drift from the mean motions have a small correlation between the longitudinal and latitudinal ones, which correspond to the equatorial acceleration. The deviations in longitude are clearly separated by the sunspot polarities. The average separation velocity between the preceding and following polarities is 52 m s(-1) . The drifts of individual sunspots corrected for the mean motion are the smallest for the Zurich GHJ class. However, they are fairly large and may influence the determination of the mean motion. Short-term variations appear as positional deviations from the linear-drift curve. These fast drifts are detected in the active Zurich classes, and are one order of magnitude larger than the linear drift. Title: Distributions of the Magnetic Field Inclination in Sunspots Authors: Shinkawa, T.; Makita, M. Bibcode: 1996mpsa.conf..615S Altcode: 1996IAUCo.153..615S No abstract at ADS Title: Rapid Sunspot Motion during a Major Solar Flare Authors: Anwar, B.; Acton, L. W.; Hudson, H. S.; Makita, M.; McClymont, A. N.; Tsuneta, S. Bibcode: 1993SoPh..147..287A Altcode: A major solar flare on 15 November, 1991 produced a striking perturbation in the position and shape of the sunspot related most closely to the flare. We have studied these perturbations by use of the aspect-sensor images from the Soft X-ray Telescope on board YOHKOH, and with ground-based data from the Mees Solar Observatory. The perturbation occurred during the impulsive phase of the flare, with a total displacement on the order of 1 arc sec. The apparent velocity of approximately 2 km s−1 exceeds that typically reported for sunspot proper motions even in flare events. We estimate that the magnetic energy involved in displacing the sunspot amounted to less than 4 × 1030 ergs, comparable to the radiant energy from the perturbed region. Examination of the Mees Observatory data shows that the spot continued moving at lower speed for a half-hour after the impulsive phase. The spot perturbation appears to have been a result of the coronal restructuring and flare energy release, rather than its cause. Title: Magnetograph Observations of Solar Faculae Authors: Kawakami, Singo; Makita, Mitsugu Bibcode: 1993PASJ...45..255K Altcode: Two solar facular regions were investigated using the Solar Vector Magnetograph of the Okayama Astrophysical Observatory. The transverse magnetic field of the faculae becomes more parallel to the solar radius as the facular region moves from the disk center to the limb. This center-to-limb variation can be explained by a numerical simulation in which the direction of facular magnetic fields is confined within a cone around the vertical. A suitable cone angle is about 30(deg) . This confinement leads to the possibility of calibrating a magnetograph measurement by considering the center-to-limb variation of the longitudinal and transverse magnetic fields. Title: Effective Lande factors of the solar spectral lines in 5000 Å - 7000 Å and sunspot magnetic fields. Authors: Makita, M.; Yatagai, H.; Nakamura, K.; Fujikawa, T.; Hirose, S. Bibcode: 1993MmKyo..38..255M Altcode: The effective Lande factors of the solar spectral lines in the wavelength region 5000 - 7000 Å are tabulated. As an application of this table, sunspot spectra are analyzed to statistically determine the magnetic field strength. Title: Ten Years of the Okayama Vector Magnetograph Authors: Makita, M.; Sakurai, T.; Shibasaki, K.; Koyano, H. Bibcode: 1993ASPC...46..180M Altcode: 1993IAUCo.141..180M; 1993mvfs.conf..180M No abstract at ADS Title: Polarization of the Domeless Solar Telescope of the Hida Observatory (Preliminary report). Authors: Makita, M.; Funakoshi, Y.; Hanaoka, Y. Bibcode: 1991sopo.work..198M Altcode: Instrumental polarization of the Domeless Solar Telescope (DST) are measured with an accuracy of 1 per cent. The variation of the Stokes parameters from sunrise to sunset is reproduced by adopting probable optical constants for the two oblique reflection mirrors in the telescope. The entrance and exit vacuum windows affect the polarization less than the measured accuracy. Title: Active regions, sunspots and their magnetic fields. Authors: Semel, Meir; Mouradian, Zadig; Soru-Escaut, Irina; Maltby, Per; Rees, David; Makita, Mitsugu; Sakurai, Takashi Bibcode: 1991sia..book..844S Altcode: Surface magnetism is the progenitor of active regions, sunspots, and all related phenomena. This cause and effect is reversible so that, using well-established empirical laws, the presence and morphology of photospheric magnetic fields can be deduced from active-region light emission structure. In the (simplifying) case of sunspots, MHD and thermodynamic theory find some success in the interpretation of the interaction of magnetic fields and solar plasma. Coronal magnetic fields also appear to be predictable by extrapolation techniques starting from the photospheric conditions. Alternatively, surface magnetism can be observed "directly" by means of the spectroscopic Zeeman effect and Stokes polarimetry. Eventually these empirical, theoretical and direct-measurement techniques must converge to identical results as we better understand the physics of active regions. Title: Detailed comparison of transverse magnetic fields of the sun with H-alpha fine structures Authors: Kawakami, Singo; Makita, Mitsugu; Kurokawa, Hiroki Bibcode: 1989PASJ...41..175K Altcode: Vectormagnetograms obtained at the Okayama Astrophysical Observatory are compared in detail with H-alpha filtergrams taken with the Domeless Solar Telescope at Hida Observatory for three active regions. The coincidence rate between the azimuth of transverse magnetic fields and elongated H-alpha dark fine structures decreases as the active region moves on the solar disk from the center to the limb. This center-to-limb variation of the azimuthal coincidence rate can be explained by the difference of elevation angle between the photospheric and chromospheric magnetic fields. The analysis of three active regions shows that, in a more active region, the magnetic field is more inclined in the photosphere, and more sheared in the vertical direction. Three active regions show different values of the azimuthal coincidence rate, and these differences are discussed in connection with the magnetic field configuration and the evolutional characteristics of the individual active regions. Title: On the structure of the sunspot magnetic field deduced from broadband circular polarization Authors: Makita, Mitsugu Bibcode: 1988VA.....31...63M Altcode: The characteristics of the broad-band circular polarization of sunspots are confirmed for sunspots of the new solar cycle. It is stronger on the limb-side of sunspots and its polarity is always positive (negative) for S (N) magnetic polarity in three recent solar cycles. The sunspot model of an unwinding emerging magnetic field proposed in the previous analysis is illustrated. Title: An experiment on the relation between incident and emerging light beams of optical fibers. Authors: Makita, M.; Imai, H. Bibcode: 1988TokRe..21..129M Altcode: No abstract at ADS Title: Measurement of the magnetic vector on the sun at the Okayama Astrophysical Observatory. Authors: Makita, Mitsugu; Hamana, Shigeo; Sakurai, Takashi; Shimizu, Minoru Bibcode: 1987LIACo..27..185M Altcode: 1987oahp.proc..185M Observations taken in Japan beginning in 1982 have been used to obtain magnetic vectors on the sun. Investigation of drift curves of the measured polarization shows that the residual instrumental polarization can be represented by trigonometric functions of twice the sun's hour angle. Peak-to-peak amplitudes of fluctuations in the line wing (5250 A) and in the neighboring continuum (5282-5297 A) are 0.0041 and 0.0001 respectively. The observed radial velocity drifts linearly at the rate of about 0.2 to 1 km/s/hr. It is suggested that corrections could give the accuracy of 10 m/s. Title: An Interpretation of the Broad Band Circular Polarization of Sunspots Authors: Makita, Mitsugu Bibcode: 1986SoPh..106..269M Altcode: The broad-band circular polarization of sunspots is discussed on the basis of the observations made in the Okayama Astrophysical Observatory. The observation with the spectrograph proves that it is the integrated polarization of spectral lines in the observed spectral range. A velocity gradient in the line-of-sight can produce this integrated polarization due to the differential saturation between Zeeman components of magnetically sensitive lines. The observed degree of polarization and its spatial distribution in sunspots is explained when we introduce a differentially twisted magnetic field in addition to the velocity gradient. The differential twist has the azimuth rotation of the magnetic field along the line-of-sight and generates the circular polarization from the linear polarization due to the magneto-optical effect. The required azimuth rotation is reasonable and amounts at most to 30°. The required velocity gradient is compatible with the line asymmetry and its spatial distribution observed in sunspots. The observed polarity rule leads to the conclusion that the sunspot magnetic field has the differential twist with the right-handed azimuth rotation relative to the direction of the main magnetic field, without regard to the magnetic polarity and to the solar cycle. The twist itself is left-handed under the photosphere, when the sunspot is assumed to be a unwinding emerging magnetic field. Title: A Detection of the Faraday Rotation by the Solar Vector Magnetograph Authors: Makita, M. Bibcode: 1986SoPh..103....1M Altcode: The Faraday rotation in the sunspot atmosphere is statistically detected by examining directions of the linear polarization obtained with the vector magnetograph of the Okayama Astrophysical Observatory. It is very effective near the spectral line center and the azimuth of the linear polarization deviates greatly from the magnetic field azimuth. In the case of the iron line, 5250 Å, the magnetic field azimuth will be obtained with an accuracy better than 15°, if observed in the line wing from 27 to 80 mÅ relative to the line center. Title: The broad-band polarization of sunspots observed from 8 February 1981to 30 August 1982. Authors: Makita, Mitsugu; Ohki, Yoshina Bibcode: 1986AnTok..21....1M Altcode: 1986AOTok..21....1M The broad-band polarization of sunspots was measured with the polarimeter fed to the solar coudé telescope of the Okayama Astrophysical Observatory. 113 polarization maps of 41 sunspot groups were obtained during this period. The observed circular polarization is strong in the limb of sunspots, roughly in proportion to the linear polarization. Its polarity is negative or positive according as the magnetic polarity is north or south. This polarity rule is found to be the same as that in the previous solar cycle. Title: A study of line asymmetry in unipolar sunspots Authors: Makita, M.; Kawakami, H. Bibcode: 1986PASJ...38..257M Altcode: The asymmetry of the line profile of Fe I (6301.5 A) in the spectrum of unipolar sunspots was analyzed. Most bisectors of the line profile could be approximated by straight lines and interpreted in terms of the variation of the line-of-sight velocity. The analysis of these bisectors, under the assumption of cylindrical symmetry, gives a sunspot-velocity structure consistent with that deduced from the Evershed outflow and inflow. The azimuthal flow increases downward to satisfy the vorticity-polarity rule proposed by the Meudon observers (Matries et al., 1973). Among the line profiles not approximated by the linear bisector, inverse-C shape profiles are most likely to occur in the umbra. Title: Observation of Magnetic Field Vector in Solar Active Regions Authors: Sakurai, T.; Makita, M. Bibcode: 1986hmps.conf...53S Altcode: No abstract at ADS Title: Solar vector magnetograms of the Okayama Astrophysical Observatory. Authors: Makita, M. Bibcode: 1986saot.conf..237M Altcode: The solar vector magnetograph of the Okayama Astrophysical Observatory has been operated since the end of 1982. The observational data usually obtained are briefly described. Title: Solar Vector Magnetograms of the Okayama Astrophysical Observatory Authors: Makita, Mitsugu; Hamana, Shigeo; Nishi, Keizo; Shimizu, Minoru; Sakurai, Takashi; Shibasaki, Kiyoto Bibcode: 1986Ap&SS.118..163M Altcode: The title instrument is mounted on the 65 cm solar Coudé telescope at the Okayama observatory. Observation is usually of the Fe i 5250 Å line. The data obtained are briefly described. Title: Observation of Magnetic Field Vector in Solar Active Regions Authors: Sakurai, T.; Makita, M.; Shibasaki, K. Bibcode: 1985tphr.conf..313S Altcode: The vector magnetograph at Okayama Astrophysical Observatory has been in operation since 1982. The conversion from the observed polarization degrees to the magnetic field components is made by using Unno's formula (1956) applied to a homogeneous magnetic field. Title: Comparisons of simultaneous vector magnetograms Authors: Makita, M.; Nishi, K.; Shimizu, M.; Hamana, S.; Sakurai, T.; Grigoryev, V. M.; Kuklin, G. V.; Selivanov, V. L. Bibcode: 1985svmf.nasa..399M Altcode: Simultaneous vector magnetograms were obtained with the different magnetographs of the Okayama Astrophysical Observatory and the Sayan Mountain Observatory in October 1983. The data obtained show a good correspondence in general. The comparison makes clear something on the measuring accuracy of each magnetograph. Good correspondence is shown in circular and linear polarizations, and, in and near sunspots, of the velocity field. The azimuth of the magnetic fields show good agreement. Title: The solar vector magnetograph of the Okayama Astrophysical Observatory Authors: Makita, M.; Hamana, S.; Nishi, K. Bibcode: 1985svmf.nasa..173M Altcode: The vector magnetograph of the Okayama Astrophysical Observatory is fed to the 65 cm solar coude telescope with a 10 m Littrow spectrograph. The polarimeter put at the telescope focus analyzes the incident polarization. Photomultipliers (PMT) at the exit of the spectrograph pick up the modulated light signals and send them to the electronic controller. The controller analyzes frequency and phase of the signal. The analyzer of the polarimeter is a combination of a single wave plate rotating at 40 Hz and a Wallaston prism. Incident linear and circular polarizations are modified at four times and twice the rotation frequency, respectively. Two compensators minimize the instrumental polarization, mainly caused by the two tilt mirrors in the optical path of the telescope. The four photomultipliers placed on the wings of the FeI 5250A line give maps of intensity, longitudinal field and transverse field. The main outputs, maps of intensity, and net linear and circular polarizations in the neighboring continuum are obtained by the other two monitor PMTs. Title: The solar vector magnetograph of the Okayama Astrophysical Observatory. Authors: Makita, M.; Hamana, S.; Nishi, K. Bibcode: 1985NASCP2374..173M Altcode: The vector magnetograph of the Okayama Astrophysical Observatory is fed to the 65 cm solar coudé telescope with a 10 m Littrow spectrograph. The polarimeter put at the telescope focus (solar image size = 31 cm) analyzes the incident polarization. Photomultipliers (PMT) at the exit of the spectrograph pick up the modulated light signals and send them to the electronic controller. The controller makes frequency and phase analyses of the signal, and the results are digitized and stored on the magnetic disk of the mini-computer. The operation of the complete vector magnetograph became possible in autumn 1982. Some preliminary data mainly on solar active regions were published recently (Sakurai and Makita, 1984). Title: Comparisons of simultaneous vector magnetograms. Authors: Makita, M.; Nishi, K.; Shimizu, M.; Hamana, S.; Sakura, T.; Grigoryev, V. M.; Grigor'ev, V. M.; Kuklin, G. V.; Selivanov, V. L. Bibcode: 1985NASCP2374..399M Altcode: Simultaneous vector magnetograms were obtained with the different magnetographs of the Okayama Astrophysical Observatory and the Sayan Mountain Observatory in October 1983. The data obtained show a good correspondence in general. The comparison makes clear something on the measuring accuracy of each magnetograph. Title: Observations by the solar vector magnetograph of the Okayama Astrophysical Observatory. Authors: Makita, M.; Hamana, S.; Nishi, K.; Shimizu, M.; Koyano, H.; Sakurai, T.; Komatsu, H. Bibcode: 1985PASJ...37..561M Altcode: 1985PASJ...37..561H The vector magnetograph of the Okayama Astrophysical Observatory has been in operation since the fall of 1982. The instrument, operation, and data reduction are described briefly. Some observations of the development of a small active region, a flare, and azimuths of the magnetic field relative to the Hα fine structure are reported. The accuracy of the measurement is limited by the incident photon number and as good as 0.1 % in the degree of polarization. Title: Observation of magnetic field vector in solar active regions. Authors: Sakurai, T.; Makita, M.; Shibasaki, K. Bibcode: 1985MPARp.212..312S Altcode: The vector magnetograph at Okayama Astrophysical Observatory has been in operation since 1982. The conversion from the observed polarization degrees to the magnetic field components is made by using Unno's formula (1956) applied to a homogeneous magnetic field. Title: A solar vector magnetograph. Authors: Makita, M. Bibcode: 1983AstHe..76..284M Altcode: No abstract at ADS Title: Magnetic and Velocity Fields of Emerging Flux Regions on the Sun Authors: Martres, M. J.; Rayrole, J.; Semel, M.; Soru-Escaut, I.; Tanaka, K.; Makita, M.; Moriyama, F.; Unno, W. Bibcode: 1982PASJ...34..299M Altcode: Emerging Flux Regions (EFR's) on the Sun observed in the Meudon-Mitaka Collaborative Solar Observation Program (1979) are discussed.

The rule found earlier (Martres et al. 1973) for the growth (or decay) of the N polarity or the decay (or growth) of the S polarity magnetic field in relation to the photospheric clockwise (or counterclockwise) vortex motion is reconfirmed for the EFR in the present solar cycle. The rule is emphasized as an indication of active generation of an electric current system by a photospheric motion.

The chromospheric manifestations of EFR's seen in Hα as arch filament systems (AFS's) and the enhanced brightness are examined with respect to the photospheric magnetic field structure derived from the white light and magnetic observations. An isolated EFR is associated with an AFS which is well coaligned with the photospheric transverse field. The typical EFR configuration may be distorted if the EFR appears in the region of the pre-existing strong field. The observational characteristics of such EFR's can also be interpreted in terms of the emergence of a nearly potential field associated with the dissipation of an excess magnetic energy. An EFR born in an older EFR shows that the flux loop is low-lying and tends to relax into a potential field configuration. Title: High accuracy measurement of the instrumental polarization of the solar coudé telescope at the Okayama Astrophysical Observatory. Authors: Makita, M.; Hamana, S.; Kawakami, H.; Nishi, K. Bibcode: 1982AnTok..19...24M Altcode: 1982AOTok..19...24M No abstract at ADS Title: Wide-Band Polarization of Sunspots Authors: Makita, M. Bibcode: 1980jfss.conf...99M Altcode: No abstract at ADS Title: Three Component Magnetic Fields of Sunspots Authors: Kawakami, H.; Makita, M. Bibcode: 1980jfss.conf..107K Altcode: No abstract at ADS Title: Determination of the Magnetic Field from the Zeeman Line Profile Authors: Makita, M. Bibcode: 1979PASJ...31..575M Altcode: A method applying the theoretical solution of the radiative transfer problem with the magnetic field to the observed Zeeman line profile is developed. The assumptions of a pure-absorption atmosphere and of no magneto-optical effect allow a model-free determination of the magnetic field averaged along the optical depth. Depth variation of line-profile parameters, such as the Doppler shift, Doppler width, damping constant, magnetic field strength, and tilt of the magnetic line of force, is obtained.

The present method of analysis is applied to a penumbral spectrum observed on May 10, 1971 and has shown an inward magnetic field, whose strength is 1500 G, making an angle of 34° against the solar surface, and an outward Evershed flow of 5.6 km s-1, parallel to the magnetic line of force. Title: The effective optical depth for the formation of absorption lines. Authors: Makita, M. Bibcode: 1977SoPh...51...43M Altcode: The contribution function method used so far to define the effective depth for the formation of absorption lines is discussed and a new definition of the effective depth is proposed. The effective depth is the level where a thin slab having the equivalent optical thickness to the total line absorption is placed so as to give the observed line intensity. Title: Magnetic field gradient in a sunspot umbra. Authors: Makita, M.; Nemoto, K. Bibcode: 1976PASJ...28..495M Altcode: Echelle spectrograms of three sunspot umbrae were obtaiaed with a wide wavelength-range analyzer of the circular polarization at the Okayama Astrophysical Observatory. The magnetic field derived from the Zeeman shift of many absorption lines cannot be interpreted by a single spectrum, but suggests a composite of two spectra, one of which is due to a cool atmosphere with magnetic field and the other due to a hot atmosphere without magnetic field. The hot component can be attributed to the stray light due to the seeing or to umbral structure, or both. The analysis, taking into account the composite nature, leads to a magnetic field gradient of G . A reanalysis of 's (1969) data, obtained also with the cchelle spectrograph, gives JH/dk >-0.7 G km-1. Key words: Echelle spectrum; Magnetic field; Sunspot. Title: Measurements of the Magnetic Field Vector of a Sunspot Authors: Nishi, K.; Makita, M. Bibcode: 1973PASJ...25...51N Altcode: A new polarimetric observation of the Fraunhofer line 6302.5A was made along the line profile considering the reduction of the instrumental polarization. The existence of a nearly horizontal magnetic field in the penumbra was confirmed. It was also found that the field direction was along the filamentary structure of the penumbra. Key words: Magnetic field; Polarization; Sunspots. Title: The Chromosphere in Continuum Emission Observed at the Total Solar Eclipse on 7 March 1970 Authors: Makita, Mitsugu Bibcode: 1972SoPh...24...59M Altcode: Direct images of the Sun were photographed in continuum emission centered at 6900 Å by the jumping film method near the second contact of the Mexico eclipse on 7 March 1970. The band width was 150 Å defined by a combination of a sharp cut filter and KODAK IV F film. The intensity distribution of the solar outer layers obtained shows a steep decrease by a factor of 0.9 in logarithmic units around 2500 km. This is interpreted as the boundary of the chromosphere and corona. Spicules observed at 3500 km are explained by log ne = 11.25 and Te ≈ 6000 K. Discussions are made in relation to the other observations and some chromosphere models. Title: The preliminary report of the observations of the March 7, 1970 total solar eclipse in Mexico. Authors: Saito, K.; Makita, M.; Hata, S.; Tojo, A. Bibcode: 1971TokRe..15..445S Altcode: No abstract at ADS Title: A polarization compensator designed for the solar coudé telescope at the Okayama Astrophysical Observatory. Authors: Makita, M. Bibcode: 1970AnTok..12..139M Altcode: 1970AOTok..12..139M No abstract at ADS Title: Instrumental polarization of the solar coudé telescope and spectrograph at the Okayama Astrophysical Observatory. Authors: Makita, M.; Nishi, K. Bibcode: 1970AnTok..12..121M Altcode: 1970AOTok..12..121M No abstract at ADS Title: A non-spherical axisymmetric model of the solar K corona of the minimum type Authors: Saito, Kuniji; Makita, Mitsugu; Nishi, Keizo; Hata, Shigeru Bibcode: 1970AnTok..12...53S Altcode: 1970AOTok..12...53S; 1970AnTok..12...51S No abstract at ADS Title: A Study of the Green TiO Band in the Sunspot Spectrum Authors: Makita, Mitsugu Bibcode: 1968SoPh....3..557M Altcode: The equivalent widths of the TiO lines in the α system have been measured on a high dispersion (11 mm/Å) spectrogram of large sunspot. The lines were so weak that the measurement was made by methods giving maximum and minimum equivalent widths, depending on the adopted continuum. The rotational temperature obtained in this way was about 3000 °K. The result is unaffected by stray light because there are no TiO lines in the undisturbed spectrum. The calculation of equivalent widths using several sunspot models (all of which can satisfy the observed data) shows that the logarithmic optical depth at the effective layer of molecular line formation is about -1.6. Title: The Scattering Function Obtained from Partial Solar Eclipse Authors: Makita, M. Bibcode: 1966PASJ...18..345M Altcode: The direct image of the sun was photographed at a partial solar eclipse, and from the moon's limb occulting the solar disk the profile of the scattering function was obtained. The profiles thus obtained do not fit a Gaussian. Near the core they look like a dispersion function, but in the wing they decrease faster than this. The working hypothesis of the preceding paper that the scattering function is the sum of two Gaussian profiles seemes to be a goed approximation. Title: On the two component model of sunspot umbrae Authors: Makita, M. Bibcode: 1964susp.conf..177M Altcode: No abstract at ADS Title: The Effect of Atmospheric Turbulence on the Solar Image and Sunspots Authors: Makita, M.; Morimoto, M. Bibcode: 1964PASJ...16....1M Altcode: On the basis of the photoelectric and photographic observations of the solar limb and sunspots, the shape of the scattering function is discussed and the pro posal is made that it is the sum of two Gaussian functions. The result does not change the previous condusion that the atmosphere of the sunspot umbra consists of two components, one hot and the other cold. The photoelectric observations give some information as to the size, frequency spectrum, and dependence of the atmospheric turbulence and, moreover, as to the correlations between the atmospheric turbulence and weather and between observations made with different instruments. Title: Physical States in Sunspots Authors: Makita, M. Bibcode: 1963PASJ...15..145M Altcode: The physical state in sunspots were studied by the line spectra, which were obtained photographically with the tower telescope of the Tokyo Astronowical Observatory, combined with the temperature distribution obtained by the photoelectric method reported in the previous paper. Throughout the study only the ratio of photospheric and sunspot equivalent widths was discussed, because it is independent of the abundance of the element and gf-value and, therefore, one can use many unblended weak lines, for which the equivalent widths can casily be calculated on the basis of pure absorption. The procedure was to find the temperature and electron pressure distributions in sunspots which give best fit to the observed ratios. The model of the penumbra obtained has the following properties; 1) It is nearly in radiative equilibrium of the plain parallel atmosphere, 2) It is about two times transparent than the photosphere, 3) It departs from hydrostatic equilibrium, but this can be explained by the reasonable magnetic field parallel to the Evershed flow, and 4) It balances the surrounding photosphere by the Evershed flow. As far as the uniform model is assumed, no consistent model could be found in the case of the umbra because of the presence of too high excitation lines, which led to very low values of pressure in deep layers and required the unreasonable magnetic and velocity flelds in order for the mechanical balance to attain horizontally and vertically. Mter some discussions the two component model having the following properties was proposed; 1) The high excitation lines are chiefly formed in the hot component of the atmosphere composed of the cold and hot components, 2) The two components are both in hydrostatic equilibrium, 3) The hot component occupies about one tenth of the umbra in area and emits about half of the total radiation at 5000A, and 4) The radiation temperatures of both components are about and . Title: Photoelectric Study of Sunspots Authors: Makita, M.; Morimoto, M. Bibcode: 1960PASJ...12...63M Altcode: The continuum of sunspot spectra was observed simultaneously at three wave lengths with the tower telescope of the Tokyo Astronomical Observatory, using the photoelectric and the rotating prism which reduced the effect of scintillation appreciably. The intensity ratio to area relation and the limb effect of sunspots are obtained and from the latter the temperature distribution is derived for the penumbra an the umbra ( and at .5 respectively). The obtained temperature distribution of the umbra with the area=70.10-6 of solar hemisphere is on the average lower than Michard's. Title: Convective Instability in Polytropic Atmospheres, I Authors: Unno, W.; Kato, S.; Makita, M. Bibcode: 1960PASJ...12..192U Altcode: The condition of the onset of thermal convection is studied for polytropic atmospheres in which both the coefficients of viscosity and thermal conductivity are assumed to be constant. A polytropic variation for the disturbance is assumed for simplicity, and the non-dimensional number, crit, characterizing the condition of marginal stability is computed for the most unstable mode with the use of the variational principle. Actual computations have been made for a few polytropic atmospheres having considerable changes in density from top to bottom. The results are compared to those of the classical Rayleigh problem, and it turns out that the critical Rayleigh number Rcrot, and the associated horizontal wavenumber depend very little on the density variation in the atmosphere, provided that the transformation from crit to Rcrot is made with the use of the density and temperature at the average height in the atmosphere. The effect of the simplifying assumption of polytropic variation on the above argument will be examined in a subsequent paper in which the effect is found to be unimportant. Title: Inhibition of Convection by a Magnetic Field Authors: Makita, M. Bibcode: 1958PASJ...10....1M Altcode: The stability of the stellar atmosphere in the presence of a magnetic field is considered using the usual hydrornagnetic equations. It i that initiallv the magnetic field is homogeneous and the atmosphere is hydrostatic We can derive the extended Wale n's criterion neglecting higher order disturbances than the second. The criterion is applied to the solar convection zone and 200 gauss is obtained for the magnetic field strength of penumbra.