Author name code: suemoto ADS astronomy entries on 2022-09-14 author:"Suemoto, Zenzaburo" ------------------------------------------------------------------------ Title: In memoriam Authors: Suemoto, Zenzaburo; Hiei, E.; Uchida, Y. Bibcode: 1993SoPh..146..203S Altcode: No abstract at ADS Title: Continuous and Line Spectra of Granules and Intergranular Lanes Authors: Suemoto, Z.; Hiei, E.; Nakagomi, Y. Bibcode: 1990SoPh..127...11S Altcode: Temperature and velocity structures above granules and intergranular lanes were studied on spectrograms covering CaII H and K lines. In agreement with our earlier results, it was confirmed more quantitatively that there appear two kinds of bright continua, one in the outer wings (granular continuum) and the other in the inner wings (temporarily called K0-continuum) of CaII H and K lines, and that these two kinds of bright continua are located more or less in a complementary fashion. Further, it was found that the bright K0-continuum is well associated with higher central residual intensity of absorption lines. These facts suggest that in the upper photosphere of, say, τ < 0.1, there are high temperature regions in the intergranular lanes. Motions above granular regions are essentially upwards, whereas those of intergranular regions are predominantly downwards, and in the uppermost photosphere the motions become more random. Title: Bright Features in the Intergranular Region Authors: Suemoto, Z.; Hiei, E. Bibcode: 1990IAUS..138...97S Altcode: No abstract at ADS Title: Bright threads in the inner wing of solar Ca II H and K lines. Authors: Suemoto, Zenzaburo; Hiei, Eijiro; Nakagomi, Yoshiteru Bibcode: 1988sscd.conf..282S Altcode: On spectrograms of the H and K lines at quiet regions of the Sun, bright threads visible in the real continuum due to the granulations are also seen in the outer wings as far as |Δλ| ≡ 3 A from the K line centre. At the inner wings (3 A ⪆ |Δλ| ⪆ 0.5 A in the K line) bright threads are also seen, but their spatial distribution is different from the former ones. The threads at the inner wings appear at the intergranular regions, and many of them are seen inside the supergranulation. These facts reflect that the granular high temperature layer stops penetrating at a certain height in the photosphere, and that the intergranular bright threads at the inner wings are due to a hotter temperature layer, located at a considerably higher photospheric layer than the granulation. Title: Bright threads in the inner wing of solar Ca II K line Authors: Suemoto, Z.; Hiei, E.; Nakagomi, Y. Bibcode: 1987SoPh..112...59S Altcode: On spectrograms of the K line at quiet regions of the Sun, bright threads visible in the real continuum due to the granulations are also seen in the outer wing as far as ¦Δλ¦ ∼ 3 Å from the line centre. At the inner wing (3 Å ≳ ¦Δλ¦ ≳ 0.5 Å) bright threads are also seen, but their spatial distribution is different from the former ones. The threads at the inner wing appear at intergranular regions, and many of them are seen inside the supergranulation. Their size and number density are about the same as those of the granulation. These facts reflect that the penetration of the granular high temperature layer stops at a certain height in the photosphere, and that the intergranular bright threads at the inner wing are due to a hotter temperature layer, located at a considerably higher photospheric layer than the granulation. Title: Time and Latitude Bulletins. October 1979 - June 1980. Authors: Suemoto, Z. Bibcode: 1980TokAT..53...45S Altcode: No abstract at ADS Title: International Time and Latitude Service at the Tokyo Astronomical Observatory during 1979. Authors: Suemoto, Z. Bibcode: 1979TokAT..53....1S Altcode: No abstract at ADS Title: International Time and Latitude Service at the Tokyo Astronomical Observatory 1979. Authors: Suemoto, Z. Bibcode: 1979TokAT..53...33S Altcode: No abstract at ADS Title: International Time and Latitude Service at the Tokyo Astronomical Observatory during 1978. Authors: Suemoto, Z. Bibcode: 1978TokAT..52....1S Altcode: No abstract at ADS Title: An empirical, statistical model for the formation of the cores of chromospheric Fraunhofer lines. Authors: Suemoto, Z. Bibcode: 1977SoPh...54....3S Altcode: We describe an empirical, statistical model for the formation of the cores of chromospheric Fraunhofer lines. The model chromosphere consists of brighter structural elements with large scale motions randomly distributed in space, and above these, darker structural elements, again randomly distributed in space. Both components overlie a more uniform lower chromosphere. The probability of finding a given number of elements along a line of sight is specified by a Poisson distribution, in terms of the average number of structures along the line of sight. When this average is small, the statistical model may behave like an effectively thin plane-parallel chromosphere, even when the optical thickness of the individual structures is very large. Title: International Time and Latitude Service at the Tokyo Astronomical Observatory during 1977. Authors: Suemoto, Z. Bibcode: 1977TokAT..51...31S Altcode: No abstract at ADS Title: Observations of the solar ultraviolet Mg II doublet. III. Authors: Kohno, T.; Yajima, N.; Suemoto, Z. Bibcode: 1977BISAT..13..799K Altcode: No abstract at ADS Title: International Time and Latitude Service at the Tokyo Astronomical Observatory during 1977. Authors: Suemoto, Z. Bibcode: 1977TokAT..51....1S Altcode: No abstract at ADS Title: Infrared spectral observations of stars. II. Authors: Tanaka, W.; Kodaira, K.; Tsuji, T.; Onaka, T.; Nagai, T.; Watanabe, T.; Suemoto, Z.; Yajima, N.; Kono, T.; Ota, S.; Koma, Y. Bibcode: 1977BISAT..13..813T Altcode: No abstract at ADS Title: Near-infrared photometry of late-type stars with balloon-borne telescope. Authors: Kodaira, K.; Tanaka, W.; Onaka, T.; Nagai, T.; Watanabe, T.; Suemoto, Z. Bibcode: 1976TokAB.245.2077K Altcode: 1976BTok..245.2077K Balloon-borne observations were made from an altitude of 25 km approximately 120 km off the coast of northeastern Japan. The balloon then drifted westward across Japan island, taking near-infrared readings of late stars with a Reticon matrix camera as it went. Alpha-Aql was used as a reference for photometric comparison. Attention is given to observations of alpha-Boo, alpha-Sco, and alpha-Her. Title: Infrared spectral observations of stars. Authors: Komaki, K.; Kodaira, K.; Tanaka, W.; Suemoto, Z. Bibcode: 1976BISAT..12..623K Altcode: No abstract at ADS Title: Observation of the centre-to-limb variations of the Sun in the vacuum ultraviolet region. Authors: Nishi, K.; Higashi, K.; Yamaguchi, A.; Suemoto, Z. Bibcode: 1976BISAT..12..959N Altcode: No abstract at ADS Title: Observation of the solar ultraviolet Mg II doublet, (2). Authors: Yajima, N.; Kohno, T.; Suemoto, Z. Bibcode: 1974TDUKK..10..174Y Altcode: No abstract at ADS Title: Observation of the solar ultraviolet Mg II doublet, (1). Authors: Kohno, T.; Yajima, N.; Suemoto, Z. Bibcode: 1974TDUKK..10..166K Altcode: No abstract at ADS Title: Attempts to Observe the Absolute Intensity and the Centre-To Variations of the Sun in the Vacuum Ultraviolet Region Authors: Nishi, K.; Suemoto, Z. Bibcode: 1971IAUS...41..393N Altcode: No abstract at ADS Title: A Measurement of the Solar H and K Profiles Authors: White, O. R.; Suemoto, Z. Bibcode: 1968SoPh....3..523W Altcode: A new series of photometric observations of the H and K lines were obtained at Sacramento Peak Observatory in 1964 and 1965. In both the observations and the data reduction special attention was given to obtaining a suitable average over the solar fine structure and to defining a proper reference continuum. The results are that the central intensities of H and K are the same and equal to 4.2% of the continuum. The limb-darkening curves at the line centres are also the same for both lines. Title: Interpretation of K Emission Line Profile Authors: Suemoto, Zenzaburo Bibcode: 1966PJAB...42..777S Altcode: No abstract at ADS Title: Spotty appearance of the solar disk as inferred from the comparison between E. U. V. and radio intensities Authors: Suemoto, Z.; Moriyama, F. Bibcode: 1965IAUS...23..109S Altcode: No abstract at ADS Title: Spotty appearance of the solar disk as inferred from the comparaison between EUV and radio intensities Authors: Suemoto, Z.; Moriyama, F. Bibcode: 1964AnAp...27..775S Altcode: No abstract at ADS Title: Turbulence in the Chromosphere Authors: Suemoto, Z. Bibcode: 1963PASJ...15..531S Altcode: Turbulence velocities in the &nromosphere were determined from the base up to 10,000 km. Measurement was made on flash spectrograms of 1958 eclipse in South Pacific. The dispersion was about 2.3 A/mm and the resolution in terms of velocity was 2-3 km/sec in most probable velocity s. Above 2000 km measuremeat was made referring to a number of individual spicules or groups of spicules. The velocity was determined by the multiplet method and is free from saturation effect, although precautions were paid not to use very saturated lines. The velo city first increases from 2-3 km/sec to 17 km/sec as we ascend from 0 km up to 2000 km, and then remains constant up to the highest level of 10,000 km. The random velocity within each spicule was estimated to be less than 7 km/sec. The velocity 17 km/sec would be representative of the ascending and descending motion of the spicule. In fact about the same velocity was obtained by measuring the line shift at the highest levels. This velocity is about three times larger than the velocity deduced from the analysis of K reversal. In order to elucidate this disagreement a new interpretation of K reversal was proposed. This is to understand the K line profile as an algebraic sum of the two different kinds of spectra, one an absorption line spectrum with a sharp absorption core and the other an emission line spectrum without a central absorption. The latter spectrum comes from spicules and the former comes from the top of the photosphere. In short, chromosphere consists of spicules down to zero km and these spicules cover the photosphere only in patches and elsewhere we are observing the bare top of the photosphere above which there is no spicule. Some remarks are also given on hydrogen and helium line widths. Title: Interpretation of Solar Extreme Ultraviolet Spectra Observed with Rockets from a New Model of the Solar Chromosphere Authors: Suemoto, Z.; Moriyama, F. Bibcode: 1963spre.conf..800S Altcode: No abstract at ADS Title: A New Model of the Chromosphere Authors: Suemoto, Zenzaburo Bibcode: 1963PJAB...39..463S Altcode: No abstract at ADS Title: Observation of the Flash Spectrum at the Total Solar Eclipse of October 12, 1958 Authors: Suemoto, Z.; Hiei, E. Bibcode: 1962PASJ...14...33S Altcode: In 1958 eclipse in South Pacific, we observed the flash spectrum with a slitless spectrograph, but with the grating used very obliquely. Because of the minifying property of this method we can measure both intensity and line profile of - chro mospheric emission lines. Dispersion was about 2.3 A/ram. Standardization were - made hy means of tube sensitometers for relative energies, and for absolute energies the partial sun was used. From the appearance of spicule structures on weaker lines it looks that the chromosphere has a sheath like spicule structure much furtber down than is believed. Short aecounts of some other features of our spectrograms are also given. Title: Structure of the Flare Authors: Suemoto, Z.; Hiei, E.; Hirayama, T. Bibcode: 1962JPSJS..17B.231S Altcode: 1962ICRC....7B.231S; 1962PSJaP..17B.231S; 1962JPSJ...17B.231S No abstract at ADS Title: Turbulence in the Chromosphere. Authors: Suemoto, Z. Bibcode: 1962AJ.....67T.283S Altcode: On our spectrograms of 1958 eclipse one can trace spicule structures as far down as 1500 km. Resemblance of these structures for all lines including even He I lines suggests that the chromosphere is composed of spicules with sheath-like structure down to this level. Turbulence velocities at lower levels were measured on weak lines and were corrected for self-absorption effect. The velocity increases slowly starting from 3 km/sec at zero height up to about 10 km/sec at 1000 km. Velocities at higher levels were measured for apparently individual spicules on H and K lines of Ca II. Linewidths for those spicules vary appreciably from spicule to spicule, suggesting that even among what seem to be individual spicules are included groups of spicules. If we interpret the smallest observed velocity as the actual velocities within an individual spicule, the turbulence velocity inside each spicule would come out to be about 7 km/sec even at the height of several thousand kilometers. Relative velocities between the spicules are relatively big, and if we include all velocities, the turbulence velocity increases upwards with the height in accordance with Redman and Suemoto's result. Title: Flash Spectrum by the Grazing Incidence Method at the Total Solar Eclipse of October 12, 1958 Authors: Suemoto, Z.; Hiei, E. Bibcode: 1959PASJ...11..122S Altcode: At the total solar eclipse of October 12, 1958, in South Pacific a new type of spectrograph was used in order to study both the intensity distributions and the profiles of chromospheric and photospheric lines. This spectrograph is similar to convetional slitless spectrographa normally used for the flash spectrum, but the essential difference is that the grating is used very obliquely. In this way we succeeded in taking flash spectra on which the line profiles are no more affected by the extension of the chromosphere and the atmospheric scintillation. Title: Balmer Series Lines of the Flare and its Structure Authors: Suemoto, Z.; Hiei, E. Bibcode: 1959PASJ...11..185S Altcode: The line widths of Balmer series lines from H to H14 were measured on a number of spectrograms of flares of medium importance taken by a wide range spectrograph with the dispersion of 3 A/mm. The width is very wide for the earlier members and decreases to a minimum somewhere around H9 and then increases slowly to higher members. By assigning the Stark broadening to higher members and the self absorp tion to lower members we derived the values of the electron density and total number of hydrogen atoms in the second quantum state. On the basis of uniform model of the flare these two values can only be made compatible when the very small geometieal thickness of the order of 10 km is attributed to the whole extension of the flare. We like to suggest, therefore, that the flare is composed of unresolvably fine, presumably thread like, condensations distributed over the whole extension. Title: Interferometric study of profiles of faint Fraunhofer lines Authors: Suemoto, Z. Bibcode: 1957MNRAS.117....2S Altcode: Profiles of well isolated Fraunhofer lines in the red were measured interferometrically by crossing a Fabry-Perot interferometer (with dielectric coating) with the 9 m spectrograph of the Cambridge Observatories. The average effective resolving power was as high as 6 x io5. The wave-length distribution of the selective absorption coefficient was derived from the measured profiles, using Vitense's Model II. For every point of the disk faint lines give broader Doppler widths than do stronger lines. It is suggested that there is a circulation in the solar atmosphere, vertical upward motion, m granules being converted into horizontal motion at about 0 4, and finally changing into downward motions back to the convection layer. Title: Temperature and turbulence in the chromosphere Authors: Redman, R. O.; Suemoto, Z. Bibcode: 1954MNRAS.114..524R Altcode: Measures of chromospheric line profiles in high resolution spectrograms obtained at the total solar eclipse of 1952 February 25 have been used to investigate further the question of temperature and turbulence in the solar chromosphere. In trying to deduce a distribution of line-of-sight velocities, arising from either temperature motions or turbulence, two problems are encountered : (a) to estimate the chromospheric heights to which the spectra refer, and (b) to correct the measures for broadening by self-absorption and Stark effect. Heights have been estimated partly from a comparison of line intensity ratios with those measured by Dr J. Houtgast on slitless spectrograms obtained at the same eclipse, and partly from the time of exposures, using the motion of the Moon relative to the Sun. Broadening by self- absorption has been estimated in the case of metallic lines by an empirical method. The corrected line widths, together with others of He 1, suggest an approximately linear increase of line-of-sight velocity with height, from km/sec at tbe base of the chromosphere, to 16 km/sec at height 2600 km. Taking into account the uncertainty in effective height, these results agree with those obtained in 1940. The hydrogen Balmer lines have been examined in more detail. The earlier members of the series are broadened by self-absorption, while later members are broadened by Stark effect. Both kinds of broadening were first estimated by an empirical method, which led to the conclusion that the temperature of the lower chromosphere does not exceed 10 000 deg. K. The hydrogen line widths were then computed more elaborately by a theoretical method, which showed that the observations could be fitted almost as well by a temperature 6 ooo deg. as by 10 000 deg. It seems unlikely that the present data will yield any closer estimate of temperature than this. Title: On Line Contours in the Anomalous Regions of the Sun Authors: Suemoto, Zenzaburo Bibcode: 1951PJAB...27...93S Altcode: No abstract at ADS Title: 太陽面異常領域の分光学的研究 Title: 太陽面異常領域の分光学的研究 Title: Spectroscopic study of the peculiar regions on the solar surface; Authors: Suemoto, Zenzaburo Bibcode: 1951PhDT........60S Altcode: No abstract at ADS Title: On the Limb Effect of Faint Fraunhofer Lines Authors: Suemoto, Zenzaburo Bibcode: 1951PJAB...27...88S Altcode: No abstract at ADS Title: Observation of the Limb Effect of Faint Fraunhofer Lines Authors: Suemoto, Z. Bibcode: 1951PASJ....2..126S Altcode: Limb center variations of some fifty faint Frannhofer lines were at Cos 0=1.0, 0.8, 0.6, 0.4, 0.3, and 0.2, and it was found that, statistically, lines. witl more rapidly witl deptl show stronger li'nb strengthening as compared wifl those with of slower decrease. Limb center variations were calcuisted for three types of variation t 5100 A, and tiiey were compared with those measured by Adam. Title: Electron Temperature of the Chromospheric Eruption Authors: Suemoto, Z. Bibcode: 1951PASJ....3..110S Altcode: The spectrogram of the chromospheric eruption of February 28, 1951 near the Ralmer series limit was studied. Oontours of H10, A 3737 of Ca+, and A 3720 of Fe were measured in order to obtain the numbers of active atoms. Considerations of the ionization showed that these densities are incompatible with an electron temperature higher than 20,()OO . Most likely electron temperature of the eruption was determined to be about 13,0000, whereas the density of atoms at the base of the eruption was estimated to be of the order of 5. 1Ot . 1) in favour of the low electron temperature of the normal chromosphere are also given. Title: Line Contours in the Anomalous Regions of the Sun Authors: Suemoto, Z. Bibcode: 1951PASJ....2..137S Altcode: Sume hundred standardized sp( tra concerning olar plienomena have beea eeuinuiated a tI tower telescope of the Tokyo Astronomical . For this purpose spectrohelioscope attachments and an a'ixiiiary were installe in the wer. Measurements were carried out by fl use of a self- inicrophotorneter constructed at our ol:servntory. Contours uf Hr, II, aud K lines in fi&es, flocculi, and flocmli over nspots were studie in ore of tlie flare si)ectr HE line is well fitted by a Doppler contour witl half width 0.44 A, corresponding to au electron temperature of 70,000 , while H and K line re fitted by the one which is the superpositien of the natural damping wing and the Doppler core witlj its width 0.070 A. Analysis of K line contour in fioccull yields tlie Doppler core of the same width, guggesting ttiat the layer r onslble for the emission l a electron temperature of the order 70,000 . The enhanced layer extends from the ba of the ere up to 10,000 kin for norinal floa but the Jayer seeim to be lifted by several fl and kilometers over sunspots. Vertical extension of tlie flare layer m' t be much higl than thet of . Title: Effect of Non-coherent Scattering on the Center Limb Variation of Strong Fraunhofer Lines Authors: Suemoto, Z. Bibcode: 1949PASJ....1...78S Altcode: No abstract at ADS