suemoto

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Author name code: suemoto
ADS astronomy entries on 2022-09-14
author:"Suemoto, Zenzaburo"

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Title: In memoriam
Authors: Suemoto, Zenzaburo; Hiei, E.; Uchida, Y.
1993SoPh..146..203S Altcode:
No abstract at ADS

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Title: Continuous and Line Spectra of Granules and Intergranular Lanes
Authors: Suemoto, Z.; Hiei, E.; Nakagomi, Y.
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 &lt; 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.

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Title: Bright Features in the Intergranular Region
Authors: Suemoto, Z.; Hiei, E.
1990IAUS..138...97S Altcode:
No abstract at ADS

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Title: Bright threads in the inner wing of solar Ca II H and K lines.
Authors: Suemoto, Zenzaburo; Hiei, Eijiro; Nakagomi, Yoshiteru
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.

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Title: Bright threads in the inner wing of solar Ca II K line
Authors: Suemoto, Z.; Hiei, E.; Nakagomi, Y.
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.

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Title: Time and Latitude Bulletins. October 1979 - June 1980.
Authors: Suemoto, Z.
1980TokAT..53...45S Altcode:
No abstract at ADS

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Title: International Time and Latitude Service at the Tokyo
Astronomical Observatory during 1979.
Authors: Suemoto, Z.
1979TokAT..53....1S Altcode:
No abstract at ADS

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Title: International Time and Latitude Service at the Tokyo
Astronomical Observatory 1979.
Authors: Suemoto, Z.
1979TokAT..53...33S Altcode:
No abstract at ADS

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Title: International Time and Latitude Service at the Tokyo
Astronomical Observatory during 1978.
Authors: Suemoto, Z.
1978TokAT..52....1S Altcode:
No abstract at ADS

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Title: An empirical, statistical model for the formation of the
cores of chromospheric Fraunhofer lines.
Authors: Suemoto, Z.
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.

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Title: International Time and Latitude Service at the Tokyo
Astronomical Observatory during 1977.
Authors: Suemoto, Z.
1977TokAT..51...31S Altcode:
No abstract at ADS

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Title: Observations of the solar ultraviolet Mg II doublet. III.
Authors: Kohno, T.; Yajima, N.; Suemoto, Z.
1977BISAT..13..799K Altcode:
No abstract at ADS

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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.
1977BISAT..13..813T Altcode:
No abstract at ADS

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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.
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.

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Title: Infrared spectral observations of stars.
Authors: Komaki, K.; Kodaira, K.; Tanaka, W.; Suemoto, Z.
1976BISAT..12..623K Altcode:
No abstract at ADS

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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.
1976BISAT..12..959N Altcode:
No abstract at ADS

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Title: Observation of the solar ultraviolet Mg II doublet, (2).
Authors: Yajima, N.; Kohno, T.; Suemoto, Z.
1974TDUKK..10..174Y Altcode:
No abstract at ADS

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Title: Observation of the solar ultraviolet Mg II doublet, (1).
Authors: Kohno, T.; Yajima, N.; Suemoto, Z.
1974TDUKK..10..166K Altcode:
No abstract at ADS

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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.
1971IAUS...41..393N Altcode:
No abstract at ADS

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Title: A Measurement of the Solar H and K Profiles
Authors: White, O. R.; Suemoto, Z.
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.

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Title: Interpretation of K Emission Line Profile
Authors: Suemoto, Zenzaburo
1966PJAB...42..777S Altcode:
No abstract at ADS

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Title: Spotty appearance of the solar disk as inferred from the
comparison between E. U. V. and radio intensities
Authors: Suemoto, Z.; Moriyama, F.
1965IAUS...23..109S Altcode:
No abstract at ADS

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Title: Spotty appearance of the solar disk as inferred from the
comparaison between EUV and radio intensities
Authors: Suemoto, Z.; Moriyama, F.
1964AnAp...27..775S Altcode:
No abstract at ADS

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Title: Turbulence in the Chromosphere
Authors: Suemoto, Z.
1963PASJ...15..531S Altcode:
Turbulence velocities in the &amp;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.

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Title: Interpretation of Solar Extreme Ultraviolet Spectra Observed
with Rockets from a New Model of the Solar Chromosphere
Authors: Suemoto, Z.; Moriyama, F.
1963spre.conf..800S Altcode:
No abstract at ADS

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Title: A New Model of the Chromosphere
Authors: Suemoto, Zenzaburo
1963PJAB...39..463S Altcode:
No abstract at ADS

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Title: Observation of the Flash Spectrum at the Total Solar Eclipse
of October 12, 1958
Authors: Suemoto, Z.; Hiei, E.
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.

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Title: Structure of the Flare
Authors: Suemoto, Z.; Hiei, E.; Hirayama, T.
1962JPSJS..17B.231S Altcode: 1962ICRC....7B.231S; 1962PSJaP..17B.231S; 1962JPSJ...17B.231S
No abstract at ADS

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Title: Turbulence in the Chromosphere.
Authors: Suemoto, Z.
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.

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Title: Flash Spectrum by the Grazing Incidence Method at the Total
Solar Eclipse of October 12, 1958
Authors: Suemoto, Z.; Hiei, E.
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.

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Title: Balmer Series Lines of the Flare and its Structure
Authors: Suemoto, Z.; Hiei, E.
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.

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Title: Interferometric study of profiles of faint Fraunhofer lines
Authors: Suemoto, Z.
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.

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Title: Temperature and turbulence in the chromosphere
Authors: Redman, R. O.; Suemoto, Z.
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.

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Title: On Line Contours in the Anomalous Regions of the Sun
Authors: Suemoto, Zenzaburo
1951PJAB...27...93S Altcode:
No abstract at ADS

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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

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Title: Spectroscopic
study of the peculiar regions on the solar surface;
Authors: Suemoto, Zenzaburo
1951PhDT........60S Altcode:
No abstract at ADS

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Title: On the Limb Effect of Faint Fraunhofer Lines
Authors: Suemoto, Zenzaburo
1951PJAB...27...88S Altcode:
No abstract at ADS

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Title: Observation of the Limb Effect of Faint Fraunhofer Lines
Authors: Suemoto, Z.
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.

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Title: Electron Temperature of the Chromospheric Eruption
Authors: Suemoto, Z.
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.

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Title: Line Contours in the Anomalous Regions of the Sun
Authors: Suemoto, Z.
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&amp;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 .

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Title: Effect of Non-coherent Scattering on the Center Limb Variation
of Strong Fraunhofer Lines
Authors: Suemoto, Z.
1949PASJ....1...78S Altcode:
No abstract at ADS