explanation blue bibcodes open ADS page with paths to full text
Author name code: shinoda
ADS astronomy entries on 2022-09-14
author:"Shinoda, Kazuya"
---------------------------------------------------------
Title: Development of Fast and Precise Scan Mirror Mechanism for an
Airborne Solar Telescope
Authors: Oba, Takayoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Kubo,
Masahito; Kawabata, Yusuke; Hara, Hirohisa; Uraguchi, Fumihiro;
Tsuzuki, Toshihiro; Tamura, Tomonori; Shinoda, Kazuya; Kodeki,
Kazuhide; Fukushima, Kazuhiko; Morales Fernández, José Miguel;
Sánchez Gómez, Antonio; Balaguer Jimenéz, María; Hernández
Expósito, David; Gandorfer, Achim
2022arXiv220713864O Altcode:
We developed a scan mirror mechanism (SMM) that enable a slit-based
spectrometer or spectropolarimeter to precisely and quickly map
an astronomical object. The SMM, designed to be installed in the
optical path preceding the entrance slit, tilts a folding mirror
and then moves the reflected image laterally on the slit plane,
thereby feeding a different one-dimensional image to be dispersed by
the spectroscopic equipment. In general, the SMM is required to scan
quickly and broadly while precisely placing the slit position across
the field-of-view (FOV). These performances are highly in demand for
near-future observations, such as studies on the magnetohydrodynamics of
the photosphere and the chromosphere. Our SMM implements a closed-loop
control system by installing electromagnetic actuators and gap-based
capacitance sensors. Our optical test measurements confirmed that the
SMM fulfils the following performance criteria: i) supreme scan-step
uniformity (linearity of 0.08%) across the wide scan range (${\pm}$1005
arcsec), ii) high stability (3${\sigma}$ = 0.1 arcsec), where the
angles are expressed in mechanical angle, and iii) fast stepping speed
(26 ms). The excellent capability of the SMM will be demonstrated
soon in actual use by installing the mechanism for a near-infrared
spectropolarimeter onboard the balloon-borne solar observatory for
the third launch, Sunrise III.
---------------------------------------------------------
Title: SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP)
for SUNRISE III: Scan mirror mechanism
Authors: Oba, Takayoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Kubo,
Masahito; Uraguchi, Fumihiro; Tsuzuki, Toshihiro; Tamura, Tomonori;
Shinoda, Kazuya; Kodeki, Kazuhide; Fukushima, Kazuhiko; Gandorfer,
Achim; del Toro Iniesta, Jose Carlos
2020SPIE11445E..4FO Altcode:
The SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP) is a
balloon-borne long-slit spectrograph for SUNRISE III to precisely
measure magnetic fields in the solar atmosphere. The scan mirror
mechanism (SMM) is installed in the optical path to the entrance slit
of the SCIP to move solar images focused on the slit for 2-dimensional
mapping. The SMM is required to have (1) the tilt stability better
than 0.035″ (3σ) on the sky angle for the diffraction-limited
spatial resolution of 0.2″, (2) step response shorter than 32 msec
for rapid scanning observations, and (3) good linearity (i.e. step
uniformity) over the entire field-of-view (60″x60″). To achieve
these performances, we have developed a flight-model mechanism
and its electronics, in which the mirror tilt is controlled by
electromagnetic actuators with a closed-loop feedback logic with
tilt angles from gap-based capacitance sensors. Several optical
measurements on the optical bench verified that the mechanism meets
the requirements. In particular, the tilt stability achives better
than 0.012″ (3σ). Thermal cycling and thermal vacuum tests have
been completed to demonstrate the performance in the vacuum and the
operational temperature range expected in the balloon flight. We
found a small temperature dependence in the step uniformity and this
dependence will be corrected to have 2-demensional maps with the
sub-arcsec spatial accuracy in the data post-processing.
---------------------------------------------------------
Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP)
for SUNRISE III: polarization modulation unit
Authors: Kubo, Masahito; Shimizu, Toshifumi; Katsukawa, Yukio;
Kawabata, Yusuke; Anan, Tetsu; Ichimoto, Kiyoshi; Shinoda, Kazuya;
Tamura, Tomonori; Nodomi, Yoshifumi; Nakayama, Satoshi; Yamada, Takuya;
Tajima, Takao; Nakata, Shimpei; Nakajima, Yoshihito; Okutani, Kousei;
Feller, Alex; del Toro Iniesta, Jose Carlos
2020SPIE11447E..A3K Altcode:
Polarization measurements of the solar chromospheric lines at
high precision are key to present and future solar telescopes for
understanding magnetic field structures in the chromosphere. The
Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for Sunrise
III is a spectropolarimeter with a polarimetric precision of 0.03 %
(1 σ). The key to high-precision polarization measurements using
SCIP is a polarization modulation unit that rotates a waveplate
continuously at a constant speed. The rotating mechanism is a DC
brushless motor originally developed for a future space mission, and
its control logic was originally developed for the sounding rocket
experiment CLASP. Because of our requirement on a speed of rotation
(0.512 s/rotation) that was 10 times faster than that of CLASP, we
optimized the control logic for the required faster rotation. Fast
polarization modulation is essential for investigating the fine-scale
magnetic field structures related to the dynamical chromospheric
phenomena. We have verified that the rotation performance can achieve
the polarization precision of 0.03 % (1 σ) required by SCIP and such
a significant rotation performance is maintained under thermal vacuum
conditions by simulating the environment of the Sunrise III balloon
flight. The waveplate was designed as a pair of two birefringent
plates made of quartz and sapphire to achieve a constant retardation
in a wide wavelength range. We have confirmed that the retardation
is almost constant in the 770 nm and 850nm wavelength bands of SCIP
under the operational temperature conditions.
---------------------------------------------------------
Title: Sunrise Chromospheric Infrared SpectroPolarimeter (SCIP)
for sunrise III: system design and capability
Authors: Katsukawa, Y.; del Toro Iniesta, J. C.; Solanki, S. K.;
Kubo, M.; Hara, H.; Shimizu, T.; Oba, T.; Kawabata, Y.; Tsuzuki,
T.; Uraguchi, F.; Nodomi, Y.; Shinoda, K.; Tamura, T.; Suematsu,
Y.; Ishikawa, R.; Kano, R.; Matsumoto, T.; Ichimoto, K.; Nagata, S.;
Quintero Noda, C.; Anan, T.; Orozco Suárez, D.; Balaguer Jiménez,
M.; López Jiménez, A. C.; Cobos Carrascosa, J. P.; Feller, A.;
Riethmueller, T.; Gandorfer, A.; Lagg, A.
2020SPIE11447E..0YK Altcode:
The Sunrise balloon-borne solar observatory carries a 1 m aperture
optical telescope and provides us a unique platform to conduct
continuous seeing-free observations at UV-visible-IR wavelengths from
an altitude of higher than 35 km. For the next flight planned for
2022, the post-focus instrumentation is upgraded with new spectro-
polarimeters for the near UV (SUSI) and the near-IR (SCIP), whereas
the imaging spectro-polarimeter Tunable Magnetograph (TuMag) is capable
of observing multiple spectral lines within the visible wavelength. A
new spectro-polarimeter called the Sunrise Chromospheric Infrared
spectroPolarimeter (SCIP) is under development for observing near-IR
wavelength ranges of around 770 nm and 850 nm. These wavelength ranges
contain many spectral lines sensitive to solar magnetic fields and
SCIP will be able to obtain magnetic and velocity structures in the
solar atmosphere with a sufficient height resolution by combining
spectro-polarimetric data of these lines. Polarimetric measurements are
conducted using a rotating waveplate as a modulator and polarizing beam
splitters in front of the cameras. The spatial and spectral resolutions
are 0.2" and 2 105, respectively, and a polarimetric sensitivity of
0.03 % (1σ) is achieved within a 10 s integration time. To detect
minute polarization signals with good precision, we carefully designed
the opto-mechanical system, polarization optics and modulation, and
onboard data processing.
---------------------------------------------------------
Title: Infrared spectro-polarimeter on the Solar Flare Telescope
at NAOJ/Mitaka
Authors: Sakurai, Takashi; Hanaoka, Yoichiro; Arai, Takehiko; Hagino,
Masaoki; Kawate, Tomoko; Kitagawa, Naomasa; Kobiki, Toshihiko;
Miyashita, Masakuni; Morita, Satoshi; Otsuji, Ken'ichi; Shinoda,
Kazuya; Suzuki, Isao; Yaji, Kentaro; Yamasaki, Takayuki; Fukuda,
Takeo; Noguchi, Motokazu; Takeyama, Norihide; Kanai, Yoshikazu;
Yamamuro, Tomoyasu
2018PASJ...70...58S Altcode: 2018PASJ..tmp...63S; 2018PASJ..tmp...82S
An infrared spectro-polarimeter installed on the Solar Flare Telescope
at the Mitaka headquarters of the National Astronomical Observatory of
Japan is described. The new spectro-polarimeter observes the full Sun
via slit scans performed at two wavelength bands, one near 1565 nm for a
Zeeman-sensitive spectral line of Fe I and the other near 1083 nm for He
I and Si I lines. The full Stokes profiles are recorded; the Fe I and Si
I lines give information on photospheric vector magnetic fields, and the
helium line is suitable for deriving chromospheric magnetic fields. The
infrared detector we are using is an InGaAs camera with 640 × 512
pixels and a read-out speed of 90 frames s<SUP>-1</SUP>. The solar
disk is covered by two swaths (the northern and southern hemispheres)
of 640 pixels each. The final magnetic maps are made of 1200 × 1200
pixels with a pixel size of 1{^”<SUB>.</SUB>}8. We have been carrying
out regular observations since 2010 April, and have provided full-disk,
full-Stokes maps, at the rate of a few maps per day, on the internet.
---------------------------------------------------------
Title: Wavefront error measurements and alignment of CLASP2 telescope
with a dual-band pass cold mirror coated primary mirror
Authors: Yoshida, Masaki; Song, Donguk; Ishikawa, Ryoko; Kano, Ryouhei;
Katsukawa, Yukio; Suematsu, Yoshinori; Narukage, Noriyuki; Kubo,
Masahito; Shinoda, Kazuya; Okamoto, Takenori J.; McKenzie, David E.;
Rachmeler, Laurel A.; Auchère, Frédéric; Trujillo Bueno, Javier
2018SPIE10699E..30Y Altcode:
"Chromospheric LAyer Spectro-Polarimeter (CLASP2)" is the next sounding
rocket experiment of the "Chromospheric Lyman-Alpha Spectro-Polarimeter
(CLASP)" that succeeded in observing for the first time the linear
polarization spectra in the hydrogen Lyman-α line (121.6 nm) and is
scheduled to be launched in 2019. In CLASP2, we will carry out full
Stokes-vector spectropolarimetric observations in the Mg ii h and k
lines near 280 nm with the spectro-polarimeter (SP), while imaging
observations in the Lyman-α line will be conducted with the slitjaw
optics (SJ). For the wavelength selection of CLASP2, the primary
mirror of the telescope uses a new dual-band pass cold mirror coating
targeting both at 121.6 nm and 280 nm. Therefore, we have to perform
again the alignment of the telescope after the installation of the
recoated primary mirror. Before unmounting the primary mirror from
the telescope structure, we measured the wave-front error (WFE) of the
telescope. The measured WFE map was consistent with what we had before
the CLASP flight, clearly indicating that the telescope alignment has
been maintained even after the flight. After the re-coated primary
mirror was installed the WFE was measured, and coma aberration was
found to be larger. Finally, the secondary mirror shim adjustments
were carried out based on the WFE measurements. In CLASP2 telescope,
we improved a fitting method of WFE map (applying 8th terms circular
Zernike polynomial fitting instead of 37th terms circular Zernike
fitting) and the improved method enables to achieve better performance
than CLASP telescope. Indeed, WFE map obtained after the final shim
adjustment indicated that the required specification (< 5.5 μm
RMS spot radius) that is more stringent than CLASP telescope was met.
---------------------------------------------------------
Title: Optical alignment of the high-precision UV spectro-polarimeter
(CLASP2)
Authors: Song, Donguk; Ishikawa, Ryohko; Kano, Ryouhei; Yoshida,
Masaki; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Shinoda, Kazuya;
Hara, Hirohisa; Okamoto, Takenori J.; Auchère, Frédéric; McKenzie,
David E.; Rachmeler, Laurel A.; Trujillo Bueno, Javier
2018SPIE10699E..2WS Altcode:
Chromospheric LAyer Spectro-Polarimeter (CLASP2) is our next sounding
rocket experiment after the success of Chromospheric Lyman-Alpha
Spectro-Polarimeter (CLASP1). CLASP2 is scheduled to launch in 2019,
and aims to achieve high precision measurements (< 0.1 %) of the
linear and circular polarizations in the Mg ii h and k lines near the
280 nm, whose line cores originate in the upper solar chromosphere. The
CLASP2 spectro-polarimeter follows very successful design concept of
the CLASP1 instrument with the minimal modification. A new grating was
fabricated with the same radius of curvature as the CLASP1 grating, but
with a different ruling density. This allows us to essentially reuse
the CLASP1 mechanical structures and layout of the optics. However,
because the observing wavelength of CLASP2 is twice longer than that
of CLASP1, a magnifier optical system was newly added in front of the
cameras to double the focal length of CLASP2 and to maintain the same
wavelength resolution as CLASP1 (0.01 nm). Meanwhile, a careful optical
alignment of the spectro-polarimeter is required to reach the 0.01 nm
wavelength resolution. Therefore, we established an efficient alignment
procedure for the CLASP2 spectro-polarimeter based on an experience
of CLASP1. Here, we explain in detail the methods for achieving the
optical alignment of the CLASP2 spectro-polarimeter and discuss our
results by comparing with the performance requirements.
---------------------------------------------------------
Title: Development of the Universal Tunable Filter and High-resolution
Imaging Observation with the Fuxian Solar Observatory
Authors: Hagino, M.; Ichimoto, K.; Ueno, S.; Kimura, G.; Otsuji, K.;
Kitai, R.; Zhong, L.; Xu, Z.; Shinoda, K.; Hara, H.; Suematsu, Y.;
Shimizu, T.
2016ASPC..504..103H Altcode:
We have developed a new narrow-band universal tunable filter to perform
imaging spectroscopy of the solar chromosphere. The development stage
of the filter has been almost finished and we shifted to the scientific
observation phase by using large grand-based telescopes. Using the
filter, a series of high-resolution images were obtained with the 1m
vacuum solar telescope at the Fuxian Solar Observatory. We succeeded in
observing several flares and fine structures of the chromospheric layer.
---------------------------------------------------------
Title: Development of a universal tunable filter for future solar
observations
Authors: Hagino, M.; Ichimoto, K.; Kimura, G.; Nakatani, Y.; Kawate,
T.; Shinoda, K.; Suematsu, Y.; Hara, H.; Shimizu, T.
2014SPIE.9151E..5VH Altcode:
We have developed a new narrowband tunable filter to perform imaging
spectroscopy of the solar chromosphere. Using Liquid Crystal Variable
Retarders (LCVRs) as the tuning elements for wavelength, wide-band
polarizers and super achromatic half-wave plates, it is possible to make
high speed tuning (about 0.1Sec), to exclude mechanical drives (and oil
tank), and to cover a wide wavelength range (510-100nm). This filter
builds up with seven stages each consisting of a pair of calcites,
LCVR, half-wave plates and linear polarizer. The full width at half
maximum (FWHM) of the filter transmission is about 0.025nm at 656.3nm.We
demonstrate that the concept of the universal tunable filter using the
LCVR's as tuning elements is highly promising for future application
to space mission and ground based observations.
---------------------------------------------------------
Title: Integral Field Spectroscopy of the Sun with Microlens Array
and Liquid Crystal Retarders
Authors: Suematsu, Y.; Shinoda, K.; Sano, I.; Kobiki, T.
2011AGUFMSH13B1947S Altcode:
Simultaneous spectrographic observations over extended solar structures,
at a high spatial resolution and temporal cadence, are important
to track and understand the physics of transient phenomena such as
Ellerman bombs, flare kernels, prominences/filaments and spicules. With
two-dimensional (2-D) field spectral data, we can make monochromatic
images at a given wavelength in a designed passband and line profile
analysis to derive 2-D distribution of atmospheric parameters. One
technique to produce a spectrum of each spatial elements in an extended
two-dimensional field is to use a micro-lens array. Replacing a slit
of a conventional spectrograph with a micro-lens array then helps to
capture two-dimensionally distributed short spectra from 2-D field
using additional optics inserted, a bandpass filter and a large format
detector. For observations of magnetic field, we can add polarization
modulator made of liquid crystal retarders which give a sequence of
alternative orthogonal polarization states with time. We describe a
design concept and limitations for observations with the micro-lens
array spectrograph and an initial result applied for a few existing
solar telescopes at NAOJ and Hida Observatory, Kyoto University.
---------------------------------------------------------
Title: Infrared Stokes Spectro-Polarimeter at the National
Astronomical Observatory of Japan
Authors: Hanaoka, Y.; Sakurai, T.; Shinoda, K.; Noguchi, M.; Miyashita,
M.; Fukuda, T.; Suzuki, I.; Hagino, M.; Arai, T.; Yamasaki, T.;
Takeyama, N.
2011ASPC..437..371H Altcode:
We are now constructing an infrared spectro-polarimeter for the Solar
Flare Telescope of NAOJ. It observes the full Sun in two wavelength
bands, one near 1.56 μm for highly Zeeman-sensitive spectral lines of
Fe I and the other near 10830 Å for He I and Si I lines. The instrument
records full Stokes profiles, and a Stokes inversion process will
give information on the strength and orientation of the magnetic field
vector for both of the photosphere and the chromosphere. The infrared
detector we are using is an InGaAs camera manufactured by a Belgian
company Xenics. Its format is 640×512 pixels and its read-out speed is
90 frames s<SUP>-1</SUP>. The solar disk will be covered by two swaths
(the northern and southern hemispheres) of 640 pixels each. The final
magnetic maps will be made of 1200×1200 pixels with a pixel size of
1.8 arcsec. Now we are operating regular observations and generate
full-disk, full-Stokes maps (a few maps per day). Our ultimate goal is
to derive the distribution of magnetic helicity over the whole surface
of the Sun, not only in sunspots and active regions.
---------------------------------------------------------
Title: Polarization Calibration of the Solar Optical Telescope
onboard Hinode
Authors: Ichimoto, K.; Lites, B.; Elmore, D.; Suematsu, Y.; Tsuneta,
S.; Katsukawa, Y.; Shimizu, T.; Shine, R.; Tarbell, T.; Title, A.;
Kiyohara, J.; Shinoda, K.; Card, G.; Lecinski, A.; Streander, K.;
Nakagiri, M.; Miyashita, M.; Noguchi, M.; Hoffmann, C.; Cruz, T.
2008SoPh..249..233I Altcode: 2008SoPh..tmp...69I
The Solar Optical Telescope (SOT) onboard Hinode aims to obtain vector
magnetic fields on the Sun through precise spectropolarimetry of
solar spectral lines with a spatial resolution of 0.2 - 0.3 arcsec. A
photometric accuracy of 10<SUP>−3</SUP> is achieved and, after the
polarization calibration, any artificial polarization from crosstalk
among Stokes parameters is required to be suppressed below the level
of the statistical noise over the SOT's field of view. This goal was
achieved by the highly optimized design of the SOT as a polarimeter,
extensive analyses and testing of optical elements, and an end-to-end
calibration test of the entire system. In this paper we review both
the approach adopted to realize the high-precision polarimeter of the
SOT and its final polarization characteristics.
---------------------------------------------------------
Title: Photopolarimetric measurement system of Mueller matrix with
dual rotating waveplates
Authors: Ichimoto, Kiyoshi; Shinoda, Kazuya; Yamamoto, Tetsuya;
Kiyohara, Junko
2006PNAOJ...9...11I Altcode:
A new photopolarimetric measurement system of Mueller matrix of optical
elements is developed using dual rotating waveplates. The waveplates in
polarization generator and analyzer rotate continuously with a constant
ratio of revolution speed, and the Mueller matrix of a sample can be
obtained in a few seconds. General principle of such measurement and the
optimization of operation parameters are discussed, followed by detailed
descriptions of the constructed system. Some examples of its application
are also demonstrated. The system is sensitive to <10<SUP>-3</SUP>
for each Mueller matrix element for weak polarization elements.
---------------------------------------------------------
Title: Flexible prism used as an image stabilizer
Authors: Sakurai, Takashi; Noguchi, Motokazu; Shinoda, Kazuya;
Tanaka, Nobuyuki
2003naoj.book...35S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations of the Mie scattered light intensities around
the Sun with a portable coronagraph
Authors: Tanaka, Nobuyuki; Kobiki, Toshihiko; Saito, Moriya; Shinoda,
Kazuya; Irie, Makoto
2002RNAOJ...6...11T Altcode:
Measurements of Mie scattering intensites around the Sun have
been carried out by using a 5 cm coronagraph at (1) Chichijima,
Ogasawara Islands, (2) Shiiba, Miyazaki prefecture, (3) Kitadaito
Island, Okinawa, (4) Hateruma Islands, Okinawa, and (5) Saku Island,
Aichi prefecture. Although our observations were limited in time
for only a few days, the results indicate that the solar corona may
be observable even at an altitude of 1,000m or less (for example
at Shiiba, Miyazaki) where the intensity of scattered light is
eventually less than 100 μI<SUB>o</SUB> (here I<SUB>o</SUB> is
the intensity of the solar disk center, and μI<SUB>o</SUB> means
I<SUB>o</SUB>×10<SUP>-6</SUP>). Comparison among the tested sites is
diffucult because the measurements were done in various seasons in the
year; and monitoring over longer time period is necessary to derive
definite conclusions. However, the sites where the scattered light
intensity is stable and less than 100 μI<SUB>o</SUB>, could be a good
site for the observations of the Sun considering the transparency of
the sky.
---------------------------------------------------------
Title: Two nakhlites from Antarctica: Y000593 and Y000749.
Authors: Imae, N.; Ikeda, Y.; Shinoda, K.; Kojima, H.; Iwata, N.
2002anme...27...45I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Flexible Prism used as an Image Stabilizer
Authors: Sakurai, T.; Noguchi, M.; Shinoda, K.; Tanaka, N.; Aoki,
K.; Hagino, M.; Mochizuki, H.
2002SoPh..205..201S Altcode:
An image stabilizer was constructed by making use of a flexible prism,
which is widely used as an anti-vibration mechanism in handheld video
cameras. The prism responds to frequencies up to 20 Hz, and can be
simply inserted into existing optics. The performance of the prism
has been confirmed by observing the Sun through it.
---------------------------------------------------------
Title: A universal polarimeter using liquid crystal variable retarders
at the Norikura Solar Observatory
Authors: Shinoda, Kazuya; Ichimoto, Kiyoshi; Fukuda, Takeo; Shin, Junho
2001RNAOJ...5...97S Altcode:
A universal Stokes polarimeter was developed for the 25-cm coronagraph
of the Norikura Solar Observatory. The polarimeter utilizes two liquid
crystal variable retarders (LCVR) as the polarization modulator and a
Savart plate as the polarization analyser. By controlling the voltages
applied to LCVRs, modulations of the polarization states are achieved
more flexibly and efficiently in a wavelength range of 450-1,600 nm. The
polarimeter is installed at the primary focus of the coronagraph to
minimize the instrumental polarization caused by optics. Two orthogonal
polarization states are measured simultaneously to minimize the effect
of guiding errors and seeing effects. Combined with the coronagraph and
the high resolution spectrograph at the coude focus, the polarimeter
enables us not only observations of photospheric Zeeman effect but also
various types of diagnostics of the solar atmosphere, including coronal
Zeeman effect, Hanle effect, impact polarization, and Stark effect.
---------------------------------------------------------
Title: An imaging system of coronal green-line with a Lyot filter.
Authors: Imai, H.; Nishino, Y.; Shinoda, K.; Ichimoto, K.
1999RNAOJ...4..157I Altcode:
An experimental observation system for taking coronal images in the
green line (Fe XIV 5303 Å) was constructed on the 25 cm coronagraph
of the Norikura Solar Observatory. By re-arranging the birefringent
elements and equipping rotating waveplates on a Lyot filter, the
authors were able to obtain images in coronal green-line and sky
continuum with a high time cadence. It is shown that this system
can provide a powerful tool for diagnosing the physical processes in
coronal transient phenomena.
---------------------------------------------------------
Title: A New Imaging System of the Corona at Norikura
Authors: Ichimoto, Kiyoshi; Noguchi, Motokazu; Tanaka, Nobuyuki;
Kumagai, Kazuyoshi; Shinoda, Kazuya; Nishino, Tetsuo; Fukuda, Takeo;
Sakurai, Takashi; Takeyama, Norihide
1999PASJ...51..383I Altcode:
A new imaging system of the coronal green line (Fe XIV 5303
Angstroms) was constructed at the Norikura Solar Observatory. The
system consists of a 10-cm coronagraph, a tunable Lyot filter, and
a cooled CCD camera. The transmission curve of the Lyot filter can
be modulated by two liquid-crystal variable retarders. This scheme
provides quick wavelength tuning and efficient subtraction of sky
background. Two-dimensional distributions of the intensity and
Doppler shift of the coronal green line can be obtained within 30
seconds with accuracies of better than 10<SUP>-6</SUP>I_Solar and 1 km
s<SUP>-1</SUP>. Regular operation was started in 1997 September. The
aim of the new system is to investigate plasma motions associated with
the magnetic field reconnection and waves in the solar corona.
---------------------------------------------------------
Title: An Experimental Study of Hydrous Mineral Formation Reaction
Between Enstatite and Water Vapor
Authors: Imae, N.; Shinoda, K.
1998M&PSA..33...73I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Flare Telescope at Mitaka
Authors: Sakurai, Takashi; Ichimoto, Kiyoshi; Nishino, Yohei; Shinoda,
Kazuya; Noguchi, Motokazu; Hiei, Eijiro; Li, Ting; He, Fengbao; Mao,
Weijun; Lu, Haitian; Ai, Guoxiang; Zhao, Zhaowang; Kawakami, Singo;
Chae, Jong-Chul
1995PASJ...47...81S Altcode:
A new solar telescope constructed recently at Mitaka, Tokyo, is
described. This instrument, called the Solar Flare Telescope, comprises
four telescopes which respectively perform: (1) magnetic-field vector
measurements, (2) Doppler-velocity measurements, (3) Hα observations,
and (4) continuum observations. The instrument has been operated as
a ground-based support for the X-ray satellite Yohkoh launched in
1991 August.
---------------------------------------------------------
Title: Optical and SXT Observations of the x9 Flare of Nov. 1992
Authors: Ichimoto, K.; Sakurai, T.; Nishino, Y.; Noguchi, M.; Shinoda,
K.; Yamaguchi, A.; Kumagai, K.; Hirayama, T.; Tsuneta, S.; Acton, L.
1994xspy.conf..259I Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Flare Telescope project.
Authors: Ichimoto, K.; Sakurai, T.; Hiei, E.; Nishino, Y.; Shinoda, K.;
Noguchi, M.; Imai, H.; Irie, M.; Miyashita, M.; Tanaka, N.; Kumagai,
K.; Sano, I.; Suematsu, Y.; Okamoto, T.; Miyazaki, H.; Fukushima,
H.; Yose, Y.; Zhao, Z. W.
1993RNAOJ...1..375I Altcode: 1993RNOAJ...1..375I
The Solar Flare Telescope was built at Mitaka in 1989. This instrument
comprises four telescopes which observe (1) Hα images, (2) continuum
images, (3) vector magnetic fields, and (4) Doppler velocities,
respectively. The instrument aims at the study of energy build-up
and energy release in solar flares, in cooperation with the Solar-A
satellite (Yohkoh). The Solar Flare Telescope has been in operation
since 1990 December.
---------------------------------------------------------
Title: Magnetic Field Observation with the Solar Flare Telescope
Authors: Ichimoto, K.; Sakurai, T.; Nishino, Y.; Shinoda, K.; Noguchi,
M.; Kumagai, K.; Imai, H.; Irie, M.; Miyashita, M.; Tanaka, N.; Sano,
I.; Suematsu, Y.; Hiei, E.
1993ASPC...46..166I Altcode: 1993IAUCo.141..166I; 1993mvfs.conf..166I
No abstract at ADS
---------------------------------------------------------
Title: White-Light Flares of 1991 June in the NOAA Region 6659
Authors: Sakurai, Takashi; Ichimoto, Kiyoshi; Hiei, Eijiro; Irie,
Makoto; Kumagai, Kazuyoshi; Miyashita, Masakuni; Nishino, Yohei;
Yamaguchi, Kisuke; Fang, Geng; Kambry, Maspul Aini; Zhao, Zhaowang;
Shinoda, Kazuya
1992PASJ...44L...7S Altcode:
We report on observations of flare activities in an active region NOAA
6659, which appeared on the sun in 1991 June. Among six X-class flares
in this region, we observed three flares (June 4, 9, and 11), all of
which were white-light flares. A detailed discussion is given concerning
a particularly interesting white-light flare which occurred on June 11.
---------------------------------------------------------
Title: GINGA observation of the X-ray pulsar 1E 2259+586 in the
supernova remnant G 109.1-1.0
Authors: Koyama, K.; Nagase, F.; Ogawara, Y.; Shinoda, K.; Kawai, N.;
Jones, M. H.; Williams, O. R.; Watson, M. G.; Makishima, K.; Ohashi, T.
1989PASJ...41..461K Altcode:
The X-ray pulsar 1E 2259+586 in the supernova remnant G109.1-1.0
was observed with the Ginga satellite from June 21 to 23, 1987. The
heliocentric pulse period is found to be 6.978759 + or - 0.000002 s,
confirming a secular spin down rate of 6.2 x 10 to the -13th s/s. The
pulsation was observed to have asymmetric double peaks in the energy
range from 1 keV to 10 keV. The upper limit on the projected semimajor
axis is 0.08 1t-s (3sigma) throughout the period range searched. The
constraint on the binary system is discussed in the light of this new
upper limit. The energy spectrum of 1E 2259+586 does not show a single
power law spectrum but exhibits a complex structure which mimics an
emission line at 7.2 keV. An attempt to ascribe the structure to a
cyclotron line feature is presented. This interpretation implies a weak
magnetic field of 5 x 10 to the 11th G at the neutron star surface of
1E 2259+586.
---------------------------------------------------------
Title: Ginga observation of the X-ray pulsar 1E2259+586 in the
supernova remnant G109.1-1.0.
Authors: Shinoda, K.; Koyama, K.; Nagase, F.; Ogawara, Y.; Kawai, N.
1988pnsb.conf...67S Altcode: 1988pbsb.conf...67S
The authors observed 1E 2259+586 on June 21-23, 1987 with the Ginga
satellite. In this paper they report briefly the pulse profile, the
pulse period and energy spectrum observed.
