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The energy spectra of gamma-ray bursts differ from those of black-body radiation and are similar to the thermal bremsstrahlung
spectra of optically thin plasma. This could be realized if the source is located in the outer atmosphere of a neutron star.
In this case, almost one half of the emitted photons hit the surface of the star. The surface of the star is heated to a temperature
of the order 107 K, and a dominant flux of X-rays with a black-body spectrum would be expected. The X-rays produced by this mechanism are
detectable in the energy range from a few keV to 10 keV. This model is discussed in relation to the recent observations in
the X-ray region at the time of gamma-ray bursts, and modifications of this model are also presented. The observation in this
energy range will bring us valuable information on the nature of gamma-ray burst sources. 相似文献
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M. Yoshimori K. Okudaira Y. Hirasima T. Igarashi M. Akasaka Y. Takai K. Morimoto T. Watanabe K. Ohki J. Nishimura T. Yamagami Y. Ogawara I. Kondo 《Solar physics》1991,136(1):69-88
The SOLAR-A spacecraft has spectroscopic capabilities in a wide energy band from soft X-rays to gamma-rays. The Wide Band Spectrometer (WBS), consisting of three kinds of spectrometers, soft X-ray spectrometer (SXS), hard X-ray spectrometer (HXS) and gamma-ray spectrometer (GRS), is installed on SOLAR-A to investigate plasma heating, high-energy particle acceleration, and interaction processes. SXS has two proportional counters and each counter provides 128-channel pulse height data in the 2–30 keV range every 2 s and 2-channel pulse count data every 0.25 s. HXS has a NaI scintillation detector and provides 32-channel pulse height data in the 20–400 keV range every 1 s and 2-channel pulse count data every 0.125 s. GRS has two identical BGO scintillation detectors and each detector provides 128-channel pulse height data in the 0.2–10 MeV range every 4 s and 4-channel pulse count data (0.2–0.7, 0.7–4, 4–7, and 7–10 MeV) every 0.25–0.5 s. In addition, each of the BGO scintillation detectors provides 16-channel pulse height data in the 8–100 MeV range every 4 s and 2-channel pulse count data (8–30 and 30–100 MeV) every 0.5 s. The SXS observations enable one to study the thermal evolution of flare plasma by obtaining time series of electron temperatures and emission measures of hot plasma; the HXS observations enable one to study the electron acceleration and heating mechanisms by obtaining time series of the electron spectrum; and the GRS observations enable one to study the high-energy electron and ion acceleration and interaction processes by obtaining time series of electron and ion spectra.After the launch the name of SOLAR-A has been changed to YOHKOH. 相似文献
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Irimajiri Y. Manabe T. Ochiai S. Masuko H. Yamagami T. Saito Y. Izutsu N. Kawasaki T. Namiki M. Murata I. 《Geoscience and Remote Sensing Letters, IEEE》2006,3(1):88-92
A balloon-borne superconducting submillimeter-wave limb-emission sounder (BSMILES) was developed to observe thermal emission lines from stratospheric minor constituents. BSMILES carries a 300-mm-diameter offset parabolic antenna, a 624-639-GHz superconductor-insulator-superconductor (SIS) receiver, a three-axis fiber-optical gyroscope, and an acousto-optical spectrometer. BSMILES was launched from the Pacific Coast of Japan. All systems operated properly and emission line spectra of stratospheric gases, such as O/sub 3/, HCl, HO/sub 2/, and O/sub 3/ isotopes were measured. The system noise temperature in double sideband (DSB) during the flight was less than 460 K over the observing bandwidth with a best value of 330 K that is 11 times as large as the quantum limit (11h/spl nu//k/sub B/). After the observation, the gondola splashed down in the Pacific Ocean and was retrieved. Almost all instruments were waterproofed, and it has been proved that they are reusable. 相似文献
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We investigate selection effects on the size and frequency relation (logN-logS curve) of cosmic gamma-ray bursts. After analyzing the published data, we find an indication that an effect is caused by the different time profiles of the bursts. The effect is important for small bursts and causes significant changes in the logN-logS curve. in order to avoid this selection effect, we mention that it is essential to use the logN-logP relation of the logN-logS relation, as already suggested by other authors. Here,P is the peak flux of the burst, which is free from bias due to the difference in time profiles. After an analysis of the published data, we find a distribution nearP
–3/2 in the range above a peak flux of 40 counts/0.25 s.We also show that the relation between the logN-logP curve and the observed celestial distribution for the bursts can easily be explained by our general arguments on a disk-like spatial distribution of burst sources in the Galaxy. 相似文献
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In this study, three-dimensional structures and the life-time behavior of arctic cyclones are investigated as case studies, using reanalysis data of JRA-25 and JCDAS. In recent years, arctic region has undergone drastic warming in conjunction with the reduced sea ice concentration in summer. The rapid reduction of the sea ice concentration is explained, to some extent, by a pressure dipole of the arctic cyclone and Beaufort high over the Arctic Ocean. This paper presents some case studies for the structure of the arctic cyclone.It is found by the analysis of this study that the arctic cyclone indicates many differences in structure and behavior compared with the mid-latitude cyclone. The arctic cyclones move rather randomly in direction over the Arctic Ocean. The arctic cyclone has a barotropic structure in the vertical from the surface to the stratosphere. The arctic cyclone detected at the sea level pressure is connected with the polar vortex at the 500 hPa level and above. Importantly, the arctic cyclone has a cold core in the troposphere and a warm core around the 200 hPa level. The mechanism of the formation is discussed based on the analyzed structure of the arctic cyclones. 相似文献
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K. Kobayashi S. Tsuneta T. Tamura K. Kumagai Y. Katsukawa M. Kubo Y. Sakamoto N. Kohara T. Yamagami Y. Saito K. Mori 《Solar physics》2008,250(2):431-441
Spectroscopic observation of solar flares in the hard X-ray energy range, particularly the 20 ∼ 100 keV region, is an invaluable
tool for investigating the flare mechanism. This paper describes the design and performance of a balloon-borne hard X-ray
spectrometer using CdTe detectors developed for solar flare observation. The instrument is a small balloon payload (gondola
weight 70 kg) with sixteen 10×10×0.5 mm CdTe detectors, designed for a 1-day flight at 41 km altitude. It observes in an energy
range of 20−120 keV and has an energy resolution of 3 keV at 60 keV. The second flight on 24 May 2002 succeeded in observing
a class M1.1 flare. 相似文献
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