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How-Do-We-See-the-Relativistic-Accretion-Disk-during-Thermal-Instability?
PASJ: Publ. Astron. Soc. Japan , 1–??,
c
2006. Astronomical Society of Japan.
How Do We See the Relativistic Accretion Disk during Thermal
Instability?
Akihiro Kawata,1 Ken-ya Watarai,1,2 and Jun Fukue1
1Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582-8582
2Research Fellow of the Japan Society for the Promotion of Science
j049340@ex.osaka-kyoiku.ac.jp
(Received 2005 November 14; accepted 0 0)
Abstract
We calculated the bolometric images of relativistic slim disks during radiation-pressure-driven thermal
instability. When the mass-accretion rate exceeds the critical one, an inner region of the standard accretion
disk bursts to change to a slim disk state having a large scale height. That is, the inner region of the disk
becomes high temperature, and the thickness of the disk increases due to the increase of the radiation
pressure. As a result, we found that the observed image of the disk during the burst strongly depends on
the inclination angle. That is, radiation from the innermost disk would be occulted by the disk outer rim
◦
for high inclination angles (i ∼ 70 ). We also calculated the spectral energy distribution during thermal
instability. The Wien peak of the spectrum of high inclination angles becomes softer than that of low
inclination angles due to the geometrical thickness. From these facts, even if the burst happens in black
hole candidates, we may not observe the burst when the inclinatio
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