–¼ŒÃ‰®‘åŠwUŒ¤XüƒOƒ‹[ƒv
–¼ŒÃ‰®‘åŠw‘åŠw‰@—ŠwŒ¤‹†‰È@‘f—±Žq‰F’ˆ•¨—ŠwêU@‰F’ˆ•¨—ŠwŒ¤‹†Žº
§464-8602 @–¼ŒÃ‰®ŽsçŽí‹æ•s˜V’¬@Tel:052-789-2921@Fax:052-789-2919
 
Home Uir Site map English
ƒwƒbƒ_[
Œ¤‹†ŽºÐ‰î Œ¤‹†ƒvƒƒWƒFƒNƒg Œ¤‹†ŠT—v Œ¤‹†¬‰Ê ƒAƒNƒZƒXƒ}ƒbƒv ‚¨–â‚¢‡‚킹 ŠÖ˜AƒŠƒ“ƒN
Œ¤‹†¬‰Ê
˜_•¶
˜_•¶ƒŠƒXƒgEnglish
1990~1999
˜_•¶ƒŠƒXƒgEnglish
2000~
˜_•¶ƒŠƒXƒg
”ŽŽm˜_•¶ƒŠƒXƒg
CŽm˜_•¶ƒŠƒXƒg
V•·‹LŽ–
 
publication

X-ray observations of the broad line radio galaxy 3C382

J.S. Kaastra, H. Kunieda, and H. Awaki

Abstract

Ginga observations of the X-ray spectrum of the broad line radio galaxy 3C382 are reported. The continuum X-ray flux was two times lower than all previous measurements. Hard X-rays constituted probably less than 10 percent of the bolometric luminosity. Variability with exponential rise/decay times of two days is present. The variability amplitude increases with increasing time scale up to at least one year. If the minimum time scale is identified with the thermal time scale in an accretion disk at 5 Schwarzschild radii and the maximum time scale of at least a year with the viscosity time scale, a typical black hole mass of 100 million solar masses and an accretion rate of 0.1 solar mass/yr is deduced. The X-ray spectrum of 3C382 consists of three components: a power law, an Fe-line, and soft excess. The energy of the Fe-line is consistent both with the cool and hotter fluorescent material.

 
Copyright (c) 2008 Nagoya University . All Rights Reserved.  
 
ƒgƒbƒvƒy[ƒW‚É–ß‚é