THE SLIM-DISK STATE OF THE ULTRALUMINOUS X-RAY SOURCE IN M83

被引：21

作者：

Soria, Roberto ^{[1
]}

Kuntz, K. D. ^{[2
]}

Long, Knox S. ^{[3
]}

Blair, William P. ^{[2
]}

Plucinsky, Paul P. ^{[4
]}

Winkler, P. Frank ^{[5
]}

机构：

[1] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia

[2] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA

[3] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 799卷 / 02期

基金：

美国国家航空航天局;

关键词：

accretion; accretion disks; black hole physics; galaxies: individual (M83); X-rays: binaries; MASS BLACK-HOLES; SUPER-EDDINGTON ACCRETION; NEARBY SPIRAL GALAXIES; SPECTRAL VARIABILITY; GRO J1655-40; MODEL; OSCILLATIONS; CANDIDATES; ABUNDANCES; 4U-1630-47;

D O I：

10.1088/0004-637X/799/2/140

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The transient ULX in M83 that went into outburst in, or shortly before, 2010 is still active. Our new XMM-Newton spectra show that it has a curved spectrum typical of the upper end of the high/soft state or slim-disk state. It appears to be spanning the gap between Galactic stellar-mass black holes (BHs) and the ultraluminous state, at X-ray luminosities of approximate to 1-3 x 10(39) erg s(-1) (a factor of two lower than in the 2010 and 2011 Chandra observations). From its broadened disk-like spectral shape at that luminosity, and from the fitted inner-disk radius and temperature, we argue that the accreting object is an ordinary stellar-mass BH with M similar to 10-20 M-circle dot. We suggest that in the 2010 and 2011 Chandra observations, the source was seen at a higher accretion rate, resulting in a power-law-dominated spectrum with a soft excess at large radii.

引用

页数：9

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