INVESTIGATING SLIM DISK SOLUTIONS FOR HLX-1 IN ESO 243-49

被引:65
作者
Godet, O. [1 ,2 ]
Plazolles, B. [1 ,2 ]
Kawaguchi, T. [3 ]
Lasota, J. -P. [4 ,5 ]
Barret, D. [1 ,2 ]
Farrell, S. A. [6 ,7 ]
Braito, V. [6 ]
Servillat, M. [8 ]
Webb, N. [1 ,2 ]
Gehrels, N. [9 ]
机构
[1] Univ Toulouse, UPS, IRAP, F-31028 Toulouse 4, France
[2] CNRS, UMR5277, F-31028 Toulouse, France
[3] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan
[4] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France
[5] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland
[6] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England
[7] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia
[8] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[9] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
基金
澳大利亚研究理事会;
关键词
accretion; accretion disks; black hole physics; galaxies: individual (ESO 243-49); methods: data analysis; X-rays: individuals (HLX-1); X-RAY SOURCES; MASS BLACK-HOLE; ACCRETION DISKS; SPECTRAL VARIABILITY; MODEL; TRANSITIONS; EVOLUTION; BEHAVIOR; SYSTEMS; BINARY;
D O I
10.1088/0004-637X/752/1/34
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The hyperluminous X-ray source HLX-1 in the galaxy ESO 243-49, currently the best intermediate-mass black hole (BH) candidate, displays spectral transitions similar to those observed in Galactic BH binaries, but with a luminosity 100-1000 times higher. We investigated the X-ray properties of this unique source by fitting multiepoch data collected by Swift, XMM-Newton, and Chandra with a disk model computing spectra for a wide range of sub- and super-Eddington accretion rates assuming a non-spinning BH and a face-on disk (i = 0 degrees). Under these assumptions we find that the BH in HLX-1 is in the intermediate-mass range (similar to 2 x 10(4) M-circle dot) and the accretion flow is in the sub-Eddington regime. The disk radiation efficiency is eta = 0.11 +/- 0.03. We also show that the source does follow the L-X alpha T-4 relation for our mass estimate. At the outburst peaks, the source radiates near the Eddington limit. The accretion rate then stays constant around 4 x 10(-4) M-circle dot yr(-1) for several days and then decreases exponentially. Such "plateaus" in the accretion rate could be evidence that enhanced mass-transfer rate is the driving outburst mechanism in HLX-1. We also report on the new outburst observed in 2011 August by the Swift X-Ray Telescope. The time of this new outburst further strengthens the similar to 1 year recurrence timescale.
引用
收藏
页数:12
相关论文
共 60 条
[1]   SLIM ACCRETION DISKS [J].
ABRAMOWICZ, MA ;
CZERNY, B ;
LASOTA, JP ;
SZUSZKIEWICZ, E .
ASTROPHYSICAL JOURNAL, 1988, 332 (02) :646-658
[2]  
ABRAMOWICZ MA, 2010, ASTRON ASTROPHYS, V521, P15
[3]   DETECTION OF IMBHs WITH GROUND-BASED GRAVITATIONAL WAVE OBSERVATORIES: A BIOGRAPHY OF A BINARY OF BLACK HOLES, FROM BIRTH TO DEATH [J].
Amaro-Seoane, Pau ;
Santamaria, Lucia .
ASTROPHYSICAL JOURNAL, 2010, 722 (02) :1197-1206
[4]  
[Anonymous], A A
[5]  
Arnaud KA, 1996, ASTR SOC P, V101, P17
[6]   THE EVOLUTION OF VISCOUS DISKS .1. MASS-TRANSFER VARIATIONS [J].
BATH, GT ;
PRINGLE, JE .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1981, 194 (03) :967-986
[7]   A unified model for the spectral variability in GRS 1915+105 [J].
Belloni, T ;
Mendez, M ;
King, AR ;
vanderKlis, M ;
vanParadijs, J .
ASTROPHYSICAL JOURNAL, 1997, 488 (02) :L109-L112
[8]   Intermediate Mass Black Holes and Nearby Dark Matter Point Sources: A Critical Reassessment [J].
Bringmann, Torsten ;
Lavalle, Julien ;
Salati, Pierre .
PHYSICAL REVIEW LETTERS, 2009, 103 (16)
[9]  
CASH W, 1979, ASTROPHYS J, V228, P939, DOI 10.1086/156922
[10]   The nature of accreting black holes in nearby galaxy nuclei [J].
Colbert, EJM ;
Mushotzky, RF .
ASTROPHYSICAL JOURNAL, 1999, 519 (01) :89-107