|
|
|
|
LEADER |
02874 am a22003013u 4500 |
001 |
93894 |
042 |
|
|
|a dc
|
100 |
1 |
0 |
|a Homan, Jeroen
|e author
|
100 |
1 |
0 |
|a MIT Kavli Institute for Astrophysics and Space Research
|e contributor
|
100 |
1 |
0 |
|a Homan, Jeroen
|e contributor
|
700 |
1 |
0 |
|a Fridriksson, Joel K.
|e author
|
700 |
1 |
0 |
|a Jonker, P. G.
|e author
|
700 |
1 |
0 |
|a Russell, David M.
|e author
|
700 |
1 |
0 |
|a Gallo, Elena
|e author
|
700 |
1 |
0 |
|a Kuulkers, Erik
|e author
|
700 |
1 |
0 |
|a Rea, Nanda
|e author
|
700 |
1 |
0 |
|a Altamirano, Diego
|e author
|
245 |
0 |
0 |
|a THE X-RAY PROPERTIES OF THE BLACK HOLE TRANSIENT MAXI J1659-152 IN QUIESCENCE
|
260 |
|
|
|b Institute of Physics/American Astronomical Society,
|c 2015-02-06T16:07:14Z.
|
856 |
|
|
|z Get fulltext
|u http://hdl.handle.net/1721.1/93894
|
520 |
|
|
|a We present new Chandra X-ray observations of the transient black hole X-ray binary MAXI J1659-152 in quiescence. These observations were made more than one year after the end of the source's 2010-2011 outburst. We detect the source at a 0.5-10 keV flux of 2.8(8) × 10[superscript -15] erg s[superscript -1] cm[superscript -2], which corresponds to a luminosity of ~1.2 × 10[superscript 31] (d/6 kpc)[superscript 2] erg s[superscript -1]. This level, while being the lowest at which the source has been detected, is within factors of ~2 of the levels seen at the end of the initial decay of the outburst and soon after a major reflare of the source. The quiescent luminosity of MAXI J1659-152, which is the shortest-orbital-period black hole X-ray binary (~2.4 hr), is lower than that of neutron-star X-ray binaries with similar periods. However, it is higher than the quiescent luminosities found for black hole X-ray binaries with orbital periods ~2-4 times longer. This could imply that a minimum quiescent luminosity may exist for black hole X-ray binaries, around orbital periods of ~5-10 hr, as predicted by binary-evolution models for the mass transfer rate. Compared to the hard state, we see a clear softening of the power-law spectrum in quiescence, from an index of 1.55(4) to an index of 2.5(4). We constrain the luminosity range in which this softening starts to (0.18-6.2) × 10[superscript -5] (d/6 kpc)[superscript 2] (M/8 M ☉) L [subscript Edd], which is consistent with the ranges inferred for other sources.
|
520 |
|
|
|a European Commission (Marie Curie Curie Intra-European Fellowship within the 7th European Community Framework Programme, contract No. IEF 274805)
|
520 |
|
|
|a United States. National Aeronautics and Space Administration (NASA Chandra award No. GO1-120498)
|
520 |
|
|
|a United States. National Aeronautics and Space Administration (NASA Chandra award No. GO2-13061X)
|
520 |
|
|
|a United States. National Aeronautics and Space Administration (contract NAS8-03060)
|
546 |
|
|
|a en_US
|
655 |
7 |
|
|a Article
|
773 |
|
|
|t Astrophysical Journal
|