2010A&A...522A..99C


Query : 2010A&A...522A..99C

2010A&A...522A..99C - Astronomy and Astrophysics, volume 522A99-99 (2010/11-1)

The 2009 outburst of H 1743-322 as observed by RXTE.

CHEN Y.P., ZHANG S., TORRES D.F., WANG J.M., LI J., LI T.P. and QU J.L.

Abstract (from CDS):

Six outbursts have been observed by RXTE from the source since 2003. Following ``a failed outburst'' with a missing high/soft state in 2008, the most recent one occurred in 2009, exhibiting all spectral transitions. An outburst was observed by RXTE from the black hole candidate H 1743-322 in 2009. We investigate this particular outburst in the context of the source outburst history. We analyze the RXTE observations of the 2009 outburst of H 1743-322, as well as the observations of the previous five outbursts for comparison. All available RXTE observations taken since 2003 sum up to a total exposure of ∼1200ks. The hardness-intensity diagram (HID) shows a complete counter-clockwise q-track for the 2009 outburst. It leaves the low/hard state but does not reach the leftmost edge of the overall HID. Near maximum, the X-ray spectra show a power law with photon index <2.4; the peak luminosity during the whole outburst reached only 20% of the Eddington luminosity. The highest disk fractional luminosity is about 0.75 for the 2009 outburst, which is close to the lower limit observed from the black hole XRB sample in their state transitions from the intermediate to the high/soft state. While the lowest hardness (6-19keV/3-6keV) values in the HID is about 0.3-0.4 for the 2009 outburst, the timing analysis shows that a transition to the high soft state occurred. During the low/hard state of the 2009 outburst, the inner radius of the accretion disk is found to be closer to the central black hole and anti-correlated with the disk temperature implying reprocessing of the hot corona on the disk's soft X-rays. In the luminosity diagram of the corona versus the disk, the tracks of the outbursts in 2003 and 2009 cross the line which represents a roughly equal contribution to the emission from the thermal and the non-thermal components; the track of the 2008 outburst has its turn-over falling on this line. This may indicate an emission balance between the corona and the disk that prevents the state transition from going further than the low/hard state.

Abstract Copyright: ∼

Journal keyword(s): X-rays: binaries - X-rays: stars - X-rays: individual: H 1743-322 - black hole physics

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 V* KV UMa HXB 11 18 10.7930420496 +48 02 12.314730120           K5V-M1V 865 0
2 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000           K3III 1254 0
3 V* V1033 Sco HXB 16 54 00.1423963019 -39 50 44.761701340       16.14   F3-6IV 1980 0
4 V* V821 Ara LXB 17 02 49.3876391280 -48 47 23.087954544         15.322 ~ 2237 0
5 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 805 0
6 2MAXI J1753-013 LXB 17 53 28.2898766424 -01 27 06.256555272 15.30 16.73 16.46 16.15 15.64 ~ 384 0
7 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2810 0
8 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4590 0

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