Observational Evidence for a High-Energy Compton Cloud in GRO J1655-40 under a High Accretion Rate

Details Observational Evidence for a High-Energy Compton Cloud in GRO J1655-40 under a High Accretion Rate Observational Evidence for a High-Energy Compton Cloud in GRO J1655-40 under a High Accretion Rate

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55..273k&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.1, pp.273-279

Physics

13

Accretion, Accretion Disks, Black Hole Physics, Stars: Individual (Gro J165540), X-Rays: Stars

Scientific paper

Observational results on GRO J1655- 40 are reported, based on the X-ray spectra obtained with the PCA and the HEXTE on-board RXTE during its 1996-1997 outburst. By referring to the 40-150keV X-ray luminosity, L40-150, six typical spectra were selected and analyzed. When L40-150 is sufficiently below ˜ 5 × 1036 erg s-1 (assuming a distance of 3.2kpc and an isotropic emission), the 3-150keV PCA/HEXTE spectra are well described by a standard spectral model consisting of an optically-thick disk spectrum and a power-law tail. L40-150 exceeds 5 × 1036 erg s-1, the standard model fails to reproduce the joint spectrum, due to a mild turn-over in the HEXTE spectrum. Successful fits are recovered when the power-law component is replaced by a broken power-law model with the break energy at ˜ 40 keV, or by an exponentially cutoff power-law model with the cutoff ener gy at 190-300keV. The fits are further improved by employing a thermal Comptonization component, wherein the electron temperature and optical depth of the Compton cloud are estimated to be 70-85keV and 0.45-0.65, respectively. These results provide strong evidence for the existence of thermal high-energy electrons, and reconfirm the picture of strong disk Comptonization.

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