Observational evidence for a high-energy Compton cloud in GRO J1655-40 under a high accretion rate

Yoshihito Kobayashi, Aya Kubota, Kazuhiro Nakazawa, Tadayuki Takahashi, Kazuo Makishima

Research output: Contribution to journalArticlepeer-review

13 Citations (Scopus)


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 40-150 keV X-ray luminosity, L40-150. six typical spectra were selected and analyzed. When L40-150 is sufficiently below ∼ 5 × 1036erg s-1 (assuming a distance of 3.2 kpc and an isotropic emission), the 3-150 keV PCA/HEXTE spectra are well described by a standard spectral model consisting of an optically-thick disk spectrum and a power-law tail. When 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 energy at 190-300 keV. 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 70-85 keV 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.

Original languageEnglish
Pages (from-to)273-279
Number of pages7
JournalPublications of the Astronomical Society of Japan
Issue number1
Publication statusPublished - 2003
Externally publishedYes


  • Accretion, accretion disks
  • Black hole physics
  • Stars: individual (GRO J1655-40)
  • X-rays: stars

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


Dive into the research topics of 'Observational evidence for a high-energy Compton cloud in GRO J1655-40 under a high accretion rate'. Together they form a unique fingerprint.

Cite this