EDP Sciences
Free Access
Volume 387, Number 2, May IV 2002
Page(s) 487 - 496
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20000524

A&A 387, 487-496 (2002)
DOI: 10.1051/0004-6361:20000524

Accretion-ejection instability and QPO in black hole binaries I. Observations

J. Rodriguez, P. Varnière, M. Tagger and Ph. Durouchoux

Service d'Astrophysique (CNRS URA 2052), CEA Saclay, 91191 Gif-sur-Yvette, France

(Received 23 May 2000 / Accepted 25 February 2002)

This is the first of two papers in which we address the physics of the low-frequency Quasi-Periodic Oscillation (QPO) of X-ray binaries, in particular those hosting a black hole. We discuss and repeat the recent analysis and spectral modelling of the micro-quasar GRO J 1655- 40by Sobczak et al. (2000, hereafter SMR), and compare it with GRS  1915+ 105; this leads us to confirm and analyze in more detail the different behavior noted by SMR, between GRO J 1655- 40and other sources, when comparing the correlation between the QPO frequency and the disk inner radius. In a companion paper (Varnière et al. 2000, hereafter Paper II) we will show that these opposite behaviors can be explained in the context of the Accretion-Ejection Instability recently presented by Tagger & Pellat (1999). We thus propose that the difference between GRO J 1655- 40and other sources comes from the fact that in the former, observed in a very high state, the disk inner radius always stays close to the Last Stable Orbit. In the course of this analysis, we also indicate interesting differences between the source properties, when the spectral fits give an anomalously low inner disk radius. This might indicate the presence of a spiral shock or a hot point in the disk.

Key words: accretion, accretion disks -- X-rays: binaries -- stars: individual: GRS 1915+105, GRO J1655-40

Offprint request: J. Rodriguez, rodrigue@discovery.saclay.cea.fr

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