Application of a relativistic accretion disc model to X-ray spectra of LMC X-1 and GRO J1655-40

Details Application of a relativistic accretion disc model to X-ray spectra of LMC X-1 and GRO J1655-40 Application of a relativistic accretion disc model to X-ray spectra of LMC X-1 and GRO J1655-40

2001-03-22

arxiv.org/abs/astro-ph/0103362v1

Mon.Not.Roy.Astron.Soc. 325 (2001) 1253

Astronomy and Astrophysics

Astrophysics

13 pages, 8 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2001.04540.x

We present a general relativistic accretion disc model and its application to the soft-state X-ray spectra of black hole binaries. The model assumes a flat, optically thick disc around a rotating Kerr black hole. The disc locally radiates away the dissipated energy as a blackbody. Special and general relativistic effects influencing photons emitted by the disc are taken into account. The emerging spectrum, as seen by a distant observer, is parametrized by the black hole mass and spin, the accretion rate, the disc inclination angle and the inner disc radius. We fit the ASCA soft state X-ray spectra of LMC X-1 and GRO J1655-40 by this model. We find that having additional limits on the black hole mass and inclination angle from optical/UV observations, we can constrain the black hole spin from X-ray data. In LMC X-1 the constrain is weak, we can only rule out the maximally rotating black hole. In GRO J1655-40 we can limit the spin much better, and we find 0.68 < a < 0.88. Accretion discs in both sources are radiation pressure dominated. We don't find Compton reflection features in the spectra of any of these objects.

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