A unified paradigm for the spectral and temporal evolution of Black Hole X-ray Binaries

Details A unified paradigm for the spectral and temporal evolution of Black Hole X-ray Binaries A unified paradigm for the spectral and temporal evolution of Black Hole X-ray Binaries

2006-11-20

arxiv.org/abs/astro-ph/0611628v1

PoSMQW6:036,2006

Astronomy and Astrophysics

Astrophysics

14 pages, 7 Figures. Contributed talk at the VIth Microquasar Workshop: "Microquasars and beyond" (Como, Italy), eds: T. Bello

Scientific paper

We present a unified picture to explain the spectral states of BH binaries based on the two-flow model. In our view, the central regions have a multi-flow configuration consisting in (1) an outer standard accretion disc (SAD) down to a transition radius $r_{tr}$, (2) an inner magnetized jet emitting disc (JED) below $r_{tr}$ driving (3) a self-collimated non relativistic MHD jet surrounding, when conditions for pair creation are met, (4) a ultra relativistic pair beam. Large values of $r_{tr}$ correspond to Hard states while small values correspond to Soft states. In between these extremes, in the high intermediate state, $r_{tr}$ can reach values that switch on a pair cascade process giving birth to ultra-relativistic pair blobs that explain the superluminal events. In this model the accretion rate but also the disc magnetization $\mu$ play important roles, the latter being necessarily in the range 0.1-1 for the MHD jet to exist. Then, with simple assumptions on $\mu$, we propose an explanation for the hysteresis behavior observed in microquasars during their outburst. We also discuss the nature, in our framework, of the X-ray corona and the origin of the X-ray variability in the hard state. Preliminary results are discussed.

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