By Rob Fender, Tomaso Belloni, Elena Gallo (auth.), T. J. Maccarone, R. P. Fender, L. C. Ho (eds.)

This quantity brings jointly contributions from a few of the world's prime specialists on black gap accretion. The papers inside characterize a part of a brand new circulation to use the relative merits of learning stellar mass and supermassive black holes and to collect the data won from the 2 ways. the themes mentioned the following run the gamut of the cutting-edge in black gap observational and theoretical work-variability, spectroscopy, disk-jet connections, and multi-wavelength campaigns on black holes are all covered.

Reprinted from ASTROPHYSICS AND house technology, 300:1-3 (2005)

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Extra info for Astrophysics and Space Science: From X-Ray Binaries to Quasars: Black Holes on all Mass Scales

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J. ), The Central Kiloparsec of Starbursts and AGN: The La Palma Connection, ASP Conference Series, Vol. 249, p. 335. S. : 1996, ApJS 102, 309. Narayan, R. : 1995, ApJ 444, 231. M. : 2002, ApJ 580, 960. : 2004, American Astronomical Society, HEAD meeting, Vol. 8, p. 10. , Venturi, T. , Morganti, R. : 2003, ApJ 585, 677. D. : 1982, Nature 295, 17. , Maiolino, R. : 1999, ApJ 522, 157. A. : 1993, ApJS 89, 1. M. : 1995, PASP 107, 803. : 1992, ApJS 79, 49. , Quataert, E. : 2003, ApJ 598, 301. JET-DISC COUPLING IN THE ACCRETING BLACK HOLE XTE J1118+480∗ JULIEN MALZAC1 , ANDREA MERLONI2 and ANDREW C.

In this paper I propose that the inner part of a black hole accretion inflow (<100 rg ) may enter a magnetically dominated, magnetosphere-like phase in which the strong, well-ordered fields play a more important role than weak, turbulent fields. In the low/hard state this flow is interior to the standard ADAF usually invoked to explain the observed hot, optically thin emission. Preliminary solutions for these new MDAFs are presented. Time-dependent X-ray and radio observations give considerable insight into these processes, and a new interpretation of the X-ray power spectrum (as arising from many disk radii) may be in order.

Unfortunately, there are major uncertainties in this determination, mainly because the jet radiative efficiency is not known. The jet is expected to be a poor radiator because most of the energy is lost in adiabatic expansion. Thus, although the radiation from the jet represents a small fraction of the bolometric luminosity the jet could dominate the energetics. 01 would already imply that the total jet power dominates over the X-ray luminosity. 1, corresponding to a jet efficiency j 3 × 10−3 . There are additional independent arguments in favour of jet dominance in low/hard state sources and in XTE J1118+480 in particular.

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