Volume 437, Number 3, July III 2005
|Page(s)||1007 - 1015|
|Section||Stellar structure and evolution|
|Published online||30 June 2005|
Spectra of black-hole binaries in the low/hard state: From radio to X-rays
University of Crete, Physics Department, PO Box 2208, 710 03, Heraklion, Crete, Greece e-mail: email@example.com Foundation for Research and Technology-Hellas, 711 10, Heraklion, Crete, Greece
Accepted: 21 March 2005
We propose a jet model for the low/hard state of Galactic black-hole X-ray sources that can explain the energy spectra from radio to X-rays. The model assumes that i) there is a magnetic field along the axis of the jet; ii) the electron density in the jet drops inversely proportional to distance; and iii) the electrons in the jet follow a power law distribution function. We have performed Monte Carlo simulations of Compton upscattering of soft photons from the accretion disk and have found power-law high-energy spectra with photon-number index in the range 1.5-2 and cutoff at a few hundred keV. The spectrum at long wavelengths (radio, infrared, optical) is modeled to come from synchrotron radiation of the energetic electrons in the jet. We find flat to inverted radio spectra that extend from the radio up to about the optical band. For magnetic field strengths of the order of G at the base of the jet, the calculated spectra agree well in slope and flux with the observations. Our model has the advantage over other existing models that it also explains many of the existing timing data such as the time lag spectra, the hardening of the power density spectra and the narrowing of the autocorrelation function with increasing photon energy.
Key words: accretion, accretion disks / black hole physics / radiation mechanisms: non-thermal / methods: statistical / X-rays: stars
© ESO, 2005
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