Accretion shock signatures in the spectrum of two-temperature advective flows around black holes

Details Accretion shock signatures in the spectrum of two-temperature advective flows around black holes Accretion shock signatures in the spectrum of two-temperature advective flows around black holes

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...434..839m&link_type=abstract

Astronomy and Astrophysics, Volume 434, Issue 3, May II 2005, pp.839-848

Physics

15

Black Hole Physics, Accretion, Accretion Disks, Hydrodynamics, Radiative Transfer, Shock Waves

Scientific paper

The centrifugal barrier supported boundary layer (CENBOL) of a black hole affects the spectrum exactly in the same way the boundary layer of a neutron star does. The CENBOL is caused by standing or oscillating shock waves that accelerate electrons very efficiently and produce a power-law distribution. The accelerated particles in turn emit synchrotron radiation in the presence of the magnetic field. We study the spectral properties of an accretion disk as a function of shock strength, compression ratio, flow accretion rate and flow geometry. In the absence of a satisfactory description of magnetic fields inside the advective disk, we only consider the stochastic fields and use the ratio of field energy density to gravitational energy density as a parameter. Not surprisingly, stronger fields produce larger humps due to synchrotron radiation. We not only include “conventional” synchrotron emission and Comptonization due to Maxwell-Boltzmann electrons in the gas, but also compute the effects of power-law electrons. For strong shocks, a bump is produced just above the synchrotron self-absorption frequency at ν_bump ˜ ν_inj [1+4/3 {R-1}/{R} {1}/{x_s1/2}]x_s^{1/2}, where, ν_inj is the frequency of the dominant photons from the pre-shock flow, and R the compression ratio of the shock located at x_s. For strong shocks, a bump at a higher frequency appears predominantly due to the power-law electrons formed at the shock front.

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