In the high state of black hole candidates, in which 2--10 keV luminosity is relatively high, the energy index of the power-law like hard X-ray emission above ~ 10 keV is typically ~ 1.5. On the other hand, in the low state}, the hard X-ray energy index is 0.3--0.9. In this paper, we suggest that this difference of the hard X-ray spectral slopes may be due to two different Comptonization mechanisms. We propose that, in the high state, the hard component is governed by the Comptonization due to the bulk motion of the almost freely falling (convergent accretion) flow close to the black hole, rather than thermal Comptonization. The spectral slope of the hard component is insensitive to the disk accretion rate governing the soft component, hence is nearly invariant in spite of the soft component variations. The power-law component due to the bulk motion Comptonization has a sharp cut-off at around the electron rest mass energy, which is consistent with high energy observations of the high state. In the low state, the spectrum is formed due to thermal Comptonization of the low-frequency disk radiation by a sub-Keplerian component (possibly undergoing a centrifugally-supported shock) which is originated from the Keplerian disk. In the limit of low disk accretion rate, the power law index is uniquely determined by the mass accretion rate of the sub-Keplerian component.

On the Spectral Slopes of Hard X-Ray Emission from Black Hole Candidates

TITARCHUK, Lev;
1996

Abstract

In the high state of black hole candidates, in which 2--10 keV luminosity is relatively high, the energy index of the power-law like hard X-ray emission above ~ 10 keV is typically ~ 1.5. On the other hand, in the low state}, the hard X-ray energy index is 0.3--0.9. In this paper, we suggest that this difference of the hard X-ray spectral slopes may be due to two different Comptonization mechanisms. We propose that, in the high state, the hard component is governed by the Comptonization due to the bulk motion of the almost freely falling (convergent accretion) flow close to the black hole, rather than thermal Comptonization. The spectral slope of the hard component is insensitive to the disk accretion rate governing the soft component, hence is nearly invariant in spite of the soft component variations. The power-law component due to the bulk motion Comptonization has a sharp cut-off at around the electron rest mass energy, which is consistent with high energy observations of the high state. In the low state, the spectrum is formed due to thermal Comptonization of the low-frequency disk radiation by a sub-Keplerian component (possibly undergoing a centrifugally-supported shock) which is originated from the Keplerian disk. In the limit of low disk accretion rate, the power law index is uniquely determined by the mass accretion rate of the sub-Keplerian component.
Ebisawa, K; Titarchuk, Lev; S. K., Chakrabarti
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11392/532925
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