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Identification of Shocks in the Spectra from Black Holes

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Abstract

We study the spectral properties of a low angular momentum flow as a function of the shock strength, compression ratio, accretion rate and flow geometry. In the absence of a satisfactory description of magnetic fields inside the advective disk, we consider the presence of only stochastic fields and use the ratio of the field energy density to the gravitational energy density as a parameter. We not only include ‘conventional’ synchrotron emission and Comptonization by Maxwell-Boltzmann electrons in the gas, but we also compute these effects due to power-law electrons. For strong shocks, a bump is produced due to the post-shock flow. Power-law spectral components due to the thermal and non-thermal electrons appear after this bump.

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Authors and Affiliations

  1. Centre for Space Physics, Chalantika, Garia Station Road, Kolkata, India

    Samir Mandal & Sandip Kumar Chakrabarti

  2. S.N. Bose National Centre for Basic Sciences, JD Block, Salt Lake, Kolkata, India

    Sandip Kumar Chakrabarti

Authors
  1. Samir Mandal
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  2. Sandip Kumar Chakrabarti
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Correspondence to Samir Mandal.

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Mandal, S., Chakrabarti, S.K. Identification of Shocks in the Spectra from Black Holes. Astrophys Space Sci 297, 269–274 (2005). https://doi.org/10.1007/s10509-005-7629-3

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  • DOI: https://doi.org/10.1007/s10509-005-7629-3

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