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Galactic nuclei luminosity: A model of steady spherically-symmetric accretion of optically-thick gas on to Kerr black holes

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Abstract

Stationary spherically-symmetric accretion on to Kerr black holes is studied. A theoretical model has been developed in which the relativistic equations of continuity, conservation of four-momentum, local energy balance, and synchrotron radiative transfer have been integrated, by means of a combination of analytical and numerical procedures. A special emphasis has been put on evaluating the outcoming fluxes, as they can be compared with observations. Calculations were performed for masses of black holes in galactic nuclei, 106 M ⊙ as representative of the hypothetical black hole in the nucleus of the Milky Way and 107 M ⊙ as representative of a moderate Seyfert nucleus. The emergent spectra differ considerably from observations, as they are severely modified by dust in more external regions. The total frequency-integrated luminosity is, however, in very good agreement with observations.

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Authors and Affiliations

  1. Cátedra de Astrofísica, Facultad de Ciencias, Granada, Spain

    C. Perán & E. Battaner

  2. Instituto de Astrofísica de Andalucía, C.S.I.C., Granada, Spain

    C. Perán & E. Battaner

Authors
  1. C. Perán
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  2. E. Battaner
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Perán, C., Battaner, E. Galactic nuclei luminosity: A model of steady spherically-symmetric accretion of optically-thick gas on to Kerr black holes. Astrophys Space Sci 127, 1–7 (1986). https://doi.org/10.1007/BF00637755

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  • DOI: https://doi.org/10.1007/BF00637755

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