Abstract
Various relations are found between the key parameters of black holes and active galactic nuclei. Some have a statistical property, others follow from the theoretical consideration of the evolution of these objects. In this paper we use a recently discovered empirical relation between the characteristic frequency of quasi-periodic oscillations of radiation ν br of black holes, their masses and matter accretion rates to determine the magnetic field strength B H at the black hole event horizon. Since the characteristic frequency can be determined from observations, the use of a new relation for the estimations of magnetic field B H can yield more definite results, since we are decreasing the number of the unknown or poorly-determined parameters of objects (it especially concerns the accretion rate Ṁ). The typical values which we have found are B H ≃ 108G for the stellar mass black holes, and B H ≃ 104G for the supermassive black holes. Besides, we demonstrate that if the linear polarization of an object is caused by the radiation of a magnetized accretion disk, then the degree of observable polarization is p ∼ ν −1/2 br .
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Original Russian Text © M.Yu. Piotrovich, N.A. Silant’ev, Yu.N. Gnedin, T.M. Natsvlishvili, 2011, published in Astrofizicheskii Byulleten, 2011, Vol. 66, No. 3, pp. 344–349.
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Piotrovich, M.Y., Silant’ev, N.A., Gnedin, Y.N. et al. Magnetic fields and quasi-periodic oscillations of black hole radiation. Astrophys. Bull. 66, 320–324 (2011). https://doi.org/10.1134/S1990341311030047
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DOI: https://doi.org/10.1134/S1990341311030047