Abstract
Based on the spectropolarimetric data of 33 Seyfert type 1 galaxies observed with the BTA-6m telescope of the Special Astrophysical Observatory, we estimated the magnetic field values at the event horizon of the supermassive black hole BH and the exponents of the power-law dependence s of the magnetic field on the radius. We used the model of optically thick geometrically thin Shakura–Sunyaev accretion disk. The average value of logBH[G] was found to be ∼4, which is in good agreement with the results obtained by other methods. The average value of s is s≈1.7, and its distribution maximum span is in the range od 1.85<s<2.0. This is a rather interesting result, since s=5/4 is usually adopted in calculations for Shakura–Sunyaev accretion disks. In addition, for two objects PG 1545+210 and 2MASX J06021107+2828382, the measured degree of polarization is greater than the maximum possible value at the angle between the line of sight and the axis of the accretion disk i=45°. It was concluded that for these objects the angle should be closer to i=60°.
Highlights
According to modern concepts, accretion disks of active galactic nuclei (AGNs) should have an intense magnetic field [1,2]
It is assumed that the magnetic field is formed as a result of the interaction of accreting matter with a rotating supermassive black hole (SMBH) [3,4,5,6,7,8]
We calculated the value of the polarization and the positional angle as a function of the value of the magnetic field intensity at the event horizon BH and the parameter s in the visible range
Summary
Accretion disks of active galactic nuclei (AGNs) should have an intense magnetic field [1,2]. Several mechanisms for the origin of the observed polarization are discussed, for example, the light scattering in accretion disks or synchrotron radiation of charged particles. These mechanisms can act in different structures, such as the plane and warped accretion disks, toroidal rings near the accretion disks and relativistic jets. It happens that different models are proposed to explain the same source. For objects of the type under study, the most popular and simple model is the optically thick geometrically thin
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