Magnetic fields in the accretion disks for various inner boundary conditions

¹ Space Research and Technology Institute, Bulgarian Academy of Sciences, Acad G. Bonchev St., Bl. 1, 1113 Sofia, Bulgaria
e-mail: danvasan@space.bas.bg
² M. V. Lomonosov Moscow State University, Leninskie gori, Bl.1, 119991 Moscow, Russia
e-mail: ea.mikhajlov@physics.msu.ru
³ Moscow Center of Fundamental and Applied Mathematics, Leninskie gori, Bl.1, 119991 Moscow, Russia
⁴ P. N. Lebedev Physical Institute, Leninskiy Prospekt, Bl.53, 119333 Moscow, Russia
⁵ N. V. Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Kaluzhskoe Hwy., Bl.4, 108840 Troitsk, Moscow, Russia
e-mail: sololoff.dd@gmail.com

Received: 17 June 2020
Accepted: 2 May 2021

Abstract

Context. The magnetic fields of accretion disks play an important role in studying their evolution. We may assume that its generation is connected to the dynamo mechanism, which is similar with that in the galactic disks.

Aims. Here, we propose a model of the magnetic field of the accretion disk that uses the same approaches that have been used for galaxies. It is necessary to obtain the field, which is expected to be less than the equipartition value, and without destroying the disk. To do so, it is necessary to formulate the basic properties of the ionized medium and to estimate the parameters governing the dynamo.

Methods. We used the no-z approximation that has been developed for thin disks. We also take different boundary conditions that can change the value of the field significantly.

Results. We show that the magnetic field strictly depends on the boundary conditions. Taking zero conditions and the fixed magnetic field condition on the inner boundary, which are connected to the physical properties of the accretion disk, we can avoid solutions that are greater than the equipartition field.