The magnetic-field structure in a stationary accretion disk


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Аннотация

The magnetic-field structure in regions of stationary, planar accretion disks around active galactic nuclei where general-relativistic effects can be neglected (from 10 to 200 gravitational radii) is considered. It is assumed that the magnetic field in the outer edges of the disk, which forms in the magnetosphere of the central black hole during the creation of the relativisitic jets, corresponds to the field of a magnetic dipole perpendicular to the plane of the disk. In this case, the azimuthal field component Bφ in the disk arises due to the presence of the radial field Bρ and the azimuthal velocity component Uφ. The value of the magnetic field at the inner radius of the disk is taken to correspond to the solution of the induction equation in a diffusion approximation. Numerical solutions of the induction equation are given for a number of cases.

Авторлар туралы

M. Piotrovich

Central (Pulkovo) Astronomical Observatory

Хат алмасуға жауапты Автор.
Email: mpiotrovich@mail.ru
Ресей, Pulkovskoye shosse 65, St. Petersburg, 196140

N. Silant’ev

Central (Pulkovo) Astronomical Observatory

Email: mpiotrovich@mail.ru
Ресей, Pulkovskoye shosse 65, St. Petersburg, 196140

Yu. Gnedin

Central (Pulkovo) Astronomical Observatory

Email: mpiotrovich@mail.ru
Ресей, Pulkovskoye shosse 65, St. Petersburg, 196140

T. Natsvlishvili

Central (Pulkovo) Astronomical Observatory

Email: mpiotrovich@mail.ru
Ресей, Pulkovskoye shosse 65, St. Petersburg, 196140

S. Buliga

Central (Pulkovo) Astronomical Observatory

Email: mpiotrovich@mail.ru
Ресей, Pulkovskoye shosse 65, St. Petersburg, 196140

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