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Conditions and mechanisms for growth of large-scale magnetic field in outer parts of galactic disks
Khasaeva T. T.1,2, Mikhailov E. A.
1,3
1Lomonosov Moscow State University, Moscow, Russia
2Institute of Earthquake Prediction Theory and Mathematical Geophysics Russian academy of sciences, Moscow, Russia
3Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia
2Institute of Earthquake Prediction Theory and Mathematical Geophysics Russian academy of sciences, Moscow, Russia
3Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia
Email: justanyan@yandex.ru, ea.mikhajlov@physics.msu.ru
The generation and evolution of magnetic fields in spiral galaxies is traditionally described by the dynamo mechanism. Most studies focus on magnetic fields at moderate distances from the center of the galactic disk. However, the existence of a galactic magnetic field in the peripheral regions of the galactic disk is confirmed by numerical models. To estimate the scale of the magnetic field in the outer regions of a spiral galaxy, an eigenvalue problem can be solved based on previously used equations. The first eigenvalues and eigenfunctions for this problem are presented. The eigenvalues can be found both theoretically and numerically. Keywords: dynamo, galaxies, magnetism, perturbation theory.
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