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Spectral problems in galactic dynamo theory: asymptotic and numerical approaches
Mikhailov E.A.
1,2,3, Zheligovsky V. A.
4, Taranyuk A. A.4,2, Frolova M. V.2
1Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia
2Lomonosov Moscow State University, Moscow, Russia
3Moscow Center of Fundamental and Applied Mathematics, Moscow, Russia
4Institute of Earthquake Prediction Theory and Mathematical Geophysics Russian academy of sciences, Moscow, Russia
2Lomonosov Moscow State University, Moscow, Russia
3Moscow Center of Fundamental and Applied Mathematics, Moscow, Russia
4Institute of Earthquake Prediction Theory and Mathematical Geophysics Russian academy of sciences, Moscow, Russia
Email: e.mikhajlov@lebedev.ru, vlad@mitp.ru, taranyuk.anton@gmail.com, pashentceva.mv17@physics.msu.ru
The origin of galactic magnetic fields is described using magnetohydrodynamics and dynamo theory. Two different scales are considered: the microscopic scale, where equations for magnetic field evolution and transport, directly following from Maxwell's equations, are applicable, and the macroscopic scale, where dynamo equations for mean fields are considered after averaging over turbulence scales. Of particular interest are models that take into account the significant thickness of the galactic disk. In all models, the possibility of magnetic field generation is described by a spectrum of corresponding differential operators. Keywords: galaxies, spectra, differential operator, magnetism.
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