Fluctuating governing parameters in galaxy dynamoстатья
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Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 5 декабря 2018 г.
Авторы:
Mikhailov E.A. ,
Pushkarev V.V.
Журнал:
Astronomical and Astrophysical Transactions
Том:
30
Номер:
3
Год издания:
2018
Издательство:
Cambridge Scientific Publishers
Местоположение издательства:
Cambridge
Первая страница:
343
Последняя страница:
350
Аннотация:
Evolution of galaxy magnetic fields is described by the so-called dynamo theory. The equations include governing parameters that describe alpha-effect, differential rotation and turbulent diffusion. Usually these coefficients are connected with average kinematic characteristics of the interstellar medium. This approach is possible for “calm” galaxies. However, if there is intensive star formation, supernova explosions and other active processes, the parameters of the interstellar gas change. The distribution of the regions where the velocities of the interstellar medium are different is quite random. So it is useful to use the model of the galaxy dynamo with random coefficients. Previous papers described fluctuating alpha-effect, but it is necessary to take into account the turbulent diffusion, too. We use the so-called no-z approximation to study the magnetic field. It takes into account that the galaxy disc is thin, so the z-derivatives can be changed by algebraic expressions. We describe the fluctuations of turbulent diffusion coefficients. We have shown that the magnetic field can be changed a lot even for quite small fluctuations of the dynamo governing parameters (associated with weak star formation). For example, the star formation that is several times higher than in the Milky Way can destroy the regular magnetic field. © Cambridge Scientific Publishers and 2018 Astronomical and Astrophysical Transactions (AApTr).
Добавил в систему:
Михайлов Евгений Александрович