Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.244..714c&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 244, June 15, 1990, p. 714-726.
Astronomy and Astrophysics
Astronomy
37
Cosmic Gases, Density Wave Model, Disk Galaxies, Interstellar Magnetic Fields, Density Distribution, Dynamo Theory, Spiral Galaxies, Velocity Distribution
Scientific paper
The present investigation of the process of magnetic-field generation in a galactic disk holding a spiral structure examines the effect of gaseous velocity fields' density-wave perturbations on galactic dynamos. Attention is given to parametric resonance, which enhances the field growth due to simple dynamos; this mechanism is analogous to the parametric excitation of a swing with a periodic change of gravity center, and is therefore called the 'swing excitation' of galactic fields. In a nonaxisymmetric case, the net effect of resonance is greatest when density wave frequency is twice as large as the dynamo wave frequency and the azimuthal wavenumber is half that of a spiral wave. The structure and dominance of bisymmetric-spiral magnetic fields is studied in the framework of the present mechanism for the cases of the M51 and M81 two-armed spiral galaxies.
Chiba Masashi
Tosa Makoto
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