Swing amplification of fast and slow density waves in thin magnetized gaseous discs

Details Swing amplification of fast and slow density waves in thin magnetized gaseous discs Swing amplification of fast and slow density waves in thin magnetized gaseous discs

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.291...91f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 291, Issue 1, pp. 91-109.

Astronomy and Astrophysics

Astronomy

41

Gravitation, Mhd, Polarization, Galaxies: Spiral, Galaxies: Structure, Radio Continuum: Galaxies

Scientific paper

The excitation and time evolution of magnetohydrodynamic (MHD) density waves are studied in a differentially rotating thin gaseous disc embedded with an azimuthal magnetic field. This analysis shows that both fast and slow MHD density waves are amplified when they swing from leading to trailing configurations, but the amplification factors of fast and slow MHD density waves depend differently on the disc differential rotation. Fast MHD density waves tend to be excited in discs of strong differential rotation, while slow MHD density waves are expected to manifest preferentially in discs of almost rigid rotation. Surface mass density and magnetic field perturbations associated with fast MHD density waves are roughly in phase. A distinct feature of slow MHD density waves is that at a fixed spatial point, there is a significant phase difference delta (i.e. pi/2

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