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Title:
Possible oscillation modes of magnetic white dwarfs
Authors:
Lou, Yu-Qing
Affiliation:
AA(Astronomy and Astrophysics Center, The University of Chicago, Chicago, IL 60637, USA )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 275, Issue 2, pp. L11-L15. (MNRAS Homepage)
Publication Date:
07/1995
Origin:
MNRAS; KNUDSEN ttp://www.blackwell-science.com
MNRAS Keywords:
MAGNETIC FIELDS, MHD, WAVES, NOVAE, CATACLYSMIC VARIABLES, STARS: OSCILLATIONS, WHITE DWARFS
Bibliographic Code:
1995MNRAS.275L..11L

Abstract

Observed field strengths of magnetic white dwarfs (MWDs) range from ~0.1 to 1000 MG. In the degenerate interior of an MWD, the sound speed is typically much higher than the Alfven speed. Assuming a simple dipolar magnetic field geometry threading throughout an MWD covered with an extremely thin non-degenerate surface layer atmosphere in radiative equilibrium, we describe basic properties of globally trapped oscillations of Alfven waves, magnetohydrodynamic (MHD) slow waves, magnetoacoustic waves, and magneto-gravity waves. Similar to the excitation of g modes of DA and DB variable white dwarfs, these four types of MHD modes could be self-excited via the kappa-mechanism for an isolated MWD. In cataclysmic variables such as AM Hers, these MHD modes of the primary MWD could be driven to excitation by magnetically channelled accretion flow from the low-mass companion on to the polar regions of the primary MWD. In particular, the excited magneto-acoustic modes with time-scales of ~0.1-10s and magneto-gravity modes with time-scales of ~100-1000s could be responsible for the quasi-periodic oscillations observed in optical and X-ray emissions from AM Hers.

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