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Astron. Astrophys. 345, 1038-1048 (1999)


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Numerical simulation of prominence oscillations

N.A.J. Schutgens 1 and G. Tóth 2

1 Atmospheric Research, KNMI, P.O. Box 201, 3730 AE De Bilt, The Netherlands
2 Department of Atomic Physics, Eötvös University, Hungary

Received 19 May 1998 / Accepted 26 October 1998

Abstract

We present numerical simulations, obtained with the Versatile Advection Code, of the oscillations of an inverse polarity prominence. The internal prominence equilibrium, the surrounding corona and the inert photosphere are well represented. Gravity and thermodynamics are not taken into account, but it is argued that these are not crucial. The oscillations can be understood in terms of a solid body moving through a plasma. The mass of this solid body is determined by the magnetic field topology, not by the prominence mass proper. The model also allows us to study the effect of the ambient coronal plasma on the motion of the prominence body. Horizontal oscillations are damped through the emission of slow waves while vertical oscillations are damped through the emission of fast waves.

Key words: Magnetohydrodynamics (MHD) – Sun: corona – Sun: magnetic fields – Sun: oscillations – Sun: photosphere – Sun: prominences

Send offprint requests to: Nick Schutgens (schutgen@knmi.nl)

© European Southern Observatory (ESO) 1999

Online publication: April 28, 1999

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