Volume 495, Number 1, February III 2009
|Page(s)||313 - 318|
|Published online||22 December 2008|
Slow magnetoacoustic standing waves in a curved solar coronal slab
Department of Computer Sciences, The State School of Higher Education in Chełm, ul. Pocztowa 54, 22-100 Chełm, Poland e-mail: firstname.lastname@example.org
2 Group of Astrophysics and Gravity Theory, UMCS, ul. Radziszewskiego 10, 20-031 Lublin, Poland
3 Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany
Accepted: 1 October 2008
Aims. We consider a model of a two-dimensional solar coronal arcade to explore the effects of a curved magnetic field topology on excitation and attenuation of slow magnetoacoustic standing waves.
Methods. The time-dependent ideal magnetohydrodynamic equations are solved numerically to find the spatial and temporal signatures of these waves.
Results. A pulse in gas pressure initially launched at a loop footpoint excites the fundamental mode of slow magnetoacoustic standing waves. The typical excitation time of such a wave mode is 2.5 wave periods, with a similar attenuation timescale. These values are remarkably similar to those recovered from observations by SOHO/SUMER in an Fe XIX line.
Conclusions. Slow magnetoacoustic standing waves are excited and attenuated more efficiently in curved magnetic field lines than in a straight magnetic slab topology. The waves supported by the magnetic arcade are in far closer agreement with observations.
Key words: Sun: corona / Sun: oscillations / Sun: magnetic fields / magnetohydrodynamics (MHD)
© ESO, 2009
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