Volume 537, January 2012
|Number of page(s)||8|
|Published online||25 January 2012|
Numerical simulations of magnetoacoustic oscillations in a gravitationally stratified solar corona⋆
1 Group of Astrophysics, Institute of Physics, UMCS, ul. Radziszewskiego 10, 20-031 Lublin, Poland
e-mail: email@example.com; firstname.lastname@example.org
2 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
3 Abastumani Astrophysical Observatory at Ilia State University, University St. 2, Tbilisi, Georgia
Received: 24 August 2011
Accepted: 5 November 2011
Aims. We consider magnetoacoustic oscillations in a gravitationally stratified solar corona, that are triggered by an initial pulse in the vertical component of velocity launched from various altitudes of the solar atmosphere.
Methods. We numerically solve two-dimensional magnetohydrodynamic equations for an ideal plasma to determine the spatial and temporal signatures of excited oscillations.
Results. Our numerical results reveal that few-min oscillations are effectively excited by the initial velocity pulses and that their waveperiods depend on the vertical location and amplitude of the pulse.
Conclusions. The building block of this scenario consists of a one-dimensional rebound shock model.
Key words: magnetohydrodynamics (MHD) / Sun: atmosphere / Sun: oscillations
Movies attached to Figs. 5 and 6 are available in electronic form at http://www.aanda.org
© ESO, 2012
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