Numerical Modelling of Slow Standing Waves in a Solar Coronal Loop

Details Numerical Modelling of Slow Standing Waves in a Solar Coronal Loop Numerical Modelling of Slow Standing Waves in a Solar Coronal Loop

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.3.59j&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

In the paper we numerically investigate slow standing waves that are impulsively generated in a solar coronal loop by the pressure and density pulse. The solved problem is considered as one- and two-dimensional and the results from both models are compared and discussed. The corresponding computer models are described by the ideal magnetohydrodynamic equations that are solved numerically on uniformly structured mesh by means of the Lax-Wendroff and flux limiter algorithms. The obtained numerical results show a time evolution of the velocity, mass density, pressure or plasma energy density in the model. Further results are the spatial profiles of velocity in fundamental or first harmonic modes, depending on the position of initial perturbations in the coronal loop, and for various positions in the work area. Our presented work is aimed at the explanation of coronal oscillations and its attenuation. These calculations are very important for the explanation of the problem of coronal heating and mechanisms of solar coronal oscillations. It is also important for an interpretation of observations because the density perturbations can produce corresponding perturbations in EUV or thermal X-ray emissions.

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