Numerical simulations of MHD waves in solar coronal loops

Mag Selwa, UMCS Lublin, Poland

The universe was always an object of our fascination. Because the Sun
is our nearest star naturally a long time ago it became an object of our
extensive observations. Nowadays, investigations of the Sun are carried by
means of observations in a wide range of wavelengths by various
instruments, having different spatial and temporal resolutions, and by
theoretical modeling. That makes possible to observe many physical
phenomena with a wide range of time scales (from seconds to a dozen of
minutes). However, observations do not explain the nature of those
phenomena and observational findings should be verified theoretically. One
model that describes solar plasma is magnetohydrodynamics (MHD).
Unfortunately, due to its intrinsic complexity MHD equations cannot be
solved analytically. As a consequence of that we adopt several numerical
codes (e.g. FLASH, CLAWPACK and VAC/AMRVAC) which are capable
of solving MHD equations with a use of different numerical methods,
parallel computation, and adaptive mesh refinement. Application of these
codes will be presented for the case of 1d, 2d or 3d models of coronal
loops with a straight or curved geometry and impulsive generation of
propagating or standing magnetosonic waves.