Dynamics and heating of the magnetic network on the Sun
Efficiency of mode transformation
Indian Institut of Astrophysics, Bangalore-560034, India e-mail: email@example.com
2 Institut für Theoretische Astrophysik, Tiergartenstr. 15, 69121 Heidelberg, Germany e-mail: firstname.lastname@example.org
Accepted: 20 April 2004
We aim to identify the physical processes which occur in the magnetic network of the chromosphere and which contribute to its dynamics and heating. Specifically, we study the propagation of transverse (kink) MHD waves which are impulsively excited in flux tubes through footpoint motions. When these waves travel upwards, they get partially converted to longitudinal waves through nonlinear effects (mode coupling). By solving the nonlinear, time-dependent MHD equations we find that significant longitudinal wave generation occurs in the photosphere typically for Mach numbers as low as 0.2 and that the onset of shock formation occurs at heights of about 600 km above the photospheric base. We also investigate the compressional heating due to longitudinal waves and the efficiency of mode coupling for various values of the plasma β, that parameterises the magnetic field strength in the network. We find that this efficiency is maximum for field strengths corresponding to , when the kink and tube wave speeds are almost identical. This can have interesting observational implications. Furthermore, we find that even when the two speeds are different, once shock formation occurs, the longitudinal and transverse shocks exhibit strong mode coupling.
Key words: Sun: magnetic fields / Sun: oscillations / Sun: chromosphere
© ESO, 2004