Excitation of transverse magnetic tube waves in stellar convection zones

Free access article

Issue		A&A Volume 386, Number 2, May I 2002


Page(s)		606 - 614
Section		Stellar atmospheres
DOI		http://dx.doi.org/10.1051/0004-6361:20011834

A&A 386, 606-614 (2002)
DOI: 10.1051/0004-6361:20011834

II. Wave energy spectra and fluxes

Z. E. Musielak^{1, 2} and P. Ulmschneider²

¹ Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA
² Institut für Theoretische Astrophysik der Universität Heidelberg, Tiergartenstr. 15, 69121 Heidelberg, Germany

(Received 4 July 2001 / Accepted 20 December 2001 )

Abstract
The wave energy spectra and fluxes for transverse magnetic tube waves generated in stellar convection zones are computed by using the analytical method developed in the previous paper of this series. The main physical process responsible for the generation of these waves is shaking of a thin and vertically oriented magnetic flux tube by the external turbulent convection. The approach includes the correlation effects, which occur when the tube is shaken over a significant fraction of its length, but is limited to linear waves. The calculations are performed for population I stars with effective temperatures ranging from $T_{\rm eff}$ = 2000 K to 10 000 K, and with gravities log g = 3-5. It is shown that the fluxes carried by linear transverse waves along a single flux tube are approximately one order of magnitude higher than those carried by linear longitudinal tube waves. The obtained results can be used to construct theoretical models of stellar chromospheres and winds.

Key words: methods: analytical -- stars: chromospheres -- stars: coronae -- stars: magnetic fields -- MHD -- waves

Offprint request: P. Ulmschneider, ulmschneider@ita.uni-heidelberg.de

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