Properties of longitudinal flux tube waves

Free access article

Issue		A&A Volume 424, Number 3, September IV 2004


Page(s)		1003 - 1010
Section		Stellar atmospheres
DOI		http://dx.doi.org/10.1051/0004-6361:20040497

A&A 424, 1003-1010 (2004)
DOI: 10.1051/0004-6361:20040497

III. Wave propagation in solar and stellar wind flows

M. Cuntz¹ and S. T. Suess²

¹ Department of Physics, Science Hall, University of Texas at Arlington (UTA), Arlington, TX 76019-0059, USA
e-mail: cuntz@uta.edu
² NASA Marshall Space Flight Center, Space Science Laboratory, Mail Stop SD 50, Huntsville, AL 35812, USA
e-mail: steven.t.suess@nasa.gov

(Received 22 March 2004 / Accepted 25 May 2004)

Abstract
We discuss the analytic properties of longitudinal tube waves taking into account ambient wind flows. This is an extension of the studies of Papers I and II, which assumed a mean flow speed of zero and also dealt with a simplified horizontal pressure balance. Applications include the study of longitudinal flux tube waves in stars with significant mass loss and the heating and dynamics of plumes in the solar wind. Slow magnetosonic waves, also called longitudinal waves, have been observed in solar plumes and are likely an important source of heating. We show that the inclusion of ambient wind flows considerably alters the limiting shock strength as well as the energy damping length of the waves.

Key words: magnetohydrodynamics (MHD) -- shock waves -- Sun: solar wind -- stars: winds, outflows

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