Volume 526, February 2011
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||04 January 2011|
Generation of longitudinal flux tube waves in theoretical main-sequence stars: effects of model parameters
Faculty of Engineering and Computer Sciences, Izmir University of
2 Department of Physics, Science Hall, University of Texas at Arlington, Arlington, TX 76019, USA
3 Institut für Theoretische Astrophysik, Universität Heidelberg, 69120 Heidelberg, Germany
Received: 21 June 2010
Accepted: 24 October 2010
Aims. We compute the wave energy fluxes carried by longitudinal tube waves along vertically oriented thin magnetic fluxes tubes embedded in the atmospheres of theoretical main-sequence stars based on stellar parameters deduced by Kurucz and Gray. In addition, we present a fitting formula for the wave energy flux based on the governing stellar and magnetic parameters.
Methods. A modified theory of turbulence generation based on the mixing-length concept is combined with the magneto-hydrodynamic equations to numerically account for the wave energies generated at the base of magnetic flux tubes.
Results. The results indicate a stiff dependence of the generated wave energy on the stellar and magnetic parameters in principal agreement with previous studies. The wave energy flux FLTW decreases by about a factor of 1.7 between G0 V and K0 V stars, but drops by almost two orders of magnitude between K0 V and M0 V stars. In addition, the values for FLTW are significantly higher for lower in-tube magnetic field strengths. Both results are consistent with the findings from previous studies.
Conclusions. Our study complements existing descriptions of magnetic energy generation in late-type main-sequence stars. Our results will be helpful for calculating theoretical atmospheric models for stars of different levels of magnetic activity.
Key words: methods: numerical / magnetohydrodynamics (MHD) / stars: chromosphere / stars: magnetic field / stars: solar-type / waves
© ESO, 2011
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