2.5d Mhd Simulations Of Winds From Red Giants Stars: Broadband Alfvén Waves

Details 2.5d Mhd Simulations Of Winds From Red Giants Stars: Broadband Alfvén Waves 2.5d Mhd Simulations Of Winds From Red Giants Stars: Broadband Alfvén Waves

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542703a&link_type=abstract

American Astronomical Society, AAS Meeting #215, #427.03; Bulletin of the American Astronomical Society, Vol. 42, p.342

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the numerical simulations of winds from evolved giant stars using a fully non-linear, time dependent, 2.5-dimensional magnetohydrodynamic (MHD) code. This study extends our previous fully non-linear MHD wind simulations to the parameter space that describes winds from red giant stars. In the current version of this Alfvén wave driven model, a wind is driven by randomly generated low-frequency non-linear Alfvén waves in a broadband frequency range at the base of the wind. We simulate freely propagated and partially reflected Alfvén waves in the gravitationally stratified atmosphere of a late-type giant star, in a self-consistent manner, until a steady-state wind is formed. Our simulations demonstrate that, unlike linear Alfven wave-driven wind models, a stellar wind model based on plasma acceleration due to low frequency broad-band non-linear Alfvén waves, can consistently reproduce the observed radial velocity profiles of the winds, their terminal velocities, the turbulent broadening of UV lines emitted from those winds and the observed mass loss rates. We find that conversion of non-linear transverse Alfvén waves into longitudinal magnetosonic waves plays the major role in depositing momentum and energy into the stellar wind. The fitting of mass-loss rates from α Tau with the predicted rate suggests a highly anisotropic stellar wind in this evolved giant. The model also predicts a variation of the wind mass-loss rates on time scales of 1 month.

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