Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21820503c&link_type=abstract
American Astronomical Society, AAS Meeting #218, #205.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
All stars are believed to possess expanding outer atmospheres known as stellar winds. The continual evaporation of gas from stars has a significant impact on stellar and planetary evolution, and also on the larger-scale evolution of gas and dust in galaxies. Despite more than a half-century of study, though, the basic mechanisms responsible for producing stellar winds are still largely unknown. Fortunately, there has been a great deal of recent progress toward identifying and characterizing the processes that produce our own Sun's mass outflow. Based on this progress, we have developed a new generation of physically motivated models of stellar wind acceleration for cool main-sequence stars and evolved giants. These models follow the production of magnetohydrodynamic turbulent motions from subsurface convection zones to their eventual dissipation and escape through the stellar wind. The magnetic activity of these stars is taken into account by extending standard age/rotation/activity indicators to include the evolution of the filling factor of strong magnetic fields in stellar photospheres. We will present tests of these models based on a large database of observationally determined mass loss rates, in combination with accurate measurements of the basic properties of these stars (e.g., masses, radii, luminosities, metallicities, and rotation rates) on which the mass loss rates must depend. The eventual goal of this project is to provide a simple stand-alone algorithm for predicting the mass loss rates of cool stars for use in stellar atmosphere and population synthesis calculations.
Cranmer Steven R.
Saar Steven H.
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