An Improved Mass-loss Description for Dust-driven Superwinds

Details An Improved Mass-loss Description for Dust-driven Superwinds An Improved Mass-loss Description for Dust-driven Superwinds

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12.1030w&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

Scientific paper

We consider the mass loss of stars during the final stages of their evolution. Our mass loss description for the tip-AGB is based on pulsating wind models in which the mass loss is driven by radiation pressure on dust grains, for a C-rich chemistry. From a grid of these models an improved approximative mass-loss rate formula has been derived which depends on the stellar parameters: effective temperature, luminosity, and mass only. The dependence of the mass-loss rate on the pulsation period has been taken into account by applying the observed period-luminosity relation for C-rich Miras. Since the wind models treat in detail the chemistry and micro-physics of the dust formation process, the resulting mass-loss rate depends strongly on the stellar effective temperature, reflecting the sensitivity of the dust formation process on the local thermodynamic conditions.

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