Mass loss in 2D Rotating Stellar Models
LESIA, Observatoire de Paris, 5 Place Jules Janssen, 92195 Meudon, France
Institute for Computational Astrophysics, Saint Mary’s University, 923 Robie St, Halifax, NS B3H 3C3, Canada
Abstract
Radiatively driven mass loss is an important factor in the evolution of massive stars. The mass-loss rates depend on a number of stellar parameters, including the effective temperature and luminosity. Massive stars are also often rapidly rotating, which affects their structure and evolution. In sufficiently rapidly rotating stars, both the effective temperature and radius vary significantly as a function of latitude, and hence mass loss rates can vary appreciably between the poles and the equator. In this work, we discuss the addition of mass loss to a 2D stellar evolution code (ROTORC) and compare evolution sequences with and without mass loss.