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Mass loss in 2D rotating stellar models

  • Catherine Lovekin (a1) and Robert G. Deupree (a2)

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 surface flux 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.

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Copyright

References

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Castor, J. I., Abbott, D. C., & Klein, R. I. 1975, ApJ, 195, 157
Deupree, R. G. 1990, ApJ, 357, 175
Deupree, R. G. 1995, ApJ, 439, 357
Vink, J. S., de Koter, A., & Lamers, H. J. G. L. M. 2001, A&A, 369, 574
von Zeipel, H. 1924, MNRAS, 84, 665
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Keywords

Mass loss in 2D rotating stellar models

  • Catherine Lovekin (a1) and Robert G. Deupree (a2)

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