Evolution of a 30 solar masses star with mass loss. I - Core H burning phase

Details Evolution of a 30 solar masses star with mass loss. I - Core H burning phase Evolution of a 30 solar masses star with mass loss. I - Core H burning phase

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.196..225f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 196, July 1981, p. 225-255. Research supported by the Natural Sciences

Other

11

Hydrogen, Nuclear Fusion, Stellar Evolution, Stellar Mass Ejection, Stellar Structure, Chemical Composition, Linear Equations, Stellar Luminosity, Stellar Models, Stellar Temperature

Scientific paper

Observational evidence in the last decade has shown that mass loss (ML) is a general characteristic of massive stars. Investigations demonstrate that during the main sequence (MS) phase of evolution, stars undergoing ML are 'overluminous' for their mass. The main aim of the considered study is to provide more basic understanding of stellar evolution with ML. For this purpose five evolutionary tracks with different ML rates (MLR) were produced. While the absolute values of the evolutionary parameters will depend on the input physics, numerical techniques and the ML algorithm employed, the relative effects of different MLR should be more independent of the stellar evolution program. In agreement with other authors who used similar as well as different ML algorithms, it is found that the luminosity of stars evolving with ML is lowered as the MLR is increased. The decrease in luminosity is found to be entirely explained by the mass-luminosity law which includes the effects of composition and radiation pressure.

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