Stellar evolution after IUE. Part 1: Massive stars during core hydrogen burning and massive close binaries

Details Stellar evolution after IUE. Part 1: Massive stars during core hydrogen burning and massive close binaries Stellar evolution after IUE. Part 1: Massive stars during core hydrogen burning and massive close binaries

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.176...15d&link_type=abstract

In ESA 3rd European IUE Conf. p 15-20 (SEE N83-11889 02-88)

Statistics

Computation

Binary Stars, Hydrogen, Iue, Stellar Evolution, Stellar Mass Ejection, Wolf-Rayet Stars, Accretion Disks, Mass Flow Rate, Mass Transfer, Stellar Coronas, Stellar Interiors, Stellar Luminosity, Stellar Mass Accretion, Stellar Spectra, Stellar Structure, Stellar Winds, X Ray Binaries

Scientific paper

The effect of mass loss rates on stellar evolution is discussed. Position of mass outflow tracks, overluminosity, and the formation of Wolf-Rayet stars are considered. Computations which take the effects of stellar wind, mass transfer and mass loss during Roche lobe overflow, and accretion into account are described. Computation and IUE studies of stellar chemical composition generally agree, except for WC stars where N lines are found in spite of theoretical expectations that during helium burning all nitrogen is depleted. Accretion computations for massive close binaries show that the chemical profile of the accreting component has the same behavior as that of a normal main sequence star of the same mass, in the stellar interior. In the outer layers the hydrogen content is smaller. The observed overluminosity of the optical companions of X-ray binaries can be explained by stellar wind mass losses.

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