Evolution of massive stars with mass loss and formation of WR stars

Details Evolution of massive stars with mass loss and formation of WR stars Evolution of massive stars with mass loss and formation of WR stars

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...101..215n&link_type=abstract

Astronomy and Astrophysics, vol. 101, no. 2, Aug. 1981, p. 215-222.

Astronomy and Astrophysics

Astrophysics

34

Stellar Evolution, Stellar Mass Ejection, Stellar Winds, Wolf-Rayet Stars, Abundance, Helium, Hertzsprung-Russell Diagram, Mass Flow Rate, Nuclear Fusion, Stellar Oscillations

Scientific paper

The plausibility of a scheme of the forming of massive WR stars is investigated by computing the evolution of stars (with initial masses of 60, 80, and 100 solar masses), taking into account mass loss to the end of core He-burning. At the beginning of core He-burning, mass loss through stellar wind is considered, with rates typical of O and Of stars. When the star becomes a transition WN, mass loss rates are increased to values observed in WR stars. During core He-burning, the two most massive stars go through a phase of vibrational instability, which induces a higher mass loss rate. All the ways of WR star forming are added to obtain a total WR/O ratio, which can be compared with observations. The corresponding average mass for WR stars is also computed. Although it is possible to find a theoretical WR/O ratio which is compatible with the observations, it is difficult to explain both the observed WR/O ratio and the average mass of WR found by Massey (1981) in the frame of the present theories of star formation.

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