Statistics – Computation
Scientific paper
Jun 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...147..300m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 147, no. 2, June 1985, p. 300-308.
Statistics
Computation
93
Stellar Mass Ejection, Stellar Oscillations, Wolf-Rayet Stars, Computational Astrophysics, Main Sequence Stars, Stellar Evolution, Stellar Models
Scientific paper
The radial vibrational instability VI of O stars; Hubble-Sandage variables (HSVs); and WR stars of classes WNL, WNE, WC, and WO is investigated theoretically by means of numerical simulations for stellar masses 85 and 120 solar mass. The results are presented in tables and graphs and discussed. It is found that as stars evolve from the HSV stage (with no VI) into the WR-star sequence, they become unstable as surface H/He becomes equal to 0.3 and the ratio of core energizing to envelope damping becomes 10,000 times greater than that on the main sequence, with pulsation periods 15-60 min and possibly with VI enhancement due to overshooting or turbulent diffusion. It is determined that a mass-loss rate of 0.00002-0.0001 solar mass/yr could be sustained by pulsations in the limiting case of a WR star evolving quasi-homogeneously at the edge of VI.
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