Stellar models and the brightening of P Cygni

Details Stellar models and the brightening of P Cygni Stellar models and the brightening of P Cygni

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...404..271e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 404, no. 1, p. 271-275.

Astronomy and Astrophysics

Astrophysics

15

Brightness Distribution, Massive Stars, Stellar Evolution, Stellar Luminosity, Stellar Models, Hertzsprung-Russell Diagram, Stellar Envelopes, Stellar Winds

Scientific paper

P Cygni is currently in the transition phase between core hydrogen and helium burning. The behavior of the stellar envelope in this phase is strongly affected by the intermittant dominance of hydrogen shell burning. We perform detailed stellar evolution calculations of this rapid transition phase using the most recent Livermore opacities. We find that observations and stellar evolution models agree very well if the initial main-sequence mass of P Cygni was about 60 +/- 5 solar masses. Depending on the mass-loss rate, P Cygni's current mass could be as low as 50 solar masses, which is still about a factor of 2 higher than that predicted by the radiation driven wind theory. Our calculations seem to favor the Schwarzschild criterion for convection over the Ledoux criterion in conjunction with semiconvection.

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