Red supergiant variables in the Large Magellanic Cloud: Their evolution and puslations

Details Red supergiant variables in the Large Magellanic Cloud: Their evolution and puslations Red supergiant variables in the Large Magellanic Cloud: Their evolution and puslations

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...289..449l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 289, no. 2, p. 449-457

Astronomy and Astrophysics

Astrophysics

13

Magellanic Clouds, Red Giant Stars, Stellar Evolution, Stellar Oscillations, Variable Stars, Opacity, Stellar Cores, Stellar Luminosity, Stellar Mass, Stellar Models, Stellar Winds

Scientific paper

Evolution and pulsations of red supergiants in the Large Magellanic Cloud (LMC) are investigated using realistic evolutionary models of 15 solar mass, 20 solar mass, and 30 solar mass, including the up-to-date opacity, the mass loss through the stellar wind and the overshooting from the convective core. It is found that the mass loss has notable effect on the evolution of stars above 20 solar mass, and that the evolution of all models during the core helium-burning stage is significantly influenced by the overshooting. The fundamental mode is found to be the pulsation mode of the observed variable stars, while the assumption of the first overtone turns out to be inconsistent with observations. The instability strip is cut off by the mass loss at the high luminosity and by the extremely small time scale during the crossing through the instability strip at the low luminosity. The ratio of the mixing length to the local pressure scale height has to increase along the RGB to fit the observations.

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