Evolution of massive stars with low metal abundance holding for the Magellanic Clouds

Details Evolution of massive stars with low metal abundance holding for the Magellanic Clouds Evolution of massive stars with low metal abundance holding for the Magellanic Clouds

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....95...14h&link_type=abstract

Astronomy and Astrophysics, vol. 95, no. 1, Feb. 1981, p. 14-17.

Astronomy and Astrophysics

Astrophysics

22

Abundance, Magellanic Clouds, Stellar Evolution, Stellar Mass, Binary Stars, Galactic Evolution, Milky Way Galaxy, Stellar Luminosity, Stellar Winds

Scientific paper

Evolutionary computations are performed for stars with masses between 20 and 100 solar masses having chemical abundances holding for the Small Magellanic Cloud (i.e., Y = 0.237, Z = 0.003). During core hydrogen burning, mass loss by stellar wind is induced. Comparison with galactic evolutionary models is presented. Massive close binary evolution with SMC abundances is followed and discussed up to core helium exhaustion. It can be stated that with regard to the luminosity, the effective temperature, the core mass, the hydrogen main sequence lifetime, the remnant structure after Roche lobe overflow in massive close binaries and the helium burning phase, the results for the SMC are very similar (i.e., within 10%) to the results obtained with galactic properties. The reason why the ratio (number of early WN)/(number of WC) is different in the Galaxy and the MC's can therefore not be an evolutionary effect caused by a lower metallicity in the Clouds. A difference in mass loss rate is the most probable reason for the ratio difference.

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