The shape of the initial-final mass relation for low and intermediate mass stars

Details The shape of the initial-final mass relation for low and intermediate mass stars The shape of the initial-final mass relation for low and intermediate mass stars

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...134l...1w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 134, no. 1, May 1984, p. L1-L3.

Astronomy and Astrophysics

Astrophysics

44

Magellanic Clouds, Star Clusters, Stellar Mass, White Dwarf Stars, Asymptotic Giant Branch Stars, Giant Stars, Stellar Evolution, Stellar Luminosity, Stellar Mass Ejection

Scientific paper

It is demonstrated how the absence of bright giants on the asymptotic giant branch of Magellanic Cloud clusters, especially in the case of NGC 1866, restricts the initial-final mass relation for evolution of low and intermediate mass stars, and confirms its upward bending shape which was derived from white dwarf data. Mass loss must be so strong that in many cases the thermal pulsing phase on the AGB is not reached. Differential mass loss operates in such a way that the single valued initial-final mass relation has to be replaced by a band of finite width.

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