The upper mass limit for white dwarf progenitors and the initial-final mass relation for low and intermediate mass stars

Details The upper mass limit for white dwarf progenitors and the initial-final mass relation for low and intermediate mass stars The upper mass limit for white dwarf progenitors and the initial-final mass relation for low and intermediate mass stars

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...121...77w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 121, no. 1, May 1983, p. 77-84.

Astronomy and Astrophysics

Astrophysics

211

Planetary Nebulae, Stellar Evolution, Stellar Mass, White Dwarf Stars, Galactic Evolution, Mass Distribution, Milky Way Galaxy

Scientific paper

New results on white dwarfs in open clusters which establish an upper mass limit of white dwarf progenitors around 8M0 have been evaluated for the construction of a semi-empirical initial-final mass relation for stellar evolution in the low and intermediate mass range. The new Mf/Mι-relation runs flatter than hitherto assumed and explains the fact that the vast majority of white dwarfs and nuclei of planetary nebulae have masses in a narrow range around 0.6Msun. High mass remnants exist in both cases but are extremely rare. This is confirmed by model calculations of galactic evolution which are carried out with improved input data on IMF, stellar birthrates, and stellar dynamics, for different Mf/Mι-relations. Constraints are thus provided for theoretical schemes of single star evolution with mass loss, dredge-up, and enrichment of the interstellar medium.

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