On the initial-final mass relation and maximum mass of white dwarf progenitors

Details On the initial-final mass relation and maximum mass of white dwarf progenitors On the initial-final mass relation and maximum mass of white dwarf progenitors

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.288..585j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 288, Issue 3, pp. 585-588.

Astronomy and Astrophysics

Astronomy

35

Stars: Evolution, White Dwarfs

Scientific paper

The four white dwarfs (WDs) discovered in the young open cluster NGC 2516 are crucial in defining the shape of the initial-final mass relation (IFMR) and upper mass limit for WD progenitors (M_wd). The cluster metallicity has been recently determined as [M/H]=-0.32+/-0.06, which is found to decrease the previously derived WD progenitor masses by 1.0-1.7Msolar. The new progenitor masses are consistent with M_wd of only 5-6Msolar, which is confirmed by integrating an extrapolated cluster mass function. The results disagree with the 8-Msolar upper limit contained in the frequently used semi-empirical IFMR of Weidemann, but are now in agreement with evolutionary models with moderate core overshoot. It is suggested that beyond an initial mass of 3Msolar, the IFMR may follow the relationship between initial mass and the core mass at the start of the thermally pulsating asymptotic giant branch, implying very efficient mass loss. According to these evolutionary models, non-degenerate carbon burning is possible in the cores of stars with initial mass <6Msolar, so a similar M_wd means there should be few carbon deflagration supernovae. However, decreasing M_wd from 8 to 5-6Msolar would significantly increase the expected numbers of core-collapse supernovae.

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