THE INITIAL-FINAL MASS RELATION : DIRECT CONSTRAINTS AT THE LOW-MASS END

@article{Kalirai2008THEIM,
  title={THE INITIAL-FINAL MASS RELATION : DIRECT CONSTRAINTS AT THE LOW-MASS END},
  author={Jason S. Kalirai and Brad M S Hansen and Daniel D Kelson and David Brian Reitzel and Robert Michael Rich and Harvey B. Richer},
  journal={The Astrophysical Journal},
  year={2008},
  volume={676},
  pages={594-609}
}
The initial-final mass relation represents a mapping between the mass of a white dwarf remnant and the mass that the hydrogen-burning main-sequence star that created it once had. The empirical relation thus far has been constrained using a sample of ~40 stars in young open clusters, ranging in initial mass from ~2.75 to 7 -->M?, and shows a general trend that connects higher mass main-sequence stars with higher mass white dwarfs. In this paper, we present CFHT CFH12K photometric and Keck LRIS… 
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We establish new constraints on the intermediate-mass range of the initial-final mass relation, and apply the results to study the evolution of stars on the thermally pulsing asymptotic giant branch
The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M ⊙
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We explore the final fates of massive intermediate-mass stars by computing detailed stellar models from the zero-age main sequence until near the end of the thermally pulsing phase. These
A Novel Approach to Constrain Rotational Mixing and Convective-core Overshoot in Stars Using the Initial–Final Mass Relation
The semi-empirical initial-final mass relation (IFMR) connects spectroscopically analyzed white dwarfs in star clusters to the initial masses of the stars that formed them. Most current stellar
The age-metallicity dependence for white dwarf stars
We present a theoretical study on the metallicity dependence of the initial to final mass relation and its influence on white dwarf age determinations. We compute a grid of evolutionary sequences
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