2008/06/30 by S. Vennes, A. Kawka · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13652.x
Accepted for publication in MNRAS (with an updated discussion on GD362)
arxiv created 2008/07/03 · openalex publication_date 2008/08/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We re-examine the evidence for the existence of ultramassive (M > 1.1 M⊙) white dwarfs based on gravitational redshift of white dwarfs in common proper motion binaries or in clusters, on parallax measurements, on orbital solutions and, finally, on the analysis of hydrogen-line profiles. We conclude that the best evidence is largely based on the analysis of Balmer-line profiles although the companion to the A8V star HR 8210 is a compelling case made initially using the large binary mass function and confirmed by an analysis of the Lyman-line spectrum. The confirmation and identification of high-mass white dwarfs, more particularly non-hydrogen-rich (non-DA) white dwarfs, using parallax measurements may prove critical in establishing the population fraction of these objects and in constraining the high end of empirical initial-mass to final-mass relations. The existence of a substantial population of ultramassive white dwarfs supports the concept of a steeper initial-mass to final-mass relations linking 6 M⊙ progenitors with ≳1.1 M⊙ white dwarfs.