Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734103o&link_type=abstract
American Astronomical Society, AAS Meeting #217, #341.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an initial-final mass relation for white dwarf stars in wide binaries that have a main sequence companion. The effective temperatures and gravities of each white dwarf component are measured by fitting theoretical model spectra to observed spectra. From these, cooling times and masses are obtained using theoretical cooling tracks. The total age of each binary is estimated from the chromospheric activity of its main sequence component. The difference between the total age of the binary and its white dwarf cooling time is approximately the main sequence lifetime of the white dwarf. From this the initial mass of the WD can be computed from standard main sequence evolution models. Since our wide binaries are much older than nearby clusters, the initial masses of our white dwarfs tend to sample the low mass end of the initial-final mass relation, a regime where clusters provide sparse information. Our results also suggest the metallicity of a star does not affect the amount of post main sequence mass loss that occurs, at least for low mass progenitors.
Holberg Jay
Oswalt Terry D.
Zhao Jun
No associations
LandOfFree
Testing the Initial-Final Mass Relation of White Dwarf Stars using Wide Binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Testing the Initial-Final Mass Relation of White Dwarf Stars using Wide Binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Testing the Initial-Final Mass Relation of White Dwarf Stars using Wide Binaries will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1402841