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Daytona Beach


Physical Sciences

Document Type


Publication/Presentation Date



We present the initial–final mass relation derived from 10 white dwarfs in wide binaries that consist of a main-sequence star and a white dwarf. The temperature and gravity of each white dwarf were measured by fitting theoretical model atmospheres to the observed spectrum using a χ2 fitting algorithm. The cooling time and mass were obtained using theoretical cooling tracks. The total age of each binary was estimated from the chromospheric activity of its main-sequence component to an uncertainty of about 0.17 dex in log t. The difference between the total age and white dwarf cooling time is taken as the main-sequence lifetime of each white dwarf. The initial mass of each white dwarf was then determined using stellar evolution tracks with a corresponding metallicity derived from spectra of their main-sequence companions, thus yielding the initial–final mass relation. Most of the initial masses of the white dwarf components are between 1 and 2M. Our results suggest a correlation between the metallicity of a white dwarf’s progenitor and the amount of post-main-sequence mass loss it experiences—at least among progenitors with masses in the range of 1–2M. A comparison of our observations to theoretical models suggests that low-mass stars preferentially lose mass on the red giant branch.

Publication Title

The Astrophysical Journal



IOP Publishing

Grant or Award Name

NSF grant AST-0807919, NSFC grant nos. 11078019 and 10821061, NSF grant AST-0708143

Additional Information

Dr. Oswalt was not affiliated with Embry-Riddle Aeronautical University at the time this paper was published.