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- W3100651483 abstract "Context. Among the spectroscopically identified white dwarfs, a fraction smaller than 2% have spectra dominated by carbon lines, mainly molecular C 2 , but also a smaller group dominated by C I and C II lines. These are together called DQ white dwarfs. Aims. We want to derive atmospheric parameters T eff , log g , and carbon abundances for a large sample of these stars and discuss implications for their spectral evolution. Methods. Sloan Digital Sky Survey spectra and ugriz photometry were used, together with Gaia Data Release 2 parallaxes and G band photometry. These were fitted to synthetic spectra and theoretical photometry derived from model atmospheres. Results. We found that the DQ hotter than T eff ~ 10 000 K have masses ~ 0.4 M ⊙ larger than the classical DQ, which have masses typical for the majority of white dwarfs (~ 0.6 M ⊙ ). We found some evidence that the peculiar DQ below 10 000 K also have significantly larger masses and may thus be the descendants of the hot and warm DQ above 10 000 K. A significant fraction of the hotter objects with T eff > 14 500 K have atmospheres dominated by carbon." @default.
- W3100651483 created "2020-11-23" @default.
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- W3100651483 date "2019-08-01" @default.
- W3100651483 modified "2023-09-25" @default.
- W3100651483 title "Carbon-rich (DQ) white dwarfs in the Sloan Digital Sky Survey" @default.
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- W3100651483 doi "https://doi.org/10.1051/0004-6361/201935946" @default.
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