On the Maximum Mass of C-O White Dwarfs

Details On the Maximum Mass of C-O White Dwarfs On the Maximum Mass of C-O White Dwarfs

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aipc..637...57d&link_type=abstract

CLASSICAL NOVA EXPLOSIONS: International Conference on Classical Nova Explosions. AIP Conference Proceedings, Volume 637, pp. 5

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Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Masses, Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Supernovae, Giant And Subgiant Stars, Accretion And Accretion Disks

Scientific paper

The formation of massive C-O white dwarfs in the range 1.1 to 1.4 Msolar opens interesting channels for novae, supernovae and accretion induced collapse events. We will review the present situation concerning the maximum mass attained by the C-O core inside an AGB star, both following standard and non-standard evolution, and taking into account the observational constraints. We find that to form C-O cores with masses greater than 1.1 Msolar, the 2nd dredge-up should be delayed and that the only obvious mechanism for that is rotation.

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