An Ultra-Massive Fast-Spinning White Dwarf in a Peculiar Post Common Envelope Binary System

Details An Ultra-Massive Fast-Spinning White Dwarf in a Peculiar Post Common Envelope Binary System An Ultra-Massive Fast-Spinning White Dwarf in a Peculiar Post Common Envelope Binary System

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1314..256m&link_type=abstract

INTERNATIONAL CONFERENCE ON BINARIES: In celebration of Ron Webbink's 65th Birthday. AIP Conference Proceedings, Volume 1314, p

Computer Science

White Dwarfs, Eclipsing Binary Stars, Pulsars, Neutron Stars, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Eclipsing Binaries, Pulsars, Neutron Stars

Scientific paper

HD49798/RX J0648.0-4418 is the only known X-ray binary composed by a hot sub-dwarf and an X-ray pulsar. An XMM-Newton observation performed in May 2008 has shown that the 13 seconds pulsations are due to a rapidly rotating white dwarf. From the pulse time delays induced by the 1.55 days orbital motion, and the system's inclination, constrained by the duration of the X-ray eclipse discovered in this observation, it has been possible to accurately measure the masses of the two stars of this post common envelope binary. With a mass of 1.28+/-0.05Msolar, RX J0648.0-4418 is one of the most massive white dwarf and the one with the shortest spin period. The future evolution of this binary system will involve a new phase of mass accretion through Roche-lobe overflow that could drive the already massive white dwarf above the Chandrasekhar limit and produce a Type Ia supernova or a millisecond pulsar.

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