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by Staff Writers Paris, France (ESA) Sep 09, 2009
XMM-Newton observations of the X-ray pulsator RX J0648.0-4418, timed to also cover the phase when the source was expected to be eclipsed by its companion, have resulted in a solid, model-independent mass estimation of this object. It appears to be a rare, ultra-massive white dwarf, whose continued study promises to provide sensitive tests for stellar evolution theories. Sandro Mereghetti and colleagues present these results in the 4 September issue of Science. The X-ray pulsator RX J0648.0-4418 and the subdwarf star HD49798 form a binary system with unique properties. The subdwarf star is a bright object in the optical and UV bands, and is well characterized. The orbital period of the system is accurately known, and the discovery in 1996 of a 13.2 s periodicity in X-rays made it clear that the companion must be either a neutron star or a white dwarf.
Binary systems are key test cases for stellar evolution models Often though, only information about one of the objects in the system (usually the brighter one) is known. This can be used to derive the mass function of the system, a combination of the two masses and the inclination of the orbital plane with respect to the line of sight. When similar information about the other object can be obtained, either spectroscopically or by measuring the time delays in the pulsations induced by the orbital motion, then the two masses can be calculated - if a good estimation of the inclination can be obtained. The latter can be constrained quite accurately if one of the objects is periodically eclipsed by the other.
A model-independent mass estimate points to a rare, massive white dwarf Armed with these data, and applying them to the equation of orbital motion, they were able to conclude that the X-ray source is a rare, ultra-massive (at least 1.2 solar masses) white dwarf. This makes RX J0648.0-4418 one of the most massive white dwarfs known to date.
Important implications for studies of stellar evolution The demonstration that this unique binary system consists of a fast-spinning, ultra-massive white dwarf in a nearby binary system (it is at a distance of 650 parsecs) which therefore can be studied in detail, provides astrophysicists with another important test bench to use in developing models of stellar evolution.
Related Links XMM-Newton Stellar Chemistry, The Universe And All Within It
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