Volume 388, Number 2, June III 2002
|Page(s)||546 - 551|
|Section||Interstellar and circumstellar matter|
|Published online||31 May 2002|
On the formation of neon-enriched donor stars in ultracompact X-ray binaries
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 119017 Moscow, Russia
2 Astronomical Institute “Anton Pannekoek”, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
3 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA, Cambridge, UK
Corresponding author: L. Yungelson, firstname.lastname@example.org
Accepted: 3 April 2002
We study the formation of neon-enriched donor stars in ultracompact X-ray binaries min) and show that their progenitors have to be low-mass (0.3–0.4) “hybrid” white dwarfs (with CO cores and thick helium mantles). Stable mass transfer is possible if in the initial stages of mass exchange mass is lost from the system, taking away the specific orbital angular momentum of the accretor (“isotropic re-emission”). The excess of neon in the transferred matter is due to chemical fractionation of the white dwarf which has to occur prior to the Roche lobe overflow by the donor. The estimated lower limit of the orbital periods of the systems with neon-enriched donors is close to 10 min. We show that the X-ray pulsar 4U 1626-67, which likely also has a neon-enriched companion, may have been formed via accretion induced collapse of an oxygen-neon white dwarf accretor if the donor was a hybrid white dwarf.
Key words: stars: white dwarfs / stars: mass loss / stars: abundances / binaries: close / X-rays: binaries
© ESO, 2002
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