Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...285..252c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 285, Oct. 1, 1984, p. 252-257. Research supported by Louisiana State Univer
Astronomy and Astrophysics
Astrophysics
73
Cataclysmic Variables, Magnetic Stars, Stellar Evolution, White Dwarf Stars, Astronomical Catalogs, Main Sequence Stars, Orbital Elements, Stellar Models, Stellar Rotation
Scientific paper
A close binary containing a magnetic white dwarf and a lower main-sequence secondary evolves through several stages following the onset of mass transfer. Whether the initial rotation period is greater or less than P(eq), the equilibrium period for disk accretion, the rotation period approaches P(eq) on a time scale of not greater than about 100-million yr, and the system becomes a DQ Her binary. Further evolution is due to angular momentum losses caused by gravitational radiation and magnetic braking of the secondary. As the orbital separation and luminosity decrease, the magnetosphere of the white dwarf encounters the secondary, if B is greater than about 3,000,000 gauss, and synchronizes the rotation of the white dwarf as in the AM Her binaries. The present model is consistent with the observation that most DQ Her binaries have P(orb) greater than 3 hr, while most AM Her binaries have P(orb) less than 2 hr.
Chanmugam G.
Ray Asok
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