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Accretion turnoff and rapid evaporation of very light secondaries in low-mass X-ray binaries
Ruderman, M.; Shaham, J.; Tavani, M.
AA(Columbia University, New York), AB(Columbia University, New York), AC(Columbia University, New York)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 336, Jan. 1, 1989, p. 507-518. (ApJ Homepage)
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NASA/STI Keywords:
Neutron Stars, Stellar Magnetic Fields, Stellar Mass, Stellar Mass Accretion, X Ray Binaries, Gamma Rays, Pulsars, Pulse Duration, Stellar Evolution
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The illumination of companion stars in very low mass X-ray binaries by various kinds of radiation from the neighborhood of the neutron star after accretion has terminated or during accretion is considered. If a neutron star's spun-up period approaches 0.001 s, pulsar kHz radiation can quench accretion by pushing surrounding plasma away from the neutron star, and may leave the companion to be evaporated by the high-energy radiation component expected from an 'isolated' millisecond radiopulsar. Expected accretion-powered MeV gamma-rays and e(+ or -) winds may also be effective in evaporating dwarf companions. Neutron star spin-down energy release may sustain the power in these radiation mechanisms even while accretion falls. Accretion-powered soft X-rays may speed the mass loss of highly evolved dwarf companions, particularly those with a large fraction of carbon and oxygen.

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