Fate of the companion stars of ultra-rapid pulsars

Details Fate of the companion stars of ultra-rapid pulsars Fate of the companion stars of ultra-rapid pulsars

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988natur.334..227v&link_type=abstract

Nature (ISSN 0028-0836), vol. 334, July 21, 1988, p. 227, 228.

Statistics

87

Companion Stars, Eclipsing Binary Stars, Pulsars, X Ray Binaries, Cataclysmic Variables, Neutron Stars, Periodic Variations, Radio Stars, Stellar Luminosity

Scientific paper

A millisecond pulsar that is formed by spin-up "recycling" in a binary system will, once the mass transfer becomes temporarily interrupted, start to evaporate its companion star as a consequence of the large impinging pulsar energy flux. This evaporation is easiest if the pulsar has a short pulse period, the companion star has a relatively large radius and is therefore hydrogen-rich, and the orbital period is short. Evaporation of companion stars induced by millisecond pulsars could account for the lack of low-mass X-ray binaries with short orbital periods below the period gap of the cataclysmic variables, and for the statistics of new-born radio pulsars and their space velocities.

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