Orbital period variability in the eclipsing pulsar binary PSR B1957+20: Evidence for a tidally powered star

Details Orbital period variability in the eclipsing pulsar binary PSR B1957+20: Evidence for a tidally powered star Orbital period variability in the eclipsing pulsar binary PSR B1957+20: Evidence for a tidally powered star

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..312a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-367X), vol. 436, no. 1, p. 312-318

Other

40

Angular Momentum, Eclipsing Binary Stars, Kepler Laws, Pulsars, Stellar Magnetic Fields, Hubble Space Telescope, Mathematical Models

Scientific paper

Recent observations indicate that the eclipsing pulsar binary PSR B1957+20 undergoes alternating epochs of orbital period increase and decrease. We apply a model developed to explain orbital period changes of alternating sign in other binaries to the PSR B1957+20 system and find that it fits the pulsars observations well. The novel feature of the PSR B1957+20 system is that the energy flow in the companion needed to power the orbital period change mechanism can be supplied by tidal dissipation, making the companion the first identified tidally powered star. The flow of energy in the companion drives magnetic activity, which underlies the observed orbital period variations. The magnetic activity and the wind driven by the pulsar irradiation results in a torque on the spin of the companion. This torque holds the companion out of synchronous rotation, causing tidal dissipation of energy. We propose that the progenitor had a approximately 2 hr orbital period and a companion mass of 0.1-0.2 solar mass, and the system is evolving to longer orbital periods by mass and angular momentum loss on a timescale of 108 yr.

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