Physics
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aspc...36..275f&link_type=abstract
In: Planets around pulsars; Proceedings of the Conference, California Inst. of Technology, Pasadena, Apr. 30-May 1, 1992 (A93-36
Physics
Accretion Disks, Binary Stars, Pulsars, Stellar Mass Ejection, Stellar Winds, Planetary Systems, Stellar Physics
Scientific paper
Although the PSR 1957+20 binary system displays a large orbital period derivative, radio observations of the ablated wind from the companion reveal a low free electron density. If the orbital period derivative provides a true indication of the mass loss rate, then the ablated material must be overwhelmingly neutral or largely confined to a narrow region about the orbital plane. However, the companion's high orbital velocity, the observed turbulence in the eclipsing wind, and the energy density of the pulsar's spin-down radiation conspire to make a neutral evaporate unlikely. Radio, optical and infrared observations are shown to suggest that the companion to PSR 1957+20 is bloated, perhaps approaching the size of its Roche lobe. The wind off the companion is most probably a low velocity flow which does not travel far from the orbital plane.
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