A refractive model for eclipsing binary radio pulsars

Details A refractive model for eclipsing binary radio pulsars A refractive model for eclipsing binary radio pulsars

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..589e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 10, 1990, p. 589-596.

Physics

17

Eclipsing Binary Stars, Pulsars, Radio Stars, Stellar Models, Companion Stars, Cosmic Plasma, Density Distribution, Stellar Atmospheres, Stellar Winds

Scientific paper

A model for binary radio pulsars is presented in which refraction by a plasma in an extended stellar atmosphere or wind causes radio eclipses. Based on PSR applying this model to PSR 1957 + 20, it is found that refractive eclipses can be created with wind densities of order 10 to the 7th/cu cm near the apparent eclipse radius of 0.7 solar. This density is easily obtained in an X-ray excited wind. A power-law density falloff can match the observed frequency dependence of the eclipse. The physics of a wind resulting from high-energy irradiation of the pulsar's companion is described. It is estimated that the mass flux in such a wind is sufficient to achieve the densities needed for refractive eclipses.

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