Formation of a 'planet' by rapid evaporation of a pulsar's companion

Details Formation of a 'planet' by rapid evaporation of a pulsar's companion Formation of a 'planet' by rapid evaporation of a pulsar's companion

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256l..35r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 2, p. L35-L37.

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Binary Stars, Circular Orbits, Evaporation, Extrasolar Planets, Pulsars, Stellar Evolution, Computational Astrophysics, Planetary Evolution, Stellar Models

Scientific paper

A model based on the binary configuration of the PSR1829-10 pulsar (Bailes et al., 1991) is used to show that the formation of a binary pulsar with a planet-size companion, large original separation, and small eccentricity could result from the rapid evaporation of a much more massive binary companion by the pulsar's radiation. Such an evaporation process is known to be taking place in at least two other binary pulsars: PSR1957 + 20 (Fruchter et al., 1990; Ryba and Taylor, 1991) and PSR1744 - 24A (Lyne et al., 1990). It is shown here that, about one million years ago, the companion mass and binary separation could have been comparable to those currently observed in the eclipsing binary pulsar PSR1957 + 20.

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