Physics
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt.........8b&link_type=abstract
Ph.D. Thesis Columbia Univ., New York, NY.
Physics
Planetary Evolution, Pulsars, Radiant Heating, Stellar Evolution, Stellar Winds, X Ray Binaries, Angular Momentum, Mass Flow Rate, Stellar Mass
Scientific paper
We show that the formation of planets around a millisecond pulsar may occur in a very late phase of Low-Mass X-Ray Binary (LMXB) or Binary-Millisecond-Pulsar (BMP) evolution. We propose a new mechanism in which the companion winds in these phases form through the combined action of the radiation heat on the companion's atmosphere and the radiation force on the slowly lifting wind. This mechanism can produce relatively high mass flow rates, and provided the companion is bloated, it explains the observed rapid angular momentum loss of the binary millisecond pulsar 1957 + 20. With such wind the evaporated matter can be supplied to a circumbinary 'excretion' disk in which the physical conditions, similar to those appropriate for the BMP1957 + 20 system, may allow the formation of planets like those observed in PSR1257 + 12. This model connects the conventional evolutionary scenario for the formation of a millisecond pulsar with the formation of planets around it.
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