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The origin of planets orbiting millisecond pulsarsA model for the formation of planets around millisecond pulsar which no longer have stellar companions is suggested. Detailed hydrodynamical models are presented which suggest that planet formation can occur either in a low-mass X-ray binary progenitor to a progenitor of a star-vaporizing millisecond pulsar when the neutron star is accreting material driven off its companion by X-ray irradiation or after a pulsar has formed and is vaporizing its companion. In both cases a circumbinary disk is created in which planets can form on a timescale of 10 exp 5 to 10 exp 6 yrs and the planets can survive a second phase in which the companion star moves toward the pulsar and is completely vaporized.
Document ID
19920049872
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Tavani, Marco
(Lawrence Livermore National Laboratory, Livermore; California, University Berkeley, United States)
Brookshaw, Leigh
(Lawrence Livermore National Laboratory Livermore, CA, United States)
Date Acquired
August 15, 2013
Publication Date
March 26, 1992
Publication Information
Publication: Nature
Volume: 356
ISSN: 0028-0836
Subject Category
Astrophysics
Accession Number
92A32496
Distribution Limits
Public
Copyright
Other

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