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Genesis stories for the millisecond pulsarTheoretical models proposed to explain the origin of the millisecond pulsar (MP) PSR 1937+214 are reviewed, examining their ability to explain its low surface dipole magnetic field (B), its low birth temperature (less than 10 to the 8th K), the absence of a companion or remnant, and its low velocity perpendicular to the Galactic plane. The models discussed are a single isolated explosion forming a rapidly spinning neutron star, spin-up of a dead pulsar by accretion from a companion, collapse of an accreting spinning white dwarf, and fusion of a tight binary composed of two old neutron stars. Although all of the models have difficulties in explaining one or more of the MP characteristics, the second model is found to be most probable in the light of present knowledge. The lack of a companion is explained by its tidal disruption after it had fed the accreting pre-pulsar for 1 Gyr or more and its mass had decreased to about 0.01 solar mass. Neutron stars accreting in this way have been observed in Galactic-bulge X-ray sources.
Document ID
19840027469
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Ruderman, M. A.
(Columbia University New York, NY, United States)
Shaham, J.
(Columbia Univ. New York, NY, United States)
Date Acquired
August 12, 2013
Publication Date
September 1, 1983
Publication Information
Publication: Comments on Modern Physics, Part C - Comments on Astrophysics
Volume: 10
ISSN: 0146-2970
Subject Category
Astrophysics
Accession Number
84A10256
Funding Number(s)
CONTRACT_GRANT: NSF PHY-80-23721
CONTRACT_GRANT: NAS8-30753
Distribution Limits
Public
Copyright
Other

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