Computer Science
Scientific paper
May 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.303..213h&link_type=abstract
Nature (ISSN 0028-0836), vol. 303, May 19, 1983, p. 213-216.
Computer Science
23
Binary Stars, Neutron Stars, Pulsars, Stellar Evolution, Angular Velocity, Roche Limit, Stellar Mass Accretion, Stellar Models
Scientific paper
The combination of short pulse period and abnormally weak surface dipole magnetic-field strength, in contrast to the canonical pulsar value of the 1.5-ms pulsar PSR 1937+214 has led to the suggestion that it is an old neutron star that was spun up by accretion in a binary system. The authors point out difficulties with such a model: massive binaries are unlikely to live sufficiently long to allow the required amount of spin-up matter to be accreted; in low-mass binaries the companion star is still expected to be present. The authors argue that a likely alternative is: formation by coalescence of two neutron stars that formed a close binary such as PSR 1913+16. These (inevitable) events may occur in the galaxy at a rate ≡10-4 yr-1, and provide a natural explanation of the millisecond rotation period.
Henrichs Hubertus F.
van den Heuvel Edward Peter Jacobus
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