Computer Science
Scientific paper
Jan 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986natur.319..384j&link_type=abstract
Nature (ISSN 0028-0836), vol. 319, Jan. 30, 1986, p. 384-386.
Computer Science
16
Binary Stars, Pulsars, Stellar Evolution, Stellar Mass Accretion, Stellar Rotation, Accretion Disks, Angular Momentum, Dwarf Stars, Neutron Stars, Stellar Mass, Stellar Orbits
Scientific paper
One suggested progenitor system for the 1.5-ms pulsar PSR1937+214 is a close binary containing, in the late stages of its evolution, a neutron star and a very-low-mass (⪉0.1 M_sun;) degenerate dwarf helium star. The two main questions that affect the plausibility of this scenario are: (1) whether the system's evolution would in fact leave the neutron star at the observed high spin rate; and (2) whether the secondary could be disrupted, leaving a single pulsar. The authors have analysed such a system and find that the equilibrium rotation period predicted for the neutron star immediately before the disruption of the secondary is so large that matter accreted from a disk after disruption would be unlikely to spin the pulsar up to the observed period. It is thus unlikely that PSR1937+214 originated in a binary system in which the companion had an extremely low mass at disruption.
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