Computer Science
Scientific paper
Aug 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.304..422s&link_type=abstract
Nature (ISSN 0028-0836), vol. 304, Aug. 4, 1983, p. 422, 423.
Computer Science
51
Binary Stars, Galactic Radiation, Pulsars, Stellar Evolution, Stellar Luminosity, X Ray Sources, Giant Stars, Milky Way Galaxy, Neutron Stars, Stellar Magnetic Fields, Stellar Mass Accretion
Scientific paper
Calculations are presented to support a model of the 6.1 msec binary pulsar system PSR1953+29 as a neutron star experiencing mass transfer from a Roche lobe-filling giant companion separated from the neutron star by a distance close to its own diameter. The giant has an envelope that is decreasing in mass by hydrogen shell burning and tidal overflow at the surface. Formulations are developed for the mass transfer rate, the temporal duration of mass transfer, and time necessary for the neutron star to spin up to its equilibrium period. The rates of mass transfer are calculated for varying masses of the giant companion, and it is found that the surface magnetic field strength of the neutron star would be about 3 billion gauss at the start of the spin-up phase, a value which was decayed greatly in the more than 1,000,000 yr since.
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