Why we see relativistic binary pulsars.

Details Why we see relativistic binary pulsars. Why we see relativistic binary pulsars.

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phr...256..109b&link_type=abstract

Physics Reports, Vol. 256, No. 1 - 3, p. 109 - 116

Physics

2

Binary Pulsars: Neutron Stars, Neutron Stars: Accretion, Neutron Stars: Binaries

Scientific paper

The hypercritical accretion described by Chevalier (1995) forces a re-examination of the evolution of binary pulsars. We favor helium star binaries as progenitors, so that the first neutron star does not have to go through a hydrogen envelope. In this way it avoids going into a black hole. We argue here that, if the neutron-star helium-star binary following the first explosion is narrow, with relative axis a ≡ 1 Rsun, then accretion from the helium star can bring the magnetic field of the neutron star down from B ≥ 1012G to B ≡ 1010G. The neutron-star neutron-star binary resulting from such a narrow progenitor is likely to also be relatively narrow, although there is a tendency in the explosions of the remaining helium star for the orbit to open up by a factor of ≡(1-e)-1, where e is the eccentricity of the relativistic neutron-star binary. Something like PSR 1913+16 or PSR 1534+12 results. Because the magnetic fields of the pulsars have been so reduced by accretion, their spin-down times are greatly increased, and, therefore, also the probability of seeing them.

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