Models for the formation of binary and millisecond radio pulsars

Details Models for the formation of binary and millisecond radio pulsars Models for the formation of binary and millisecond radio pulsars

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984japa....5..209v&link_type=abstract

Journal of Astrophysics and Astronomy (ISSN 0250-6335), vol. 5, Sept. 1984, p. 209-233.

Astronomy and Astrophysics

Astrophysics

81

Binary Stars, Pulsars, Radio Stars, Stellar Evolution, Gravitational Collapse, Neutron Stars, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Models, White Dwarf Stars

Scientific paper

The peculiar combination of a relatively short pulse period and a relatively weak surface dipole magnetic field strength of binary radio pulsars finds a consistent explanation in terms of (1) decay of the surface dipole component of neutron-star magnetic fields on a timescale of (2 - 5)×106yr, in combination with (2) spin-up of the rotation of the neutron star during a subsequent mass-transfer phase. The four known binary radio pulsars appear to fall into two different categories. Two of them, PSR 0655+64 and PSR 1913+16, have short orbital periods (<25 h) and high mass functions, indicating companion masses ≥0.7 M_sun;. The other two, PSR 0820+02 and PSR 1953+29, have long orbital periods (≥117 d), nearly circular orbits, and low mass functions, suggesting companion masses of about 0.3 M_sun;. Among the binary models proposed for the formation of the 1.5-millisecond pulsar, the only ones that appear to be viable are those in which the companion disappeared by coalescence with the neutron star.

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