The magnetic field strength versus orbital period relation for binary radio pulsars with low-mass companions: evidence for neutron-star formation by accretion-induced collapse?

Details The magnetic field strength versus orbital period relation for binary radio pulsars with low-mass companions: evidence for neutron-star formation by accretion-induced collapse? The magnetic field strength versus orbital period relation for binary radio pulsars with low-mass companions: evidence for neutron-star formation by accretion-induced collapse?

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297l..41v&link_type=abstract

Astronomy and Astrophysics, v.297, p.L41

Astronomy and Astrophysics

Astrophysics

84

Neutron Stars, Binary Pulsars, Pulsars, Accretion-Induced Collapse

Scientific paper

The 24 binary radio pulsars with nearly circular orbits and low-mass companions (0.2-0.4xMsun_ helium white dwarfs in most cases) show a remarkable correlation between spin period P and orbital period P_or_ and between dipole surface magnetic field strength B_S_, and P_or_. The observed B_S_, vs. P_or_ relation is consistent with increasing decay of the neutron-star magnetic field with increasing amounts of matter accreted, as has been proposed on theoretical grounds by various authors. Neutron stars in binaries to which more than 0.45xfxMsun_ was transferred have field strengths below 10^9^G, where f(=<1) is the fraction of the transferred matter that is not lost from the systems. The only one exception in the galactic disk (out of twelve systems) is the PSR 1831-00 system, in which >0.7xfxMsun_ was transferred but the pulsar still has a strong magnetic field (~0.8x10^11^G). Adopting the field decay by accretion models, the only way in which this can be explained is that the neutron star in this system was formed near the end of the mass-transfer phase, by the accretion-induced collapse (AIC) of a white dwarf.

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