Postaccretion magnetic field evolution of neutron stars

Details Postaccretion magnetic field evolution of neutron stars Postaccretion magnetic field evolution of neutron stars

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...442l..53y&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 442, no. 2, p. L53-L56

Astronomy and Astrophysics

Astrophysics

16

Magnetic Field Configurations, Pulsars, Stellar Evolution, Stellar Magnetic Fields, Stellar Models, Accretion Disks, Electromagnetic Surface Waves, Stellar Mass Accretion

Scientific paper

We present the first calculations of magnetic field evolution following accretion-induced field reduction which demonstrate the possibility of subsequent surface magnetic field growth. Assuming the preaccretion field is pushed down or advected below the accreting material, we show that significant diffusion of the suppressed field back to the surface can occur within a Galactic age approximately 1010 yr. This produces surface fields characteristic of standard pulsars if the total mass transferred is below a critical value delta Mc approximately 0.04 solar masses. We then show how this provides a natural explanation for the existence of old pulsars with high inferred surface dipole fields which are still observable. Using our results in conjunction with a model for accretion-induced field reduction we predict the evolution of a binary pulsar's spin and magnetic field through its postaccretion lifetime. This analysis also provides a qualitative explanation for a recent suggestion that the magnetic fields and spins of recycled pulsars have a bimodal distribution.

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