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Magnetic Field Decay in the Non-superfluid Regions of Neutron Star Cores

Published online by Cambridge University Press:  12 April 2016

A.G. Muslimov  and
H.M. Van Horn
A.G. Muslimov
Affiliation:
Department of Physics and Astronomy and C.E. Kenneth Mees Observatory, University of Rochester, Rochester NY 14627-0011USA
H.M. Van Horn
Affiliation:
Department of Physics and Astronomy and C.E. Kenneth Mees Observatory, University of Rochester, Rochester NY 14627-0011USA

Abstract

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We consider a simple model for the evolution of a poloidal magnetic field initally trapped in a region containing normal npe matter within the outerliquid core of a neutron star. We have performed numerical computations for neutron stars with masses of 1.4, 1.6, and 1.7 M⊙ that undergo very rapid cooling due to the direct Urca process. Because the timescale for the magnetic field decay is directly proportional to T2, such a cooling history produces a rapid decline in the magnetic-field strength B, even for B as low as ∼ 1012 G. In particular, we show that an initially quasi-homogeneous magnetic field of strength B = 1012 G declines during the first ∼ 1 Myr.

Type
Posters
Information
International Astronomical Union Colloquium , Volume 147: The Equation of State in Astrophysics , 1994 , pp. 591 - 595
Copyright
Copyright © Cambridge University Press 1994

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