Journal Article

Modelling pulsar glitches with realistic pinning forces: a hydrodynamical approach

B. Haskell, P. M. Pizzochero and T. Sidery

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 420, issue 1, pages 658-671
Published in print February 2012 | ISSN: 0035-8711
Published online January 2012 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2011.20080.x
Modelling pulsar glitches with realistic pinning forces: a hydrodynamical approach

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Although pulsars are some of the most stable clocks in the Universe, many of them are observed to ‘glitch’, i.e. to suddenly increase their spin frequency  with fractional increases that range from  to . In this paper, we focus on the ‘giant’ glitches, i.e. glitches with fractional increases in the spin rate of the order of , that are observed in a subclass of pulsars including the Vela. We show that giant glitches can be modelled with a two-fluid hydrodynamical approach. The model is based on the formalism for superfluid neutron stars of Andersson & Comer and on the realistic pinning forces of Grill & Pizzochero. We show that all stages of Vela glitches, from the rise to the post-glitch relaxation, can be reproduced with a set of physically reasonable parameters and that the sizes and waiting times between giant glitches in other pulsars are also consistent with our model.

Keywords: stars: neutron; pulsars: general; pulsars: individual: PSR B0833–45

Journal Article.  10883 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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