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Modelling pulsar glitches with realistic pinning forces: a hydrodynamical approach

Haskell, B. and Pizzochero, P. M. and Sidery, Trevor Llyod (2012) Modelling pulsar glitches with realistic pinning forces: a hydrodynamical approach. Monthly Notices of the Royal Astronomical Society, 420 (1). pp. 658-671. ISSN 0035-8711 (print) ; 1365-2966 (online)

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Official URL: http://dx.doi.org/10.1111/j.1365-2966.2011.20080.x

Abstract

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 Delta nu/nu approximate to 10(-11) to 10(-5). In this paper, we focus on the 'giant' glitches, i.e. glitches with fractional increases in the spin rate of the order of Delta nu/nu approximate to 10(-6), 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.

Item Type:Article
Uncontrolled Keywords:stars: neutron; pulsars: general; pulsars: individual: PSR B0833-45
Subjects:Q Science > QB Astronomy > QB460-466 Astrophysics
Q Science > QB Astronomy
ID Code:18973
Deposited By:Trevor Llyod Sidery
Deposited On:06 Apr 2012 11:48
Last Modified:06 Apr 2012 11:48

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