Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars

Ali Alpar, M.; Baykal, Altan

doi:10.1111/j.1365-2966.2006.10893.x

Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars

Aug, 2006

Published in:

Mon.Not.Roy.Astron.Soc. 372 (2006) 489

e-Print:

astro-ph/0608055 [astro-ph]

DOI:

10.1111/j.1365-2966.2006.10893.x

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Abstract: (arXiv)

Almost all pulsars with anomalous positive

\ddot \Omega

measurements (corresponding to anomalous braking indices in the range 5

<n<

100), including all the pulsars with observed large glitches (

\Delta\Omega/\Omega

>

10

^{-7}

) as well as post glitch or interglitch

\ddot \Omega

measurements obey the scaling between

\ddot \Omega

and glitch parameters originally noted in the Vela pulsar. Negative second derivative values can be understood in terms of glitches that were missed or remained unresolved. We discuss the glitch rates and a priori probabilities of positive and negative braking indices according to the model developed for the Vela pulsar. This behavior supports the universal occurrence of a nonlinear dynamical coupling between the neutron star crust and an interior superfluid component. The implied lower limit to dynamical energy dissipation in a neutron star with spindown rate

\dot \Omega

is

\dot E_{diss}> 1.7 \times 10 ^{-6} \dot E_{rot}

. Thermal luminosities and surface temperatures due to dynamical energy dissipation are estimated for old neutron stars which are spinning down as rotating magnetic dipoles beyond the pulsar death line.

pulsars: general

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Figures(0)

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