Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars

Details Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars

2006-08-02

arxiv.org/abs/astro-ph/0608055v1

Mon.Not.Roy.Astron.Soc.372:489,2006

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2006.10893.x

Almost all pulsars with anomalous positive $\ddot \Omega $ measurements (corresponding to anomalous braking indices in the range 5$$ 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.

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