Pulsar Constraints on Neutron Star Structure and Equation of State

Details Pulsar Constraints on Neutron Star Structure and Equation of State Pulsar Constraints on Neutron Star Structure and Equation of State

1999-09-08

arxiv.org/abs/astro-ph/9909146v1

Phys.Rev.Lett.83:3362-3365,1999

Astronomy and Astrophysics

Astrophysics

5 pages, including figures. To appear in Physical Review Letters

Scientific paper

10.1103/PhysRevLett.83.3362

With the aim of constraining the structural properties of neutron stars and the equation of state of dense matter, we study sudden spin-ups, glitches, occurring in the Vela pulsar and in six other pulsars. We present evidence that glitches represent a self-regulating instability for which the star prepares over a waiting time. The angular momentum requirements of glitches in Vela indicate that at least 1.4% of the star's moment of inertia drives these events. If glitches originate in the liquid of the inner crust, Vela's `radiation radius' must exceed ~12 km for a mass of 1.4 solar masses. Observational tests of whether other neutron stars obey this constraint will be possible in the near future.

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