Pulsar Constraints on Neutron Star Structure and Equation of State

Bennett Link; Richard I. Epstein; James M. Lattimer

doi:10.1103/PhysRevLett.83.3362

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Pulsar Constraints on Neutron Star Structure and Equation of State

Bennett Link, Richard I. Epstein, and James M. Lattimer

Phys. Rev. Lett. 83, 3362 – Published 25 October 1999

Abstract

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 $\geq 1.4 %$ of the star's moment of inertia drives these events. If glitches originate in the liquid of the inner crust, Vela's “radiation radius” $R_{\infty}$ must exceed $≃ 12 km$ for a mass of ${1.4 M}_{⊙}$ . Observational tests of whether other neutron stars obey this constraint will be possible in the near future.

Received 6 May 1999

DOI:https://doi.org/10.1103/PhysRevLett.83.3362

Authors & Affiliations

Bennett Link^*

Department of Physics, Montana State University, Bozeman, Montana 59717

Richard I. Epstein^†

Los Alamos National Laboratory, Mail Stop D436, Los Alamos, New Mexico 87545

James M. Lattimer^‡

Department of Physics and Astronomy, State University of New York, Stony Brook, New York 11974-3800

^*Also at Los Alamos National Laboratory, Los Alamos, NM.Electronic address: blink@dante.physics.montana.edu
^†Electronic address: epstein@lanl.gov
^‡Electronic address: lattimer@astro.sunysb.edu

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Vol. 83, Iss. 17 — 25 October 1999

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