Pulsar Constraints on Neutron Star Structure and Equation of State
- Department of Physics, Montana State University, Bozeman, Montana 59717 (United States)
- Los Alamos National Laboratory, Mail Stop D436, Los Alamos, New Mexico 87545 (United States)
- Department of Physics and Astronomy, State University of New York, Stony Brook, New York 11974-3800 (United States)
With the aim of constraining the structural properties of neutron stars and the equation of state of dense matter, we study sudden spin-ups, {ital 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 {ge}1.4{percent} of the star`s moment of inertia drives these events. If glitches originate in the liquid of the inner crust, Vela`s {open_quotes}radiation radius{close_quotes} R{sub {infinity}} must exceed {approx_equal}12 km for a mass of 1.4M{sub {circle_dot}} . Observational tests of whether other neutron stars obey this constraint will be possible in the near future. {copyright} {ital 1999} {ital The American Physical Society}
- OSTI ID:
- 692558
- Journal Information:
- Physical Review Letters, Journal Name: Physical Review Letters Journal Issue: 17 Vol. 83; ISSN 0031-9007; ISSN PRLTAO
- Country of Publication:
- United States
- Language:
- English
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