Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts

Details Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts

Publishing date

Jan 2002

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...564..909c&link_type=abstract

Journals

The Astrophysical Journal, Volume 564, Issue 2, pp. 909-913.

Science

Astronomy and Astrophysics

Field

Astronomy

Additional info 2

7

Additional info 3

Dense Matter, Stars: Evolution, Stars: Interiors, Stars: Neutron, Stars: Rotation

Type

Scientific paper

Abstract

As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central density increases and the nuclear matter in its core converts to quark matter, which leads to a drastic decrease of the stellar moment of inertia, and even results in an era of spin-up of the pulsar (Glendenning, Pei, & Weber 1997). We find that given a certain equation of state in the liquid core, even if the backbending of the moment of inertia as a function of the rotating frequency occurs, an increase of the total moment of inertia by only 1% could carry adequate angular momentum and stop the star spin-up. This small discrepancy in the total moment of inertia might be due to the different properties of subnuclear matter in the crust, especially to different transition density and pressure at the inner boundary of the solid crust between various models. The strong dependence of the phenomenon of backbending on the physical state of the crust provides, in principle, a new observational approach to check and constrain theories on subnuclear matter.

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