Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..541w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 2, May 10, 1992, p. 541-549. Research supported by Max Kade Founda
Astronomy and Astrophysics
Astrophysics
58
Neutron Stars, Relativity, Stellar Rotation, Einstein Equations, Formalism, Stellar Models
Scientific paper
Models of general relativistic rotating neutron stars, constructed from Hartle's (1967) perturbative 'slow' rotation formalism of massive relativistic objects, are compared with their counterparts obtained from the exact solution of Einstein's equations. It is found that both methods, perturbative and exact, lead to compatible results down to rotational Kepler periods P(K) of about 0.5 ms, a value which is by far smaller than the smallest yet observed pulsar period. This finding rests on the reinvestigation of Hartle's method, supplementing it by a self-consistency condition inherent in the determination of the Kepler frequency, and analyzing carefully sequences of star models near their end points. A collection of 17 representative neutron matter equations of state served as an input. Because of its simple structure, Hartle's method should prove to be a practical tool for testing models of the nuclear equation of state with data on pulsar periods. The form of an approximate empirical formula for the general relativistic Kepler frequency is obtained, and proportionality to the Newtonian expression arises in about equal parts from the equatorial flattening and the frame dragging.
Glendenning Norman K.
Weber Fridolin
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