Limiting angular velocity of realistic relativistic neutron star models

Details Limiting angular velocity of realistic relativistic neutron star models Limiting angular velocity of realistic relativistic neutron star models

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991zphya.339..211w&link_type=abstract

Zeitschrift für Physik A Hadrons and Nuclei, Volume 339, Issue 1, pp.211-215

Physics

4

97.10.Kc, 97.60.Jd

Scientific paper

The Keplerian velocity as well as those frequencies at which instability against gravitational radiation-reaction sets in are calculated for rotating neutron star models of gravitational mass 1.5 M &sun;. The investigation is based on four different, realistic neutron star matter equations of state. Our results indicate that the gravitational radiation instability sets in well below (i.e., 63 71% of) the Keplerian frequency, and that young neutron stars are limited to rotational periods greater than about 1 ms. In young and therefore hot ( T≈1010 K) neutron stars the m=5(±1) modes and in old stars after being spun up and reheated by mass accretion, the m=4 and/or m=3 modes may set the limit on stable rotation.

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