Gravitational radiation from a solid-crust neutron star

Details Gravitational radiation from a solid-crust neutron star Gravitational radiation from a solid-crust neutron star

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985natur.314..334a&link_type=abstract

Nature (ISSN 0028-0836), vol. 314, March 28, 1985, p. 334-336.

Statistics

Computation

21

Computational Astrophysics, Neutron Stars, Stellar Gravitation, Stellar Radiation, Energy Dissipation, Pulsars, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Structure

Scientific paper

The role of gravitational radiation in the angular momentum loss of millisecond pulsars is investigated. Balancing gravitational radiation power against the rate of rotational energy loss, the authors find that if the effective triaxiality ɛeff exceeds ɛmax ≡ 10-9, gravitational radiation alone would spin a millisecond pulsar down at a faster rate than the observed P. It is shown that ɛeff very low ɛmax, so that gravitational radiation is not likely to play a major role in the evolution of millisecond pulsars even in the absence of damping. Damping times for precession of the solid crust are estimated to be <2×103 yr.

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