Simulation of a population of gravitational wave-driven neutron stars

Details Simulation of a population of gravitational wave-driven neutron stars Simulation of a population of gravitational wave-driven neutron stars

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005cqgra..22s1027p&link_type=abstract

Classical and Quantum Gravity, Volume 22, Issue 18, pp. S1027-S1039 (2005).

Physics

Scientific paper

I study, via a Monte Carlo simulation, a population of neutron stars evolving through the emission of gravitational waves. A starting population, with ages uniformly distributed back to 100 Myr (or 500 Myr), is evolved in the galactic gravitational potential to the present time. Neutron stars' natal kick velocity and the Gould Belt, with an enhanced formation rate, are taken into account. Neutron stars' ellipticity is assumed to be distributed exponentially with mean value treated as a parameter. The detectability of the emitted gravitational signals, by the first and planned second generation of interferometric detectors, is estimated.

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