Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.276..347c&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 276, NO. 1/SEP1, P. 347, 1995
Astronomy and Astrophysics
Astronomy
51
Radiation Mechanisms: Nonthermal - Methods: Statistical - Binaries: General - Stars: Neutron - Pulsars: General - Galaxy: Stellar Content
Scientific paper
We use a detailed computer simulation of the galactic pulsar population to estimate the number of neutron star-neutron star (NS-NS) binaries in the Galaxy. Our calculations are based on the three known systems of this class, PSRs B1534+12, B1913+16 and B2303+46, and use the latest results from sensitive pulsar surveys covering a large area of sky. We estimate that there are ˜240 potentially observable NS-NS binaries in the Galaxy. As B1534+12 and B1913+16 will eventually merge due to the emission of gravitational radiation in a known time-scale, we can deduce the galactic merging rate ℜ of NS-NS binaries; we estimate ℜ ˜10-7 yr-1. Taking account of several factors which affect the number of NS-NS systems that can be detected, we arrive at a more realistic nominal value of ℜ ˜ 3 x 10-6 yr-1. Thus we have to look far beyond the Galaxy to the Gpc range in order to witness several NS-NS star mergings per year. The next generation of gravitational wave detectors are expected to have sensitivities approaching that required to probe to such distances.
Curran Stephen J.
Lorimer Dunc. R.
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