| BINARY MERGER AND COALESCENCE |
Coalescing binary neutron stars are among the most promising sources of
gravitational radiation for detection by interferometers such as LIGO,
VIRGO and GEO. LIGO has been designed and optimized to detect these
events at a distance of 200 Mpc after significant interferometric
improvements. To accomplish this, it has been devised to be most sensitive
at as low a frequency as possible (approximately 200 Hz) where the waveform
from the binary neutron star is strongest. However, the waveform at this
frequency is due almost solely to the inspiral phase and contains little
information about the coalescence itself.
The coalescence regime probably lies at or beyond the upper end of the
frequency range accessible to broad-band detectors, but it may be observed
using specially designed narrow band interferometers or resonant detectors.
The extraction and examination of this waveform will reveal the masses,
spins and orbital parameters of these systems. A study of this phenomenon
also should yield information about the neutron star radii, and hence the
equation of state for nuclear matter which will manifest itself only in
the coalescence waveform.
Recent studies suggest that binary inspiral due to the effects of energy
loss by the gravitational radiation reaction (GRR),
and the eventual coalescence
of the component stars, may be detectable by these instruments at a rate of
several per year. The inspiral phase comprises the last several thousand
binary orbits and covers the frequency range approximately 10 to 1000 Hz,
where the broad-band interferometers are most sensitive.
The coalescence regime probably lies at or beyond the upper end of the frequency range accessible to broad-band detectors, but it may be observed using specially designed narrow band interferometers or resonant detectors. The extraction and examination of this waveform will reveal the masses, spins and orbital parameters of these systems. A study of this phenomenon also should yield information about the neutron star radii, and hence the equation of state for nuclear matter which will manifest itself only in the coalescence waveform.
Recent studies suggest that binary inspiral due to the effects of energy loss by the gravitational radiation reaction (GRR), and the eventual coalescence of the component stars, may be detectable by these instruments at a rate of several per year. The inspiral phase comprises the last several thousand binary orbits and covers the frequency range approximately 10 to 1000 Hz, where the broad-band interferometers are most sensitive.