Broad-band gravitational-wave pulses from binary neutron stars in eccentric orbits

Abstract

Maximum gravitational wave emission from binary stars in eccentric orbits occurs near the periastron passage. We show that for a stationary distribution of binary neutron stars in the Galaxy, several high-eccentricity systems with orbital periods in the range from tens of minutes to several days should exist that emit broad gravitational-wave pulses in the frequency range 1-100 mHz. The space interferometer LISA could register the pulsed signal from these system at a signal-to-noise ratio level $S/N>5\sqrt{5}$ in the frequency range $\sim 10^{-3}-10^{-1}$ Hz during one-year observational time. Some detection algorithms for such a signal are discussed.

17 pages, LATEX, 3 figures, Astronomy Letters, 2002, in press; typos corrected, refference added

References in corpus (2)

• The gravitational wave signal from the Galactic disk population of binaries containing two compact objects
• Gravitational wave background from coalescing compact stars in eccentric orbits

Cited by in corpus (2)

• Phasing of gravitational waves from inspiralling eccentric binaries
• Accurate and efficient gravitational waveforms for certain galactic compact binaries