Galactic Binary Gravitational Wave Noise within LISA Frequency Band

Details Galactic Binary Gravitational Wave Noise within LISA Frequency Band Galactic Binary Gravitational Wave Noise within LISA Frequency Band

1998-01-06

arxiv.org/abs/astro-ph/9801034v1

Astrophys.J.494:674-679,1998

Astronomy and Astrophysics

Astrophysics

16 pages with 1 eps figure, aasms4.sty, to appear in the ApJ vol. 494 February 20, 1998 issue

Scientific paper

10.1086/305217

Gravitational wave noise associated with unresolved binary stars in the Galaxy is studied with the special aim of determining the upper frequency at which it stops to contribute at the rms noise level of the proposed space-born interferometer (LISA). The upper limit to this background is derived from the statistics of SN Ia explosions, part of which can be triggered by binary white dwarf coalescences. The upper limiting frequency at which binary stochastic noise crosses LISA rms sensitivity is found to lie within the range 0.03-0.07 Hz, depending on the galactic binary white dwarf coalescence rate. To be reliably detectable by LISA, the energy density of relic cosmological background per logarithmic frequency interval should be Omega_{GW}h_{100}^2>10^{-8} at f>0.03 Hz.

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