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Gravitational wave noise associated with unresolved binary stars in theGalaxy is studied with the special aim of determining the upper frequency atwhich it stops to contribute at the rms noise level of the proposed space-borninterferometer (LISA). The upper limit to this background is derived from thestatistics of SN Ia explosions, part of which can be triggered by binary whitedwarf coalescences. The upper limiting frequency at which binary stochasticnoise crosses LISA rms sensitivity is found to lie within the range 0.03-0.07Hz, depending on the galactic binary white dwarf coalescence rate. To bereliably detectable by LISA, the energy density of relic cosmologicalbackground per logarithmic frequency interval should beOmega_{GW}h_{100}^2>10^{-8} at f>0.03 Hz.Comment: 16 pages with 1 eps figure, aasms4.sty, to appear in the ApJ vol. 494  February 20, 1998 issu

Galactic Binary Gravitational Wave Noise within the LISA Frequency Band