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Extragalactic Gravitational Wave Background


General shape of the GWB formed by extragalactic binaries  was considered in earlier works (Lipunov et al., 1987a[120], Hills et al., 1990[66]). Now we turn to the question about how the GWB changes if one makes observations with a GW detector with a specific angular resolution tex2html_wrap_inline12063 . It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs  (at a rate of tex2html_wrap_inline89451 per 100 year) and NS (at a rate of tex2html_wrap_inline89451 per tex2html_wrap_inline12215 - tex2html_wrap_inline12217 year) in our Galaxy, against a background of the extragalactic stochastic GW. In analogy with our Galaxy, critical frequencies must exist for the extragalactic background. Above them only merging  NS will cross a given frequency interval at a rate of up to tex2html_wrap_inline8945100 per year if one observes all galaxies within 200 Mpc. Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. The same questions as for the Milky Way galaxy are addressed.

Mike E. Prokhorov
Sat Feb 22 18:38:13 MSK 1997