2010A&A...521A..85Y

The gravitational wave (GW) background in the range 0.01-30 mHz has been assumed to be dominated by unresolved radiation from double white dwarf binaries (DWDs). Recent investigations indicate that, at short periods, a number of DWDs should be resolvable sources of GW. We characterize the GW signal which would be detected by LISA from DWDs in the Galaxy. We have constructed a Galactic model in which we consider distinct contributions from the bulge, thin disc, thick disc, and halo, and subsequently executed a population synthesis approach to determine the birth rates, numbers, and period distributions of DWDs within each component. In the Galaxy as a whole, our model predicts the current birth rate of DWDs to be 3.21x10^–2yr^–1, the local density to be 2.2x10^–4pc^–3 and the total number to be 2.76x10⁸. Assuming SNIa are formed from the merger of two CO white dwarfs, the SNIa rate should be 0.0013yr^–1. The frequency spectra of DWD strain amplitude and number distribution are presented as a function of galactic component, DWD type, formation channel, and metallicity. We confirm that CO+He and He+He white dwarf (WD) pairs should dominate the GW signal at very high frequencies (logfHz^–1>-2.3), while CO+CO and ONeMg WD pairs have a dominant contribution at logfHz^–1≤-2.3. Formation channels involving two common-envelope (CE) phases or a stable Roche lobe overflow phase followed by a CE phase dominate the production of DWDs detectable by LISA at logfHz^–1>-4.5. DWDs with the shortest orbital periods will come from the CE+CE channel. The Exposed Core plus CE channel is a minor channel. A number of resolved DWDs would be detected, making up 0.012% of the total number of DWDs in the Galaxy. The majority of these would be CO+He and He+He pairs formed through the CE+CE channel.