Gravitational waves from in-spirals of compact objects in binary common-envelope evolution

Detection of gravitational-wave (GW) sources enables the characterisation of binary compact objects and of their in-spiral. However, other dissipative processes can affect the in-spiral. Here we show that the in-spiral of compact objects through a gaseous common-envelope (CE) arising from an evolved stellar companion produces a novel type of GW-sources, whose evolution is dominated by the dissipative gas dynamical friction effects from the CE, rather than the GW-emission itself. The evolution and properties of the GW-signals differ from those of isolated gas-poor mergers significantly. We find characteristic strains of $\sim10^{-23}$-$10^{-21}$ ($10{\rm kpc}/{D}$) for such sources -- observable by next-generation space-based GW-detectors. The evolution of the GW-signal can serve as a probe of the interior regions of the evolved star, and the final stages of CE-evolution, otherwise inaccessible through other observational means. Moreover, such CE-mergers are frequently followed by observable explosive electromagnetic counterparts and/or the formation of exotic stars.

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