- Conference date: 19-23 June 2006
- Location: Greenbelt, Maryland (USA)
Double white dwarf (DWD) binary systems are considered to be among the most promising sources of gravitational waves for LISA. The path that DWD binaries traverse across LISA’s “absolute” strain‐frequency domain during the detached, inspiral phase of their evolution is well‐understood. Theoretical constraints on the properties of the white dwarf stars allow us also to map out the evolutionary trajectories of DWD binaries during a phase when they are semi‐detached and undergoing stable mass transfer. We have identified population boundaries that define distinct sub‐domains in LISA’s strain‐frequency diagram where inspiraling and/or mass‐transferring systems will and will not be found; sub‐domains where progenitors of Type Ia supernovae reside also are identified. We identify for what subset of these populations it should be possible to measure frequency shifts and, hence, directly follow orbit evolutions, given LISA’s anticipated operational time. We show how such measurements should permit the determination of binary system parameters, such as luminosity distances and chirp masses, for mass‐transferring as well as inspiraling systems.
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