Population Boundaries for Evolving White Dwarf Binaries on the LISA Sensitivity Curve

Details Population Boundaries for Evolving White Dwarf Binaries on the LISA Sensitivity Curve Population Boundaries for Evolving White Dwarf Binaries on the LISA Sensitivity Curve

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.7411k&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #74.11; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Double White Dwarf (DWD) binaries are considered to be among the most promising sources for gravitational waves for LISA. Theoretical constraints on the properties of the white dwarf stars allow us to map out the evolutionary trajectories of these systems in the ``absolute" gravitational wave strain-frequency domain. We have identified population boundaries where inspiralling and/or mass transferring systems can be found. Further, we define sub-domains in which systems undergo stable/unstable, sub/super-Eddington mass transfer and the progenitors of Type Ia supernovae reside. We do this in the context of either direct impact or disk accretion, efficient or inefficient tidal coupling between the spins of the components and the orbit. We identify for what subset of these populations it should be possible to measure frequency shifts and determine binary system parameters like chirp mass and luminosity distance, given LISA's anticipated operational time. This work has been supported in part by NSF grants AST 04-07070 and PHY 03-26311 and in part through NASA's ATP program grant NAG5-13430.

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