Population Boundaries for Galactic White Dwarf Binaries in LISA's Amplitude-Frequency Domain

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dc.creatorKopparapu, Ravi Kumar
dc.creatorTohline, Joel E.
dc.date2006-10-18
dc.date.accessioned2026-07-07T10:40:34Z
dc.date.available2026-07-07T10:40:34Z
dc.descriptionDetached, inspiraling and semi-detached, mass-transferring double white dwarf (DWD) binary systems are both expected to be important sources for the proposed space-based gravitational-wave detector, LISA. The mass-radius relationship of individual white dwarf stars in combination with the constraints imposed by Roche geometries permit us to identify population boundaries for DWD systems in LISA's ``absolute'' amplitude-frequency diagram. With five key population boundaries in place, we are able to identify four principal population sub-domains, including one sub-domain that identifies where progenitors of Type Ia supernovae will reside. Given one full year of uninterrupted operation, LISA should be able to measure the rate at which the gravitational-wave frequency $f$ and, hence, the orbital period is changing in the highest frequency subpopulation of our Galaxy's DWD systems. We provide a formula by which the distance to each DWD system in this subpopulation can be determined; in addition, we show how the masses of the individual white dwarf stars in mass-transferring systems may be calculated.
dc.description23 pages, 3 figures, Accepted for publication in Astrophysical Journal
dc.identifierhttps://arxiv.org/abs/astro-ph/0610555
dc.identifierhttp://arxiv.org/abs/astro-ph/0610555
dc.identifierAstrophys.J.655:1025-1032,2007
dc.identifierdoi:10.1086/510234
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/181369
dc.subjectAstrophysics
dc.titlePopulation Boundaries for Galactic White Dwarf Binaries in LISA's Amplitude-Frequency Domain
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