Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aipc..456...61w&link_type=abstract
The second international laser interferometer space antenna symposium (LISA) on the detection and observation of gravitational w
Other
21
Gravitational Wave Detectors And Experiments, Gravitational Radiation Detectors, Mass Spectrometers, And Other Instrumentation And Techniques
Scientific paper
We use recent population synthesis models for the production of close double white dwarfs [1] to calculate their gravitational wave spectrum. The properties of that spectrum are nearly independent of the assumptions involved in that model, depending in normalization only on the frequency of primordial binaries of intermediate mass, orbital periods of a few years, and mass ratios near unity. The gravitational wave energy density at lower frequencies in the LISA window will provide a robust measure of the galactic type Ia supernova rate. Roughly 3600 individual close white dwarf binaries should be resolvable at frequencies above the confusion limit at 3.6 mHz, with 90 percent of these systems showing detectable orbital evolution due to gravitational radiation within a 5-year mission lifetime. For these binaries, distances and chirp masses can be obtained independently, making it possible to study their intrinsic and spatial distributions separately. In an exceptional one or two cases, it should be possible to detect v̈ within a 5-year mission, providing an important probe into tidal heating processes preceding a merger. The probability of observing an actual merger within a 5-year mission is small (about 15%), but not negligible. Only a small fraction of mergers can produce supernovae. However, it will be possible to identify supernova progenitors from the general population of close double white dwarfs, and to predict their outburst dates with uncertainties as small as a century, or even a few years in the most favorable of cases.
Han Zhanwen
Webbink Ronald F.
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