Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..tsf..ca06t&link_type=abstract
American Physical Society, Joint Fall Meeting of the Texas Section of the APS, AAPT, and Zone 13 of the SPS, October 15-17, 1998
Astronomy and Astrophysics
Astrophysics
Scientific paper
We report on work that is part of a comprehensive study of the gravitational radiation emitted by binaries consisting of a rotating black hole and a stellar-mass object (which could be a main-sequence star, a white dwarf or a neutron star). Studies of this kind are of direct relevance to the NASA OMEGA mission and the projected European LISA mission, which propose to set up interferometric gravitational wave detectors in space. We present the modeling of astrophysical processes having direct impact on the study of gravitational radiation detectable by these types of interferometers; that is, astrophysical systems for which the gravitational wave signal is in the low-frequency band (10-4-1 Hz), which is the band involving massive black holes (BH) with masses in the range 10^3M_solar <= M_h<= 10^8M_solar . The models are developed with the viewpoint that binary collisions can be approximated as perturbations about the object representing the final outcome of the collision: the close-limit approximation. We particularly study the signal to noise (SNR) of the waveforms that can be constructed from solutions generated by the the close-limit approximation. We also introduce the method of matched filters to relate for any source of waves, the SNR, obtained from matched filtering, to the gravitational waveform measured by the detector and to the spectral density of the strain noise in the detector.
Diaz Mario C.
Rodríguez Adrienne
Torres Charlie Jr.
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