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LISA and the Future of Gravitational Wave Physics and Astronomy [electronic resource].

Published
Washington, D.C. : United States. Dept. of Energy. Office of Science, 2003.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy.
Additional Creators
Fermi National Accelerator Laboratory, United States. Department of Energy. Office of Science, and United States. Department of Energy. Office of Scientific and Technical Information
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Summary
Gravitational waves offer views of the universe which complement those in electromagnetic waves and neutrinos. Just as different frequencies of the electromagnetic spectrum highlight different astrophysical phenomena, different frequencies of gravitational radiation will highlight different kinds of objects. The NASA/ESA Laser Interferometer Space Antenna (LISA), planned for launch in 2010, will detect and measure gravitational radiation from astronomical sources at frequencies 0.0001 Hz to 0.1 Hz (vs. 10-1000 Hz for ground-based detectors like LIGO). LISA will detect continuous signals from: thousands of exotic binary stars in the Milky Way, merging supermassive black holes in the nuclei of merging galaxies at redshifts from 0 to 100, and compact stars scattered into supermassive black holes. The latter will provide precision tests of strong-field predictions of relativity, such as the No-Hair Theorem and energy extraction from rotating black holes. We will conclude with an outline of some of the limitations of, and remarkable possibilities for the future of gravitational wave physics and astronomy.
Report Numbers
E 1.99:1015660
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Note
Published through SciTech Connect.
03/05/2003.
Fermilab Colloquia, Fermi National Accelerator Laboratory (FNAL), Batvia, Illinois (United States), presented on March 05, 2003.
Phinney, Sterl.
Funding Information
AC02-07CH11359
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