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Gravitational radiation from rapidly rotating nascent neutron starsWe study the secular evolution and gravitational wave signature of a newly formed, rapidly rotating neutron star. The neutron star may arise from core collapse in a massive star or from the accretion-induced collapse of a white dwarf. After a brief dynamical phase, the nascent neutron star settles into an axisymmetric, secularly unstable state. Gravitational radiation drives the star to a nonaxisymmetric, stationary equilibrium configuration via the bar-mode instability. The emitted quasi-periodic gravitational waves have a unique signature: the wave frequency sweeps downward from a few hundred Hertz to zero, while the wave amplitude increase from zero to a maximum and then decays back to zero. Such a wave signal could detected by broadband gravitational wave interferometers currently being constructed. We also characterize two other types of gravitational wave signals that could arise in principle from a rapidly rotating, secularly unstable neutron star: a high-frequency (f greater than or approximately = 1000 Hz) wave which increases the pattern-speed of the star, and a wave that actually increases the angular momentum of the star.
Document ID
19950054920
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Lai, Dong
(Cornell Univ. Ithaca, NY, United States)
Shapiro, Stuart L.
(Cornell Univ. Ithaca, NY, United States)
Date Acquired
August 16, 2013
Publication Date
March 20, 1995
Publication Information
Publication: The Astrophysical Journal, Part 1
Volume: 442
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
95A86519
Funding Number(s)
CONTRACT_GRANT: NAGW-2364
CONTRACT_GRANT: NSF AST-91-19475
Distribution Limits
Public
Copyright
Other

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