Gravitational wave bursts from cosmic strings

Physical Review Letters

Volumn 85, Issue 18, 2000, Pages 3761-3764

  Damour, Thibault ^a   Vilenkin, Alexander ^b  

^a INSTITUT DES HAUTES ÉTUDES SCIENTIFIQUES   (France)

^b TUFTS UNIVERSITY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ASTROPHYSICS; ELEMENTARY PARTICLES; FOURIER TRANSFORMS; FREQUENCY DOMAIN ANALYSIS; PERTURBATION TECHNIQUES; TIME DOMAIN ANALYSIS;

COSMIC STRINGS; COSMOLOGICAL NETWORK; HIGH FREQUENCY GRAVITATIONAL WAVES;

COSMIC RAYS;

EID: 0034294425     PISSN: 00319007     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevLett.85.3761     Document Type: Article

References (18)

1. For a review of string properties and evolution see, e.g., A. Vilenkin and E. P. S. Shellard, Cosmic Strings and Other Topological Defects (Cambridge University Press, Cambridge, 1994).
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8. The possibility of detection of gravitational wave bursts from cosmic string cusps has been pointed out by V. Berezinsky, B. Hnatyk, and A. Vilenkin, astro-ph/0001213.
9. The actual length of the loop changes as the loop oscillates. The invariant length is defined as l = E/μ, where E is the loop's energy in its center-of-mass frame.
10. N. Turok, Nucl. Phys. B242, 520 (1984).
11. The waveform (4) differs from that obtained earlier by T. Vachaspati, Phys. Rev. D 35, 1767 (1987). As shown in [17], the leading term considered by Vachaspati is pure gauge and can be removed by a coordinate transformation.
12. The horizontal lines in Fig. 1 (and Fig. 2) should not be used to estimate the SNR for the detection of the stochastic background, which is optimized by a different filtering technique.
13. V. Berezinsky, B. Hnatyk, and A. Vilenkin, astro-ph/ 0001213.
14. m ∼ 1. By contrast, in the model of [13] the (300 times more numerous) GRBs come from a larger volume, up to redshifts ∼4.
15. R. Schilling (private communication).
16. P. L. Bender and D. Hils, Classical Quantum Gravity 14, 1439 (1997).
17. T. Damour and A. Vilenkin (to be published).
18. D. Garfinkle and T. Vachaspati, Phys. Rev. D 37, 257 (1988).