Gravitational radiation from cosmic (super)strings: Bursts, stochastic background, and observational windows

By T. Damour, A. Vilenkin. 2004

399 citations recorded by the source corpus.

The gravitational wave (GW) signals emitted by a network of cosmic strings are reexamined in view of the possible formation of a network of cosmic superstrings at the end of brane inflation. The reconnection probability p of intersecting fundamental or Dirichlet strings might be much smaller than 1, and the properties of the resulting string network may differ significantly from those of ordinary strings (which have p=1). In addition, it has been recently suggested that the typical length of newly formed loops may differ by a factor {epsilon}<<1 from its standard estimate. Here, we analyze the effects of the two parameters p and {epsilon} on the GW signatures of strings. We consider both the GW bursts emitted from cusps of oscillating string loops, which have been suggested as candidate sources for the LIGO/VIRGO and LISA interferometers, and the stochastic GW background, which may be detectable by pulsar-timing observations. In both cases we find that previously obtained results are quite robust, at least when the loop sizes are not suppressed by many orders of magnitude relative to the standard scenario. We urge pulsar observers to reanalyze a recently obtained 17-yr combined data set to see whether the large scatter exhibited bymore » a fraction of the data might be due to a transient GW burst activity of some sort, e.g., to a near cusp event.« less

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/781760c393eb91fdc2086d9ec6e31f8c18f3d2db

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Citations in the corpus

Physics, Astrophysics and Cosmology with Gravitational Waves (2009, background): “String theory might lead to the production of cosmic strings, which might be observed through their gravitational wave emission [142].”
The astrophysical gravitational wave stochastic background (2011, background): “In a recent work, Damour & Vilenkin (2000, 2001, 2005) and Siemens et al. (2007) considered the stochastic background created by cusps of oscillating cosmic superstring loops at the end of Brane inflation.”
The POEMMA (Probe of Extreme Multi-Messenger Astrophysics) observatory (2020, background): “Next-generation gravitational-wave detectors are expected to probe Gμ ∼ 10−12 [171, 172].”
Beyond the Standard Models with cosmic strings (2019, methodology): “ [38], after taking into account uncertainties on the loop size at formation and on the number of emitting modes. Note that it can also be strengthened by decreasing the inter-commutation probability [40,121,122]. By using the EPTA sensitivity curve derived in [123], we obtain the upper bound on G, ”
Gravitational-wave sensitivity curves (2014, background): “More speculatively, it has been hypothesized that cosmic strings could also be a potential source (Damour and Vilenkin 2005, Binétruy et al 2012, Aasi et al 2014a).”
Stochastic gravitational wave background from smoothed cosmic string loops (2017, background): “[38] Thibault Damour and Alexander Vilenkin, “Gravitational radiation from cosmic (super)strings: Bursts, stochastic background, and observational windows,” Phys.”
Semianalytic calculation of gravitational wave spectrum nonlinearly induced from primordial curvature perturbations (2018, background): “per, there are yet other mechanisms of GW production in the early universe including those associated with preheating [9{12], phase transitions [13{15], and topological defects such as cosmic strings [16,17]. In particular, it should be noted that the GWs are also produced from the primordial curvat”
Upper Bounds on the Low-Frequency Stochastic Gravitational Wave Background from Pulsar Timing Observations: Current Limits and Future Prospects (2006, methodology): “(14) As emphasized by Damour & Vilenkin (2005), the above expression for the upperbound may be simplified using the fact that both p and ǫeff are less then one and h is expected to be greater than .65: Gµ ≤ 1.5× 10−8c−3/2.”