Gravitational waves from kinks on infinite cosmic strings

Kawasaki, Masahiro; Miyamoto, Koichi; Nakayama, Kazunori

doi:10.1103/physrevd.81.103523

Cited by 37 publications

(55 citation statements)

References 46 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As for the detection of cosmic string network, we have discussed the expected weak lensing signals based on a very simple model, and the model prediction should be further improved for future application to the lensing measurements. There are several missing pieces, including the contribution of tensor perturbations [120][121][122][123][124] and the correlation between different string segments [74], which may enhance the signal-to-noise ratio. We hope to come back these issues near future.…”

Section: Discussionmentioning

confidence: 99%

Weak lensing generated by vector perturbations and detectability of cosmic strings

Yamauchi

Namikawa

Taruya

2012

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract. We study the observational signature of vector metric perturbations through the effect of weak gravitational lensing. In the presence of vector perturbations, the nonvanishing signals for B-mode cosmic shear and curl-mode deflection angle, which have never appeared in the case of scalar metric perturbations, naturally arise. Solving the geodesic and geodesic deviation equations, we drive the full-sky formulas for angular power spectra of weak lensing signals, and give the explicit expressions for E-/B-mode cosmic shear and gradient-/curl-mode deflection angle. As a possible source for seeding vector perturbations, we then consider a cosmic string network, and discuss its detectability from upcoming weak lensing and CMB measurements. Based on the formulas and a simple model for cosmic string network, we calculate the angular power spectra and expected signal-to-noise ratios for the B-mode cosmic shear and curl-mode deflection angle. We find that the weak lensing signals are enhanced for a smaller intercommuting probability of the string network, P , and they are potentially detectable from the upcoming cosmic shear and CMB lensing observations. For P ∼ 10 −1 , the minimum detectable tension of the cosmic string will be down to Gµ ∼ 5×10 −8 . With a theoretically inferred smallest value P ∼ 10 −3 , we could even detect the string with Gµ ∼ 5 × 10 −10 .

show abstract

Section: Discussionmentioning

confidence: 99%

Weak lensing generated by vector perturbations and detectability of cosmic strings

Yamauchi

Namikawa

Taruya

2012

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…[30]. frequency comparable to the Hubble parameter are, as discussed in [11], emitted by new kinks, one finds that the peak at ' $ 100ð' $ 5Þ is due to GWs emitted slightly before the recombination (reionization) by kinks which are born a little before the recombination (reionization). Since the BB spectrum by kinks is comparable to or somewhat greater than that by network dynamics in some regions, the total BB power spectrum induced by cosmic strings is deformed by the effect of the GWs from kinks on infinite strings.…”

Section: Bb Power Spectrummentioning

confidence: 95%

“…III, we briefly review the result of Ref. [11] for the GW spectrum from kinks which will be used in the following analysis. In Sec.…”

Section: Introductionmentioning

confidence: 99%

B-mode polarization induced by gravitational waves from kinks on infinite cosmic strings

2010

Self Cite

View full text Add to dashboard Cite

We investigate the effect of the stochastic gravitational wave (GW) background produced by kinks on infinite cosmic strings, whose spectrum was derived in our previous work, on the B-mode power spectrum of the cosmic microwave background (CMB) anisotropy. We find that the B-mode polarization due to kinks is comparable to that induced by the motion of the string network and hence the contribution of GWs from kinks is important for estimating the B-mode power spectrum originating from cosmic strings. If the tension of cosmic strings is large enough, i.e., G * 10 À8 , B-mode polarization induced by cosmic strings can be detected by future CMB experiments.

show abstract

“…The spectrum of the gravitational wave background originating from kinks on infinite strings are calculated in ref. [33].…”

Section: Contentsmentioning

confidence: 99%

Improved calculation of the gravitational wave spectrum from kinks on infinite cosmic strings

Matsui

Horiguchi

Nitta

et al. 2016

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Gravitational wave observations provide unique opportunities to search for cosmic strings. One of the strongest sources of gravitational waves is discontinuities of cosmic strings, called kinks, which are generated at points of intersection. Kinks on infinite strings are known to generate a gravitational wave background over a wide range of frequencies. In this paper, we calculate the spectrum of the gravitational wave background by numerically solving the evolution equation for the distribution function of the kink sharpness. We find that the number of kinks for small sharpness is larger than the analytical estimate used in a previous work, which makes a difference in the spectral shape. Our numerical approach enables us to make a more precise prediction on the spectral amplitude for future gravitational wave experiments.

show abstract

Gravitational waves from kinks on infinite cosmic strings

Cited by 37 publications

References 46 publications

Weak lensing generated by vector perturbations and detectability of cosmic strings

Weak lensing generated by vector perturbations and detectability of cosmic strings

B-mode polarization induced by gravitational waves from kinks on infinite cosmic strings

Improved calculation of the gravitational wave spectrum from kinks on infinite cosmic strings

Contact Info

Product

Resources

About