Stochastic gravitational wave backgrounds

Christensen, N.

doi:10.1088/1361-6633/aae6b5

Cited by 266 publications

(206 citation statements)

References 394 publications

(838 reference statements)

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“…6 5 The lack of correlation between time intervals is due to the acausal relationship between distant GW sources, while the lack of correlation between different m is due to statistical isotropy. 6 Note that Cov[X, Y ] S,Ω ≡ XY * S,Ω − X S,Ω Y * S,Ω , which is not equal to Cov[X, Y ] S Ω .…”

Section: Shot Noise and Hierarchical Averagingmentioning

confidence: 99%

Estimating the angular power spectrum of the gravitational-wave background in the presence of shot noise

2019

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There has been much recent interest in studying anisotropies in the astrophysical gravitational-wave (GW) background, as these could provide us with interesting new information about galaxy clustering and large-scale structure. However, this information is obscured by shot noise, caused by the finite number of GW sources that contribute to the background at any given time. We develop a new method for estimating the angular spectrum of anisotropies, based on the principle of combining statistically-independent data segments. We show that this gives an unbiased estimate of the true, astrophysical spectrum, removing the offset due to shot noise power, and that in the limit of many data segments, it is the most efficient (i.e. lowest-variance) estimator possible.

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Section: Shot Noise and Hierarchical Averagingmentioning

confidence: 99%

Estimating the angular power spectrum of the gravitational-wave background in the presence of shot noise

2019

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“…Such a stochastic GW background is mentioned in Ref. [22] to be the most sizable. We have obtained that the probabilities to detect relatively low energy neutrinos, with E " p1˜10 2 q keV, can reach the asymptotic values in Eq.…”

Section: Resultsmentioning

confidence: 96%

“…(11), we get that ρ I p0q " ρp0q. Then, we take that ρ I p0q 11 " F e is the initial probability ("flux) of ν e , ρ I p0q 22 " F x " 1´F e is the initial probability ("flux) of ν x , and ρ I p0q 12 " ρ I p0q 21 " 0, that implies that there are no correlations between the initial fluxes of different flavors. Now Eq.…”

Section: Neutrino Flavor Oscillations In a Gravitational Wavementioning

confidence: 99%

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Neutrino flavor oscillations in stochastic gravitational waves

Dvornikov

2019

Phys. Rev. D

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We study neutrino flavor oscillations in a plane gravitational wave (GW) with circular polarization. For this purpose we use the solution of the Hamilton-Jacobi equation to get the contribution of GW to the effective Hamiltonian for the neutrino mass eigenstates. Then, considering stochastic GWs, we derive the equation for the density matrix for flavor neutrinos and analytically solve it in the two flavors approximation. We predict the ratios of fluxes of different flavors at a detector for cosmic neutrinos with relatively low energies owing to the interaction with such a GW background. The obtained result is compared with the recent observation of the flavor content of the astrophysical neutrinos fluxes. * maxdvo@izmiran.ru

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“…One of the prime targets of gravitational-wave (GW) astronomy in the coming years is going to be the detection of relic GWs that were produced in the early Universe [1]. There is a wealth of possible sources of primordial GWs [2,3], among which cosmological phase transitions [4] represent a particularly well-motivated scenario. Indeed, many extensions of the Standard Model (SM) predict a strong first-order phase transition (SFOPT) in the early Universe that readily results in an observable GW signal [5].…”

Section: Introductionmentioning

confidence: 99%

A fresh look at the gravitational-wave signal from cosmological phase transitions

Alanne

Hügle

Platscher

et al. 2020

J. High Energ. Phys.

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Many models of physics beyond the Standard Model predict a strong first-order phase transition (SFOPT) in the early Universe that leads to observable gravitational waves (GWs). In this paper, we propose a novel method for presenting and comparing the GW signals that are predicted by different models. Our approach is based on the observation that the GW signal has an approximately model-independent spectral shape. This allows us to represent it solely in terms of a finite number of observables, that is, a set of peak amplitudes and peak frequencies. As an example, we consider the GW signal in the real-scalar-singlet extension of the Standard Model (xSM). We construct the signal region of the xSM in the space of observables and show how it will be probed by future space-borne interferometers. Our analysis results in sensitivity plots that are reminiscent of similar plots that are typically shown for dark-matter direct-detection experiments, but which are novel in the context of GWs from a SFOPT. These plots set the stage for a systematic model comparison, the exploration of underlying model-parameter dependencies, and the construction of distribution functions in the space of observables. In our plots, the experimental sensitivities of future searches for a stochastic GW signal are indicated by peak-integrated sensitivity curves. A detailed discussion of these curves, including fit functions, is contained in a companion paper.

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Stochastic gravitational wave backgrounds

Cited by 266 publications

References 394 publications

Estimating the angular power spectrum of the gravitational-wave background in the presence of shot noise

Estimating the angular power spectrum of the gravitational-wave background in the presence of shot noise

Neutrino flavor oscillations in stochastic gravitational waves

A fresh look at the gravitational-wave signal from cosmological phase transitions

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