Detecting circular polarisation in the stochastic gravitational-wave background from a first-order cosmological phase transition

Ellis, John; Fairbairn, Malcolm; Lewicki, Marek; Vaskonen, Ville; Wickens, Alastair

doi:10.1088/1475-7516/2020/10/032

Cited by 22 publications

(44 citation statements)

References 129 publications

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“…Our result is consistent with the results reported in ref. [64], which require strong first-order phase transitions, i.e., α ∼ 1, for a detectable polarized signal; see the first right panel of their figure (8). The strength of the transition α is the ratio of vacuum to radiation energy density and it is related to the kinetic energy induced in the plasma by the efficiency κ, which becomes ∼ 55% of the radiation energy density for α = 1 [10,110].…”

Section: Detectability Of Gw Energy Density and Polarizationmentioning

confidence: 99%

“…, and A is a constant that we omit, since we are interested in the spectral shapes, and we will use equations (3.2) and (3.3) to compute the polarization, which does not depend on A. 15 Previous analytical assumptions [62][63][64] consider two types of turbulence:…”

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

“…The inclusion of the subinertial range leads to an increase on polarization at wave numbers right below the peak, which is a more realistic scenario when compared to the numerical results, especially for the case of HK turbulence. The model described above assumes that the partial helicity [62][63][64], and using a broken power law with a Batchelor spectrum in the subinertial range (dotted lines), for fractional helicities h = 0.1, 0.3, 0.5, 0.8, and 1. We use k * = 600 for comparison with the numerical simulations.…”

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

“…We have confirmed using numerical simulations that in the case of an initial magnetic field with a Kolmogorov spectrum for both the magnetic energy density and helicity, the analytical model previously considered in refs. [62][63][64] using HK turbulence gives an accurate prediction of the degree of circular polarization, which gets better when we consider a broken power law. However, when we consider the scenario in which the magnetic field is generated via MHD forcing for a short amount of time, and non-linear interactions appear, allowing to have different spectral slopes at different scales, previous analytical estimates underpredict considerably the polarization degree peak and fail to predict the appropriate shape, which is not given by either the HK nor the HT models, but presents non-linearly combined features of both.…”

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

“…More recently, the two types of spectra have been studied to model the turbulence produced in a first-order EWPT in ref. [64], in the context of detection prospects through LISA by using the dipole modulation induced by the proper motion of the solar system, as proposed in refs. [66,67], and recently applied to LISA in ref.…”

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confidence: 99%

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Polarization of gravitational waves from helical MHD turbulent sources

Pol,

Mandal,

Brandenburg

et al. 2021

Preprint

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We use direct numerical simulations of decaying primordial hydromagnetic turbulence with helicity to compute the resulting gravitational wave (GW) production and its degree of circular polarization. The turbulence is sourced by magnetic fields that are either initially present or driven by an electromotive force applied for a short duration, given as a fraction of one Hubble time. In both types of simulations, we find a clear dependence of the polarization of the resulting GWs on the fractional helicity of the turbulent source. We find a low frequency tail below the spectral peak shallower than the f 3 scaling expected at super-horizon scales, in agreement with similar recent numerical simulations. This type of spectrum facilitates its observational detection with the planned Laser Interferometer Space Antenna (LISA). We show that driven magnetic fields produce GWs more efficiently than magnetic fields that are initially present, leading to larger spectral amplitudes, and to modifications of the spectral shape. In particular, we observe a sharp drop of GW energy above the spectral peak that is in agreement with the previously obtained results. The helicity does not have a huge impact on the maximum spectral amplitude in any of the two types of turbulence considered. However, the GW spectrum at wave numbers away from the peak becomes smaller for larger values of the magnetic fractional helicity. Such variations of the spectrum are most noticeable when magnetic fields are driven. The degree of circular polarization approaches zero at frequencies below the peak, and reaches its maximum at the peak. At higher frequencies, it stays finite if the magnetic field is initially present, and it approaches zero if it is driven. We predict that the spectral peak of the GW signal can be

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Section: Detectability Of Gw Energy Density and Polarizationmentioning

confidence: 99%

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

Section: Comparison To the Analytical Prediction Of The Spectrum Of P...mentioning

confidence: 99%

mentioning

confidence: 99%

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Polarization of gravitational waves from helical MHD turbulent sources

Pol,

Mandal,

Brandenburg

et al. 2021

Preprint

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Dark matter and dark radiation from the early universe with a modulus coupled to the PQMSSM

Baer

Barger

Deal

2023

J. High Energ. Phys.

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The supersymmetrized DFSZ axion model is especially compelling in that it contains 1. the SUSY solution to the gauge hierarchy problem, 2. the Peccei-Quinn (PQ) solution to the strong CP problem and 3. the Kim-Nilles solution to the SUSY μ problem. In a string setting, where a discrete R-symmetry ($$ {\textbf{Z}}_{24}^R $$ Z 24 R for example) may emerge from the compactification process, a high-quality accidental axion (accion) can emerge from the accidental, approximate remnant global U(1)PQ symmetry where the decay constant fa is linked to the SUSY breaking scale, and is within the cosmological sweet zone. In this setup, one also expects the presence of stringy remnant moduli fields ϕi. Here, we consider the situation of a single light modulus ϕ coupled to the PQMSSM in the early universe, with mixed axion plus higgsino-like WIMP dark matter. We evaluate dark matter and dark radiation production via nine coupled Boltzmann equations and assess the severity of the cosmological moduli problem (CMP) along with dark matter and dark radiation production rates. We find that typically the light modulus mass should be mϕ ≳ 104 TeV to avoid the moduli-induced dark matter overproduction problem. If one is able to (anthropically) tune the modulus field amplitude, we find a value of ϕ0 ≲ 10–7mP would be required to solve the overall CMP.

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Sensitivity to dark sector scales from gravitational wave signatures

Dent

Dutta

Ghosh

et al. 2022

J. High Energ. Phys.

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We consider gravitational sound wave signals produced by a first-order phase transition in a theory with a generic renormalizable thermal effective potential of power law form. We find the frequency and amplitude of the gravitational wave signal can be related in a straightforward manner to the parameters of the thermal effective potential. This leads to a general conclusion; if the mass of the dark Higgs is less than 1% of the dark Higgs vacuum expectation value, then the gravitational wave signal will be unobservable at all upcoming and planned gravitational wave observatories. Although the understanding of gravitational wave production at cosmological phase transitions is still evolving, we expect this result to be robust.

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Detecting circular polarisation in the stochastic gravitational-wave background from a first-order cosmological phase transition

Cited by 22 publications

References 129 publications

Polarization of gravitational waves from helical MHD turbulent sources

Polarization of gravitational waves from helical MHD turbulent sources

Dark matter and dark radiation from the early universe with a modulus coupled to the PQMSSM

Sensitivity to dark sector scales from gravitational wave signatures

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