Spectrum of gravitational radiation from primordial turbulence

Gogoberidze, G.; Kahniashvili, Tina; Kosowsky, Arthur

doi:10.1103/physrevd.76.083002

Cited by 195 publications

(245 citation statements)

References 68 publications

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“…More recent works have addressed various possibilities for early-universe physics leading to detectable cosmological gravitational wave backgrounds and have analyzed in more detail the turbulent spectrum as well as the spectrum of the gravitational wave signal [15][16][17][18][19][20][21]. However, to the best of our knowledge, there are no studies of turbulence at the QCD epoch assuming a crossover transition and employing a realistic lattice QCD equation of state (EoS) for the primordial fluid.…”

Section: Introductionmentioning

confidence: 99%

Unveiling the cosmological QCD phase transition through the eLISA/NGO detector

Roque

Lugones

2013

Phys. Rev. D

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We study the evolution of turbulence in the early universe at the QCD epoch using a state-ofthe-art equation of state derived from lattice QCD simulations. Since the transition is a crossover we assume that temperature and velocity fluctuations were generated by some event in the previous history of the Universe and survive until the QCD epoch due to the extremely large Reynolds number of the primordial fluid. The fluid at the QCD epoch is assumed to be non-viscous, based on the fact that the viscosity per entropy density of the quark gluon plasma obtained from heavy-ion collision experiments at the RHIC and the LHC is extremely small. Our hydrodynamic simulations show that the velocity spectrum is very different from the Kolmogorov power law considered in studies of primordial turbulence that focus on first order phase transitions. This is due to the fact that there is no continuous injection of energy in the system and the viscosity of the fluid is negligible. Thus, as kinetic energy cascades from the larger to the smaller scales, a large amount of kinetic energy is accumulated at the smallest scales due to the lack of dissipation. We have obtained the spectrum of the gravitational radiation emitted by the motion of the fluid finding that, if typical velocity and temperature fluctuations have an amplitude (∆v)/c 10 −2 and/or ∆T /Tc 10 −3 , they would be detected by eLISA at frequencies larger than ∼ 10 −4 Hz.PACS numbers: 98.80. Cq, 95.85.Sz, 25.75.Nq, 12.38.Gc,

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Section: Introductionmentioning

confidence: 99%

Unveiling the cosmological QCD phase transition through the eLISA/NGO detector

Roque

Lugones

2013

Phys. Rev. D

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“…There should also be a contribution to the GW spectra from the turbulence immediately following the bubble collisions (instead of from the collisions themselves), and this contribution may be quite large [53,54]. However, this still requires a strongly first-order phase transition and will therefore contain gauge artifacts similar to those in the simpler calculation.…”

Section: Calculating Gw Spectramentioning

confidence: 99%

Gravity waves from a cosmological phase transition: Gauge artifacts and daisy resummations

2011

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The finite-temperature effective potential customarily employed to describe the physics of cosmological phase transitions often relies on specific gauge choices, and is manifestly not gauge-invariant at finite order in its perturbative expansion. As a result, quantities relevant for the calculation of the spectrum of stochastic gravity waves resulting from bubble collisions in first-order phase transitions are also not gauge-invariant. We assess the quantitative impact of this gauge-dependence on key quantities entering predictions for gravity waves from first order cosmological phase transitions. We resort to a simple abelian Higgs model, and discuss the case of R ξ gauges. By comparing with results obtained using a gauge-invariant Hamiltonian formalism, we show that the choice of gauge can have a dramatic effect on theoretical predictions for the normalization and shape of the expected gravity wave spectrum. We also analyze the impact of resumming higher-order contributions as needed to maintain the validity of the perturbative expansion, and show that doing so can suppress the amplitude of the spectrum by an order of magnitude or more. We comment on open issues and possible strategies for carrying out "daisy resummed" gauge invariant computations in non-Abelian models for which a gauge-invariant Hamiltonian formalism is not presently available.

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“…refs. [1,4,[55][56][57][58][59][60][61][62][63][64][65][66][67][68]). These scenarios may be effectively probed by upcoming gravitational wave experiments, such as eLISA [69], or Big Bang Observer [70].…”

Section: Jhep10(2015)135mentioning

confidence: 99%

Bubble expansion and the viability of singlet-driven electroweak baryogenesis

Kozaczuk

2015

J. High Energ. Phys.

139

146

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The standard picture of electroweak baryogenesis requires slowly expanding bubbles. This can be difficult to achieve if the vacuum expectation value (VEV) of a gauge singlet scalar field changes appreciably during the electroweak phase transition. It is important to determine the bubble wall velocity in this case, since the predicted baryon asymmetry can depend sensitively on its value. Here, this calculation is discussed and illustrated in the real singlet extension of the Standard Model. The friction on the bubble wall is computed using a kinetic theory approach and including hydrodynamic effects. Wall velocities are found to be rather large (v w 0.2) but compatible with electroweak baryogenesis in some portions of the parameter space. If the phase transition is strong enough, however, a subsonic solution may not exist, precluding non-local electroweak baryogenesis altogether. The results presented here can be used in calculating the baryon asymmetry in various singlet-driven scenarios, as well as other features related to cosmological phase transitions in the early Universe, such as the resulting spectrum of gravitational radiation.

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Spectrum of gravitational radiation from primordial turbulence

Cited by 195 publications

References 68 publications

Unveiling the cosmological QCD phase transition through the eLISA/NGO detector

Unveiling the cosmological QCD phase transition through the eLISA/NGO detector

Gravity waves from a cosmological phase transition: Gauge artifacts and daisy resummations

Bubble expansion and the viability of singlet-driven electroweak baryogenesis

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