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Journal articles on the topic 'Cosmological phase transitions'

Author: Grafiati

Published: 30 November 2024

Last updated: 31 July 2025

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1

KIM, SANG PYO. "DYNAMICAL THEORY OF PHASE TRANSITIONS AND COSMOLOGICAL EW AND QCD PHASE TRANSITIONS." Modern Physics Letters A 23, no. 17n20 (2008): 1325–35. http://dx.doi.org/10.1142/s0217732308027692.

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We critically review the cosmological EW and QCD phase transitions. The EW and QCD phase transitions would have proceeded dynamically since the expansion of the universe determines the quench rate and critical behaviors at the onset of phase transition slow down the phase transition. We introduce a real-time quench model for dynamical phase transitions and describe the evolution using a canonical real-time formalism. We find the correlation function, the correlation length and time and then discuss the cosmological implications of dynamical phase transitions on EW and QCD phase transitions in

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2

Athron, Peter, Csaba Balázs, and Lachlan Morris. "Supercool subtleties of cosmological phase transitions." Journal of Cosmology and Astroparticle Physics 2023, no. 03 (2023): 006. http://dx.doi.org/10.1088/1475-7516/2023/03/006.

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Abstract We investigate rarely explored details of supercooled cosmological first-order phase transitions at the electroweak scale, which may lead to strong gravitational wave signals or explain the cosmic baryon asymmetry. The nucleation temperature is often used in phase transition analyses, and is defined through the nucleation condition: on average one bubble has nucleated per Hubble volume. We argue that the nucleation temperature is neither a fundamental nor essential quantity in phase transition analysis. We illustrate scenarios where a transition can complete without satisfying the nuc

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3

Buckley, Matthew R., Peizhi Du, Nicolas Fernandez, and Mitchell J. Weikert. "Dark radiation isocurvature from cosmological phase transitions." Journal of Cosmology and Astroparticle Physics 2024, no. 07 (2024): 031. http://dx.doi.org/10.1088/1475-7516/2024/07/031.

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Abstract Cosmological first order phase transitions are typically associated with physics beyond the Standard Model, and thus of great theoretical and observational interest. Models of phase transitions where the energy is mostly converted to dark radiation can be constrained through limits on the dark radiation energy density (parameterized by ΔN eff). However, the current constraint (ΔN eff < 0.3) assumes the perturbations are adiabatic. We point out that a broad class of non-thermal first order phase transitions that start during inflation but do not complete until after reheating leave

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4

Hogan, C. J. "Gravitational radiation from cosmological phase transitions." Monthly Notices of the Royal Astronomical Society 218, no. 4 (1986): 629–36. http://dx.doi.org/10.1093/mnras/218.4.629.

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5

MÉGEVAND, ARIEL. "GRAVITATIONAL WAVES FROM COSMOLOGICAL PHASE TRANSITIONS." International Journal of Modern Physics A 24, no. 08n09 (2009): 1541–44. http://dx.doi.org/10.1142/s0217751x09044966.

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6

Kurki-Suonio, H., and M. Laine. "Supersonic deflagrations in cosmological phase transitions." Physical Review D 51, no. 10 (1995): 5431–37. http://dx.doi.org/10.1103/physrevd.51.5431.

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7

Vachaspati, Tanmay. "Magnetic fields from cosmological phase transitions." Physics Letters B 265, no. 3-4 (1991): 258–61. http://dx.doi.org/10.1016/0370-2693(91)90051-q.

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8

Durrer, Ruth. "Gravitational waves from cosmological phase transitions." Journal of Physics: Conference Series 222 (April 1, 2010): 012021. http://dx.doi.org/10.1088/1742-6596/222/1/012021.

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9

Athron, Peter, Lachlan Morris, and Zhongxiu Xu. "How robust are gravitational wave predictions from cosmological phase transitions?" Journal of Cosmology and Astroparticle Physics 2024, no. 05 (2024): 075. http://dx.doi.org/10.1088/1475-7516/2024/05/075.

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Abstract Gravitational wave (GW) predictions of cosmological phase transitions are almost invariably evaluated at either the nucleation or percolation temperature. We investigate the effect of the transition temperature choice on GW predictions, for phase transitions with weak, intermediate and strong supercooling. We find that the peak amplitude of the GW signal varies by a factor of a few for weakly supercooled phase transitions, and by an order of magnitude for strongly supercooled phase transitions. The variation in amplitude for even weakly supercooled phase transitions can be several ord

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10

Jinno, Ryusuke, Thomas Konstandin, Henrique Rubira, and Isak Stomberg. "Higgsless simulations of cosmological phase transitions and gravitational waves." Journal of Cosmology and Astroparticle Physics 2023, no. 02 (2023): 011. http://dx.doi.org/10.1088/1475-7516/2023/02/011.

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Abstract First-order cosmological phase transitions in the early Universe source sound waves and, subsequently, a background of stochastic gravitational waves. Currently, predictions of these gravitational waves rely heavily on simulations of a Higgs field coupled to the plasma of the early Universe, the former providing the latent heat of the phase transition. Numerically, this is a rather demanding task since several length scales enter the dynamics. From smallest to largest, these are the thickness of the Higgs interface separating the different phases, the shell thickness of the sound wave

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11

JANSEN, KARL. "COSMOLOGICAL PHASE TRANSITIONS FROM LATTICE FIELD THEORY." International Journal of Modern Physics E 20, supp02 (2011): 71–77. http://dx.doi.org/10.1142/s0218301311040621.

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In this proceedings contribution we discuss the fate of the electroweak and the quantum chromodynamics phase transitions relevant for the early stage of the universe at non-zero temperature. These phase transitions are related to the Higgs mechanism and the breaking of chiral symmetry, respectively. We will review that non-perturbative lattice field theory simulations show that these phase transitions actually do not occur in nature and that physical observables show a completely smooth behaviour as a function of the temperature.

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12

Strumia, Alessandro, and Nikolaos Tetradis. "Bubble-nucleation rates for cosmological phase transitions." Journal of High Energy Physics 1999, no. 11 (1999): 023. http://dx.doi.org/10.1088/1126-6708/1999/11/023.

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13

Mégevand, Ariel, and Alejandro D. Sánchez. "Detonations and deflagrations in cosmological phase transitions." Nuclear Physics B 820, no. 1-2 (2009): 47–74. http://dx.doi.org/10.1016/j.nuclphysb.2009.05.007.

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14

Gleiser, Marcelo, and Edward W. Kolb. "Dynamics of cosmological phase transitions: Metastability revisited." Vistas in Astronomy 37 (January 1993): 429–32. http://dx.doi.org/10.1016/0083-6656(93)90068-u.

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15

Ignatius, J., K. Kajantie, H. Kurki-Suonio, and M. Laine. "Growth of bubbles in cosmological phase transitions." Physical Review D 49, no. 8 (1994): 3854–68. http://dx.doi.org/10.1103/physrevd.49.3854.

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16

Ignatius, J. "Bubble free energy in cosmological phase transitions." Physics Letters B 309, no. 3-4 (1993): 252–57. http://dx.doi.org/10.1016/0370-2693(93)90929-c.

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17

Vachaspati, Tanmay. "Magnetic fields in the aftermath of phase transitions." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 366, no. 1877 (2008): 2915–23. http://dx.doi.org/10.1098/rsta.2008.0074.

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The COSLAB effort has focused on the formation of topological defects during phase transitions. Yet there is another potentially interesting signature of cosmological phase transitions, which also deserves study in the laboratory. This is the generation of magnetic fields during phase transitions. In particular, cosmological phase transitions that also lead to preferential production of matter over antimatter (‘baryogenesis’) are expected to produce helical (left-handed) magnetic fields. The study of analogous processes in the laboratory can yield important insight into the production of helic

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18

Branchina, Carlo, Angela Conaci, Stefania De Curtis, et al. "New calculation of collision integrals for cosmological phase transitions." EPJ Web of Conferences 314 (2024): 00031. https://doi.org/10.1051/epjconf/202431400031.

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First order phase transitions in the early universe may have left a variety of experimentally accessible imprints. The dynamics of such transitions is governed by the density perturbations caused by the propagation of the bubble wall in the false vacuum plasma, conveniently described by a Boltzmann equation. The determination of the bubble wall expansion velocity is crucial to determine the experimental signatures of the transition. We report on the first full (numerical) solution to the Boltzmann equation. Differently from traditional ones, our approach does not rely on any ansatz. The result

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19

Ghodmare, S. G., and K. P. Pande. "Phase Transitions and Asymptotic Behaviors in (2+1)-Dimensional Spacetimes with Perfect Fluids and Cosmological Constant." Indian Journal Of Science And Technology 18, no. 24 (2025): 1908–14. https://doi.org/10.17485/ijst/v18i24.797.

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Objectives: The study first examines the (2+1)-dimensional cosmic holographic principle with 𝑝 = 𝜔𝜌 + Λ, then studies cosmological solutions for this modified equation of state. Method: We analyze a (2+1)-dimensional holographic cosmology with the modified Eos 𝑝 = 𝜔𝜌 + Λ (Λ = 𝛼𝜌), resolving hydrodynamic instabilities in dark/phantom energy. By exploring free parameter space (𝜔, 𝛼), we derive cosmological solutions, identifying three dynamical regimes. Analytical and numerical methods reveal late-time acceleration, bouncing/cyclic universes, and stability criteria. The study connects EoS parame

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20

Giombi, L., and Mark Hindmarsh. "General relativistic bubble growth in cosmological phase transitions." Journal of Cosmology and Astroparticle Physics 2024, no. 03 (2024): 059. http://dx.doi.org/10.1088/1475-7516/2024/03/059.

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Abstract We use a full general relativistic framework to study the self-similar expansion of bubbles of the stable phase into a flat Friedmann-Lemaître-Robertson-Walker Universe in a first order phase transition in the early Universe. With a simple linear barotropic equation of state in both phases, and in the limit of a phase boundary of negligible width, we find that self-similar solutions exist, which are qualitatively similar to the analogous solutions in Minkowski space, but with distinguishing features. Rarefaction waves extend to the centre of the bubble, while spatial sections near the

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21

Kisslinger, Leonard S. "Cosmological Phase Transitions—EWPT-QCDPT: Magnetic Field Creation." Magnetochemistry 8, no. 10 (2022): 115. http://dx.doi.org/10.3390/magnetochemistry8100115.

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We review the cosmic microwave background (CMBR) estimate of ordinary matter, dark matter and dark energy in the universe. Then, we review the cosmological electroweak (EWPT) and quantum chromodynamics (QCDPT) phase transitions. During both the EWPT and QCDPT, bubbles form and collide, producing magnetic fields. We review dark matter produced during the EWPT and the estimate of dark matter via galaxy rotation.

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22

Kosowsky, Arthur, Michael S. Turner, and Richard Watkins. "Gravitational waves from first-order cosmological phase transitions." Physical Review Letters 69, no. 14 (1992): 2026–29. http://dx.doi.org/10.1103/physrevlett.69.2026.

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23

Lange, David, Marc Sher, Joel Sivillo, and Robert Welsh. "A hand‐held demonstration of cosmological phase transitions." American Journal of Physics 61, no. 11 (1993): 1049–50. http://dx.doi.org/10.1119/1.17339.

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24

Espinosa, José R., Thomas Konstandin, José M. No, and Géraldine Servant. "Energy budget of cosmological first-order phase transitions." Journal of Cosmology and Astroparticle Physics 2010, no. 06 (2010): 028. http://dx.doi.org/10.1088/1475-7516/2010/06/028.

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25

Zaripov, Farkhat. "Oscillating Cosmological Solutions in the Modified Theory of Induced Gravity." Advances in Astronomy 2019 (April 24, 2019): 1–15. http://dx.doi.org/10.1155/2019/1502453.

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This work is the extension of author’s research, where the modified theory of induced gravity (MTIG) is proposed. In the framework of the MTIG, the mechanism of phase transitions and the description of multiphase behavior of the cosmological scenario are proposed. The theory describes two systems (stages): Einstein (ES) and “restructuring” (RS). This process resembles the phenomenon of a phase transition, where different phases (Einstein’s gravitational systems, but with different constants) pass into each other. The hypothesis that such transitions are random and lead to stochastic behavior o

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26

JOHNSON, MIKKEL B., L. S. KISSLINGER, E. M. HENLEY, W.-Y. P. HWANG, and T. STEVENS. "NON-ABELIAN DYNAMICS IN FIRST-ORDER COSMOLOGICAL PHASE TRANSITIONS." Modern Physics Letters A 19, no. 13n16 (2004): 1187–94. http://dx.doi.org/10.1142/s0217732304014549.

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Bubble collisions in cosmological phase transitions are explored, taking the non-abelian character of the gauge fields into account. Both the QCD and electroweak phase transitions are considered. Numerical solutions of the field equations in several limits are presented.

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27

Mielczarek, Jakub. "Big Bang as a Critical Point." Advances in High Energy Physics 2017 (2017): 1–5. http://dx.doi.org/10.1155/2017/4015145.

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This article addresses the issue of possible gravitational phase transitions in the early universe. We suggest that a second-order phase transition observed in the Causal Dynamical Triangulations approach to quantum gravity may have a cosmological relevance. The phase transition interpolates between a nongeometric crumpled phase of gravity and an extended phase with classical properties. Transition of this kind has been postulated earlier in the context of geometrogenesis in the Quantum Graphity approach to quantum gravity. We show that critical behavior may also be associated with a signature

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28

KIM, WONTAE, and EDWIN J. SON. "TWO NONCOMMUTATIVE PARAMETERS AND REGULAR COSMOLOGICAL PHASE TRANSITION IN THE SEMICLASSICAL DILATON COSMOLOGY." Modern Physics Letters A 23, no. 15 (2008): 1079–91. http://dx.doi.org/10.1142/s0217732308027047.

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We study cosmological phase transitions from modified equations of motion by introducing two noncommutative parameters in the Poisson brackets, which describes the initial- and future-singularity-free phase transition in the soluble semiclassical dilaton gravity with a nonvanishing cosmological constant. Accelerated expansion and decelerated expansion appear alternatively, where the model contains the second accelerated expansion. The final stage of the universe approaches the flat spacetime independent of the initial state of the curvature scalar as long as the product of the two noncommutati

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29

Saslaw, William C., and Farooq Ahmad. "GRAVITATIONAL PHASE TRANSITIONS IN THE COSMOLOGICAL MANY-BODY SYSTEM." Astrophysical Journal 720, no. 2 (2010): 1246–53. http://dx.doi.org/10.1088/0004-637x/720/2/1246.

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30

Kurki-Suonio, H., and M. Laine. "Bubble growth and droplet decay in cosmological phase transitions." Physical Review D 54, no. 12 (1996): 7163–71. http://dx.doi.org/10.1103/physrevd.54.7163.

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31

Sigl, Günter, Angela V. Olinto, and Karsten Jedamzik. "Primordial magnetic fields from cosmological first order phase transitions." Physical Review D 55, no. 8 (1997): 4582–90. http://dx.doi.org/10.1103/physrevd.55.4582.

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32

Mégevand, Ariel, and Santiago Ramírez. "Bubble nucleation and growth in slow cosmological phase transitions." Nuclear Physics B 928 (March 2018): 38–71. http://dx.doi.org/10.1016/j.nuclphysb.2018.01.012.

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33

Dienes, Keith R., E. Dudas, T. Gherghetta, and A. Riotto. "Cosmological phase transitions and radius stabilization in higher dimensions." Nuclear Physics B 543, no. 1-2 (1999): 387–422. http://dx.doi.org/10.1016/s0550-3213(98)00855-4.

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34

Leitao, Leonardo, and Ariel Mégevand. "Spherical and non-spherical bubbles in cosmological phase transitions." Nuclear Physics B 844, no. 3 (2011): 450–70. http://dx.doi.org/10.1016/j.nuclphysb.2010.11.012.

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35

Gleiser, Marcelo, and Mark Trodden. "Weakly first order cosmological phase transitions and fermion production." Physics Letters B 517, no. 1-2 (2001): 7–12. http://dx.doi.org/10.1016/s0370-2693(01)00974-1.

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36

HWANG, W.-Y. P. "SOME THOUGHTS ON THE COSMOLOGICAL QCD PHASE TRANSITION." International Journal of Modern Physics A 23, no. 30 (2008): 4757–77. http://dx.doi.org/10.1142/s0217751x08042845.

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The cosmological QCD phase transitions may have taken place between 10-5 s and 10-4 s in the early universe offers us one of the most intriguing and fascinating questions in cosmology. In bag models, the phase transition is described by the first-order phase transition and the role played by the latent "heat" or energy released in the transition is highly nontrivial and is being classified as the first-order phase transition. In this presentation, we assume, first of all, that the cosmological QCD phase transition, which happened at a time between 10-5 s and 10-4 s or at the temperature of abo

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37

RAYCHAUDHURI, B., F. RAHAMAN, and M. KALAM. "ON TOPOLOGICAL DEFECTS AND COSMOLOGICAL CONSTANT." Modern Physics Letters A 29, no. 01 (2014): 1450007. http://dx.doi.org/10.1142/s0217732314500072.

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Einstein introduced cosmological constant in his field equations in an ad hoc manner. Cosmological constant plays the role of vacuum energy of the universe which is responsible for the accelerating expansion of the universe. To give a theoretical support, it remains an elusive goal to modern physicists. We provide a prescription to obtain cosmological constant from the phase transitions of the early universe when topological defects, namely monopole might have existed.

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38

Bécar, Ramón, P. A. González, Joel Saavedra, Yerko Vásquez, and Bin Wang. "Phase transitions in four-dimensional AdS black holes with a nonlinear electrodynamics source." Communications in Theoretical Physics 73, no. 12 (2021): 125402. http://dx.doi.org/10.1088/1572-9494/ac3073.

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Abstract In this work we consider black hole solutions to Einstein’s theory coupled to a nonlinear power-law electromagnetic field with a fixed exponent value. We study the extended phase space thermodynamics in canonical and grand canonical ensembles, where the varying cosmological constant plays the role of an effective thermodynamic pressure. We examine thermodynamical phase transitions in such black holes and find that both first- and second-order phase transitions can occur in the canonical ensemble while, for the grand canonical ensemble, Hawking–Page and second-order phase transitions a

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39

Zou, De-Cheng, Ming Zhang, Chao Wu, and Rui-Hong Yue. "Critical Phenomena of Charged AdS Black Holes in Rastall Gravity." Advances in High Energy Physics 2020 (January 24, 2020): 1–9. http://dx.doi.org/10.1155/2020/4065254.

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We construct analytical charged anti-de Sitter (AdS) black holes surrounded by perfect fluids in four dimensional Rastall gravity. Then, we discuss the thermodynamics and phase transitions of charged AdS black holes immersed in regular matter like dust and radiation, or exotic matter like quintessence, ΛCDM type, and phantom fields. Surrounded by phantom field, the charged AdS black hole demonstrates a new phenomenon of reentrant phase transition (RPT) when the parameters Q, Np, and ψ satisfy some certain condition, along with the usual small/large black hole (SBH/LBH) phase transition for the

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40

Jinno, Ryusuke, and Jun'ya Kume. "Gravitational effects on fluid dynamics in cosmological first-order phase transitions." Journal of Cosmology and Astroparticle Physics 2025, no. 02 (2025): 057. https://doi.org/10.1088/1475-7516/2025/02/057.

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Abstract Cosmological first-order phase transition (FOPT) sources the stochastic gravitational wave background (SWGB) through bubble collisions, sound waves, and turbulence. So far, most studies on the fluid profile of an expanding bubble are limited to transitions that complete in a much shorter time scale than the cosmic expansion. In this study, we investigate gravitational effects on the fluid profile beyond the self-similar regime. For this purpose we combine a hydrodynamic scheme in the presence of gravity with a fluid computation scheme under energy injection from the bubble wall. By pe

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41

Zhang, Ming, De-Cheng Zou, and Rui-Hong Yue. "Reentrant Phase Transitions and Triple Points of Topological AdS Black Holes in Born-Infeld-Massive Gravity." Advances in High Energy Physics 2017 (2017): 1–11. http://dx.doi.org/10.1155/2017/3819246.

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Motivated by recent developments of black hole thermodynamics in de Rham, Gabadadze, and Tolley (dRGT) massive gravity, we study the critical behaviors of topological Anti-de Sitter (AdS) black holes in the presence of Born-Infeld nonlinear electrodynamics. Here the cosmological constant appears as a dynamical pressure of the system and its corresponding conjugate quantity is interpreted as thermodynamic volume. This shows that, besides the Van der Waals-like SBH/LBH phase transitions, the so-called reentrant phase transition (RPT) appears in four-dimensional space-time when the coupling coeff

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42

Sigl, Günter. "Cosmological gravitational wave background from phase transitions in neutron stars." Journal of Cosmology and Astroparticle Physics 2006, no. 04 (2006): 002. http://dx.doi.org/10.1088/1475-7516/2006/04/002.

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43

Mégevand, Ariel, and Santiago Ramírez. "Bubble nucleation and growth in very strong cosmological phase transitions." Nuclear Physics B 919 (June 2017): 74–109. http://dx.doi.org/10.1016/j.nuclphysb.2017.03.009.

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44

Housset, Joaquín, Joel F. Saavedra, and Francisco Tello-Ortiz. "Cosmological FLRW phase transitions and micro-structure under Kaniadakis statistics." Physics Letters B 853 (June 2024): 138686. http://dx.doi.org/10.1016/j.physletb.2024.138686.

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45

Ma, Yubo, Yang Zhang, Ren Zhao, et al. "Phase transitions and entropy force of charged de Sitter black holes with cloud of string and quintessence." International Journal of Modern Physics D 29, no. 15 (2020): 2050108. http://dx.doi.org/10.1142/s0218271820501084.

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In this paper, we investigate the combined effects of the cloud of strings and quintessence on the thermodynamics of a Reissner–Nordström–de Sitter black hole. Based on the equivalent thermodynamic quantities considering the correlation between the black hole horizon and the cosmological horizon, we extensively discuss the phase transitions of the spacetime. Our analysis proves that similar to the case in AdS spacetime, second-order phase transitions could take place under certain conditions, with the absence of first-order phase transition in the charged de Sitter (dS) black holes with cloud

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46

Kurbashev, B., and G. Aliasqarova. "ON SYMMETRY CHANGES DURING PHASE TRANSITIONS IN THE EARLY HOT UNIVERSE AND CRYSTALLINE SOLIDS." MODERN SCIENCE AND RESEARCH 3, no. 4 (2024): 1267–69. https://doi.org/10.5281/zenodo.11090952.

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<em>The results of a comparative analysis of phase transitions that occur in the early hot Universe and various crystalline substances are presented. It is assumed that the principle of preserving macroscopic symmetry should take place in all types of phase transitions. It is shown that many cosmological and crystallographic problems can be solved on the basis of the principle of macroscopic conservation.</em>

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47

Chabab, M., H. El Moumni, S. Iraoui, K. Masmar, and S. Zhizeh. "More insight into microscopic properties of RN-AdS black hole surrounded by quintessence via an alternative extended phase space." International Journal of Geometric Methods in Modern Physics 15, no. 10 (2018): 1850171. http://dx.doi.org/10.1142/s0219887818501712.

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In this work, we study the phase transition of the charged-AdS black hole surrounded by quintessence via an alternative extended phase space defined by the charge square [Formula: see text] and her conjugate [Formula: see text], a quantity proportional to the inverse of horizon radius, while the cosmological constant is kept fixed. The equation of state is derived under the form [Formula: see text] and the critical behavior of such black hole analyzed. In addition, we examine the role of the quintessence parameter and its effects on phase transitions. Besides that, we explore the connection be

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48

Lev, B. I., and A. G. Zagorodny. "Some peculiarities of noise-induced phase transition." Low Temperature Physics 48, no. 11 (2022): 949–55. http://dx.doi.org/10.1063/10.0014595.

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Two fundamental evolutionary principles, namely the H-theorem and the least-energy principle, are applied to describe the phase transition in condensed environments and cosmological models. We assume that in the presence of a spontaneously induced scalar field, which can be treated as an order parameter, the energy of the ground state is lower than the ground state energy without such a field. Taking into account the self-consistent interaction of the scalar field with the fluctuations of the fields of other nature and the principles mentioned above, it is possible to show the possibility of t

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49

BURDYUZHA, V. V., Yu N. PONOMAREV, O. D. LALAKULICH, and G. M. VERESHKOV. "THE TUNNELING, THE SECOND ORDER RELATIVISTIC PHASE TRANSITIONS AND PROBLEM OF THE MACROSCOPIC UNIVERSE ORIGIN." International Journal of Modern Physics D 05, no. 03 (1996): 273–92. http://dx.doi.org/10.1142/s0218271896000199.

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We propose that the Universe was created from “Nothing” with a relatively small number of particles and it very quick relaxed to a quasi-equilibrium state at the Planck parameters. The classic cosmological solution for this Universe, with the calculation of its ability to undergo the second order relativistic phase transition (RPT), has two branches divided by a gap. On one of these branches near to the “Nothing” state the second order RPT is not possible at the GUT scale. The other branch is thermodynamically unstable. The quantum process of tunneling between the cosmological solution branche

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50

Peter, Niksa, Schlederer Martin, and Sigl Günter. "Gravitational waves produced by compressible MHD turbulence from cosmological phase transitions." Classical and Quantum Gravity 35, no. 14 (2018): 144001. http://dx.doi.org/10.1088/1361-6382/aac89c.

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