Supercooling and phase coexistence in cosmological phase transitions

Alejandro D. Sanchez; Ariel Megevand

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Supercooling and phase coexistence in cosmological phase transitions

Ariel Megevand, Alejandro D. Sanchez

High Energy Physics - Phenomenology · Submitted 6 Dec 2007

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We find thermodynamical constraints on some quantities that determine the dynamics, namely, the latent heat, the radiation energy density and the false-vacuum energy density.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.18 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.09 · compares with prior results 0.05 · mentions code or data availability 0.02.

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Cosmological phase transitions are predicted by Particle Physics models, and have a variety of important cosmological consequences, which depend strongly on the dynamics of the transition. In this work we investigate in detail the general features of the development of a first-order phase transition. We find thermodynamical constraints on some quantities that determine the dynamics, namely, the latent heat, the radiation energy density and the false-vacuum energy density. Using a simple model with a Higgs field, we study numerically the amount and duration of supercooling and the subsequent reheating and phase coexistence. We analyze the dependence of the dynamics on the different parameters of the model, namely, the energy scale, the number of degrees of freedom and the couplings of the scalar field with bosons and fermions. We also inspect the implications for the cosmological outcomes of the phase transition.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Cosmological phase transitions are predicted by Particle Physics models, and have a variety of important cosmological consequences, which depend strongly on the dynamics of the transition.	background 1.00	0.03	0.03	asserted 0.75
s1	In this work we investigate in detail the general features of the development of a first-order phase transition.	contribution 1.00	0.84	0.03	asserted 0.69
s2	We find thermodynamical constraints on some quantities that determine the dynamics, namely, the latent heat, the radiation energy density and the false-vacuum energy density.	result 0.91	0.96	0.21	asserted 1.00
s3	Using a simple model with a Higgs field, we study numerically the amount and duration of supercooling and the subsequent reheating and phase coexistence.	method 0.88	0.96	0.08	asserted 0.97
s4	We analyze the dependence of the dynamics on the different parameters of the model, namely, the energy scale, the number of degrees of freedom and the couplings of the scalar field with bosons and fermions.	contribution 0.73	0.94	0.05	asserted 0.95
s5	We also inspect the implications for the cosmological outcomes of the phase transition.	contribution 0.56	0.90	0.10	unclear 0.70

What kind of paper the classifier reports this is: simulation study 0.99 · evidence from simulation or computation 1.00.

What was examined, and what was not

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arXiv listing abstract v3

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full text
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P abstract

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C citations
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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

Cosmological phase transitions are predicted by Particle Physics models, and have a variety of important cosmological consequences, which depend strongly on the dynamics of the transition. In this work we investigate in detail the general features of the development of a first-order phase transition. We find thermodynamical constraints on some quantities that determine the dynamics, namely, the latent heat, the radiation energy density and the false-vacuum energy density. Using a simple model with a Higgs field, we study numerically the amount and duration of supercooling and the subsequent reheating and phase coexistence. We analyze the dependence of the dynamics on the different parameters of the model, namely, the energy scale, the number of degrees of freedom and the couplings of the scalar field with bosons and fermions. We also inspect the implications for the cosmological outcomes of the phase transition.

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References

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Building a Better Beta: Nucleation and Timescales in Cosmological Phase Transitions
hep-ph 2026-08 conditional novelty 6.0 of 10

A new timescale β_ν, defined as the first moment of the bubble lifetime distribution, avoids pathologies of previous definitions and alters gravitational wave spectra by up to an order of magnitude.
Non-Abelian Dark Forces and the Relic Densities of Dark Glueballs
hep-ph 2016-05 conditional novelty 6.0 of 10

Dark glueballs freeze out through 3-to-2 annihilation, leaving the lightest 0++ state with nearly all the relic density and heavier states suppressed by orders of magnitude, except the C-odd 1+− state, which is small ...
PTagent: An LLM-assisted tool for finite-temperature model construction in cosmological phase transitions
hep-ph 2026-10 conditional novelty 5.5 of 10

PTagent is an LLM-agent framework that turns SARAH files, papers, or DRalgo sources into human-approved finite-temperature potentials for CosmoTransitions and PhaseTracer.

How the literature uses it

20 arXiv papers cite this in 41 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 28 sentences without a confident label

Uses its method or tool 4 papers

We solved Eq. ([ref]) iteratively by the overshoot-undershoot method[See Ref. [ref] for details.].

Detonations and deflagrations in cosmological phase transitions · The Nucleation temperature · 0.89
To obtain temperature corrections one adds to potential temperature dependent parts [ref] : [equation] $δV_T$ stands for standard temperature corrections of first order: [equation] where $n_i$ and $n_j$ are numbers of degrees of freedom of considered boson or fermion particle with field-dependent mass $m_i(ϕ_k)$ and $J_B$ and $J_F$ are thermal bosonic (B) or fermionic (F) functions defined as follows: [equation] [equation] One should also add infrared contributions from higher order diagrams [ref] , which are of the same order as corrections from ([ref]): [equation] which is the so-called ring improvement of the potential and is sufficient for high temperatures, when $(m/T)≪ 1$.

Spontaneous scale symmetry breaking at high temperature · Quantum Field Theory at finite temperature: · 0.82
We will solve Eq. ([ref]) iteratively by the overshoot-undershoot method, and we will integrate Eq. ([ref]), Eq. ([ref]), and the set of Eqs. ([ref])-([ref]) numerically (see Ref. [ref] for details).

Gravitational waves from the electroweak phase transition · Bubble nucleation, expansion and percolation · 0.98

Uses its data or values 1 paper

Numerical results (see, e.g., [ref] ) give values which range from $R_b∼H^-1$ for very strong phase transitions to $R_b∼10^-5 H^-1$ or smaller for weak phase transitions.

Stability of cosmological deflagration fronts · The electroweak phase transition · 0.90

Cites it as support 1 paper

As a consequence, bubble nucleation effectively begins at lower temperatures $T_i$ [ref] .

Gravitational waves from the electroweak phase transition · Extra scalars · 0.98

Cites it as background 7 papers

The dilution of thermal relic abundance of DM due to FOPT has been studied in the past by considering some toy-model-like effective potential such as adding a larger degree of freedom from the hidden sector [ref] .

Dilution of Dark Matter Relic abundance due to First Order Electroweak Phase Transition · Introduction · 0.82
In a first-order cosmological phase transition, bubbles nucleate and expand, converting the high-temperature phase into the low-temperature one (see, e.g., [ref] ).

Analytic approach to the motion of cosmological phase transition fronts · Introduction · 1.00
The nature of cosmological phase transition is addressed in [ref] .

Scalar Representations in the Light of Electroweak Phase Transition and Cold Dark Matter Phenomenology · Impact of Multiplets' Sizes on EWPhT · 0.95

What it cites · 33 sentences without a confident label

Compares with 2 papers

Our results for the distance $d$ agree in order of magnitude with those of Refs. [ref] .

The Effects of Electro-weak Phase Transition Dynamics on Baryogenesis and Primordial Nucleosynthesis · Electroweak baryogenesis and baryon inhomogeneities · 1.00
We solved Eq. ([ref]) iteratively by the overshoot-undershoot method[We have checked our program by comparing with the results of Ref. [ref] for the bounce and Ref. [ref] for the evolution of the phase transition.].

Towards the Theory of Cosmological Phase Transitions · Phase transition dynamics · 0.99

Cites as background 10 papers

The nucleation and growth of bubbles in a first order phase transition has been extensively studied (see e.g. [ref] ).

The Effects of Electro-weak Phase Transition Dynamics on Baryogenesis and Primordial Nucleosynthesis · Phase transition dynamics · 1.00
The nucleation and growth of bubbles in a first order phase transition has been extensively studied (see e.g. [ref] ).

Dynamical evolution of the Universe in the quark-hadron phase transition and possible nugget formation · Phase transition dynamics · 1.00
The nucleation and growth of bubbles in a first order phase transition has been extensively studied (see e.g. [ref] ).

Towards the Theory of Cosmological Phase Transitions · Phase transition dynamics · 1.00

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