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Cosmology with a TeV mass GUT Higgs
High Energy Physics - Phenomenology · Submitted 28 Feb 1995
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This can lead to a cosmological history radically different from what is usually assumed to have occurred between the standard inflationary and nucleosynthesis epochs, which may solve the gravitino and Polonyi/moduli problems in a natural way.
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The abstract, sentence by sentence
The most natural way to break the GUT gauge symmetry is with a Higgs field whose vacuum expectation value is of order $10^{16}\,\mbox{GeV}$ but whose mass is of order $10^2$ to $10^3\,\mbox{GeV}$. This can lead to a cosmological history radically different from what is usually assumed to have occurred between the standard inflationary and nucleosynthesis epochs, which may solve the gravitino and Polonyi/moduli problems in a natural way.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The most natural way to break the GUT gauge symmetry is with a Higgs field whose vacuum expectation value is of order $10^{16}\,\mbox{GeV}$ but whose mass is of order $10^2$ to $10^3\,\mbox{GeV}$. | background 0.68 | 0.11 | 0.23 | asserted 0.89 |
| s1 | This can lead to a cosmological history radically different from what is usually assumed to have occurred between the standard inflationary and nucleosynthesis epochs, which may solve the gravitino and Polonyi/moduli problems in a natural way. | interpretation 0.89 | 0.25 | 0.63 | hedged possibility 1.00 |
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The paper
Original abstract
The most natural way to break the GUT gauge symmetry is with a Higgs field whose vacuum expectation value is of order $10^{16}\,\mbox{GeV}$ but whose mass is of order $10^2$ to $10^3\,\mbox{GeV}$. This can lead to a cosmological history radically different from what is usually assumed to have occurred between the standard inflationary and nucleosynthesis epochs, which may solve the gravitino and Polonyi/moduli problems in a natural way.
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References
How later papers used it
61 later papers cite it
1 later paper by other authors is listed below: 1 compared its own results with it.
Compares with it 1 paper
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Said its own matter domination epoch has the same advantages as this paper's thermal inflation, without resorting to yet another scalar field and/or scalar potential.
About a (standard model) universe dominated by the right matter (2008) · 0.91 · paraphrased: the licence does not allow quoting
How the literature uses it
59 arXiv papers cite this in 88 sentences
Papers citing it · 54 sentences without a confident label
Compares with it 1 paper
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In this sense our matter domination epoch has the same advantages as thermal inflation [ref] , without resorting to yet another scalar field and /or scalar potential.
About a (standard model) universe dominated by the right matter · Introduction · 0.91
Cites it as background 29 papers
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The second inflation period is induced by a new field (the so-called flaton) trapped at its origin by coupling with the thermal bath [ref] .
N-body simulations of structure formation in thermal inflation cosmologies · Introduction · 0.84
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In this section, we briefly review the thermal inflation scenario [ref] and introduce density perturbations as a setting for the next sections (for the details, [ref] ). fig:history shows the cosmological history with thermal inflation, and the universe experiences the following four major phases.
Modeling Cosmological Perturbations of Thermal Inflation · Review of Thermal Inflation · 1.00
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Thermal Inflation [ref] is a brief period of inflation (lasting about 10 e-folds) that could have occurred after a period of prior primordial inflation.
Thermal Inflation with a Thermal Waterfall Scalar Field Coupled to a Light Spectator Scalar Field · Thermal Inflation · 0.99
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