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Large-Scale Primordial Magnetic Fields from Inflation and Preheating

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Ola Tornkvist, Anne-Christine Davis, Konstantinos Dimopoulos, Tomislav Prokopec

Astrophysics · Submitted 14 Nov 2000

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

The authors' main claim With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.

how it is stated · asserted 0.93 read the record →

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arXiv IDastro-ph/0011278 (version 1)
Pith IDOPB3COAR, Pith's permanent record of this paper and its review
CitationAnne-Christine Davis, Konstantinos Dimopoulos, Ola Tornkvist, Tomislav Prokopec. "Large-Scale Primordial Magnetic Fields from Inflation and Preheating." arXiv:astro-ph/0011278 (2000). https://pith.science/paper/OPB3COAR
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,595 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.13 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.62 · compares with prior results 0.07 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. method 0.70 0.31 0.04 asserted 0.72
s1 Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. method 0.68 0.64 0.11 asserted 1.00
s2 The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. result 1.00 0.83 0.14 asserted 0.91
s3 With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields. result 0.53 0.88 0.83 asserted 0.93

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.83.

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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

We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.

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References
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3 arXiv papers cite this in 3 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 · 1 sentence without a confident label

Cites it as background 2 papers
  • Primordial seed fields (which may be amplified later by the dynamo mechanism [ref] ) are generated before structure formation, for instance out of the expansion of the universe, either during inflation [ref] , or in cosmological models with a bounce [ref] .[Cosmological magnetic fields may also be produced during phase transitions, see for instance [ref] , or through the generation of vortical currents [ref] .] However, since minimally-coupled electromagnetism is conformally invariant, the expansion cannot affect its vacuum state.

    Primordial Magnetogenesis in a Bouncing Universe · Introduction · 0.95

  • Primordial seed fields (which may be amplified later by the dynamo mechanism [ref] ) are generated before structure formation, for instance out of the expansion of the universe, either during inflation [ref] , or in cosmological models with a bounce [ref] .[Cosmological magnetic fields may also be produced during phase transitions, see for instance [ref] , or through the generation of vortical currents [ref] .] However, since minimally-coupled electromagnetism is conformally invariant, the expansion cannot affect its vacuum state.

    Quantum Effects in Cosmology · Primordial Magnetogenesis in Bouncing Cosmology · 0.89

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