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Quantum Cosmological Correlations in an Inflating Universe: Can fermion and gauge fields loops give a scale free spectrum?
High Energy Physics - Theory · Submitted 30 Nov 2006
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim It is shown here that departures from scale invariance are never large even when Dirac, vector, and conformal scalar fields are present \emph{during} inflation.
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The abstract, sentence by sentence
This paper extends the calculation of quantum corrections to the cosmological correlation $<\zeta\zeta>$, which has been done by Weinberg for a loop of minimally coupled scalars, to other types of matter loops and a general and realistic potential. It is shown here that departures from scale invariance are never large even when Dirac, vector, and conformal scalar fields are present \emph{during} inflation. No fine tuning is needed, in the sense that effective masses or coupling constants can have arbitrary values. Even when the mass is as large as $M_{Pl}$, the one-loop result is still naturally smaller than the classical one. Thus, the results show that the existence of these fields \emph{during} inflation may not be ruled out and is consistent with natural reheating.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | This paper extends the calculation of quantum corrections to the cosmological correlation $<\zeta\zeta>$, which has been done by Weinberg for a loop of minimally coupled scalars, to other types of matter loops and a general and realistic potential. | contribution 0.93 | 0.70 | 0.06 | asserted 0.96 |
| s1 | It is shown here that departures from scale invariance are never large even when Dirac, vector, and conformal scalar fields are present \emph{during} inflation. | result 1.00 | 0.93 | 0.72 | asserted 1.00 |
| s2 | No fine tuning is needed, in the sense that effective masses or coupling constants can have arbitrary values. | result 0.81 | 0.81 | 0.16 | asserted 1.00 |
| s3 | Even when the mass is as large as $M_{Pl}$, the one-loop result is still naturally smaller than the classical one. | result 1.00 | 0.91 | 0.10 | asserted 1.00 |
| s4 | Thus, the results show that the existence of these fields \emph{during} inflation may not be ruled out and is consistent with natural reheating. | interpretation 1.00 | 0.80 | 0.40 | hedged possibility 0.99 |
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The paper
Original abstract
This paper extends the calculation of quantum corrections to the cosmological correlation $<\zeta\zeta>$, which has been done by Weinberg for a loop of minimally coupled scalars, to other types of matter loops and a general and realistic potential. It is shown here that departures from scale invariance are never large even when Dirac, vector, and conformal scalar fields are present \emph{during} inflation. No fine tuning is needed, in the sense that effective masses or coupling constants can have arbitrary values. Even when the mass is as large as $M_{Pl}$, the one-loop result is still naturally smaller than the classical one. Thus, the results show that the existence of these fields \emph{during} inflation may not be ruled out and is consistent with natural reheating.
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References
How the literature uses it
12 arXiv papers cite this in 22 sentences
Papers citing it · 13 sentences without a confident label
Contests it 3 papers
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However, it was pointed out in [ref] that there were mistakes in the computation, since the loop correction computed in [ref] and subsequent related studies [ref] have a $log(k/ μ)$ dependence.
Bispectrum at 1-loop in the Effective Field Theory of Inflation · Introduction · contest 0.87
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Summarizing: in the calculation performed in dimensional regularization the effect of considering the terms proportional to $δ$ in the measure and in the wavefunction has achieved the result of transforming the logarithmic divergency $log(k/μ)$ found in the literature [ref] into log(k/μ)+log(-Hη_k )∼log(H/μ) , where we have used that $k η_k ∼-1$.
On Loops in Inflation · $∙$ Remaining $δ-$components · contest 0.83
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Some earlier analyses using dimensional regularization did not properly take this effect into account (e.g. [ref] ), leading to incorrect results that violated the dilatation symmetry.] [equation] Although for the purpose we are interested in (i.e. obtaining the one-loop power spectrum of tensor modes at zeroth order in $ϵ$) this differential problem can be solved exactly, in more complicated situations this may not be the case.
Finite parts of inflationary loops · Tensor power spectrum in slow-roll inflation at one loop · contest 0.86
Cites it as background 4 papers
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The possibility of an infrared perturbative breakdown was explored by Sasaki, Suzuki, Yamamoto & Yokoyama [ref] , and later authors computed loop corrections in a variety of different settings; for example, Refs. [ref] .
One-loop corrections to the curvature perturbation from inflation · Introduction · 0.90
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This question was taken up by Weinberg in 2005 [ref] , and later by Chaicherdsakul [ref] .
Infrared effects in inflationary correlation functions · Time-dependent logarithms · 0.87
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Later estimates of loop effects were made in a large number of models [ref] , even at two-loop order [ref] .
One-loop corrections to a scalar field during inflation · Introduction · 0.87
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