Loop Corrections to Standard Model fields in inflation

Chen, Xingang; Wang, Yi; Xianyu, Zhong Zhi

doi:10.1007/jhep08(2016)051

Cited by 109 publications

(103 citation statements)

References 114 publications

(180 reference statements)

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“…This will then allow smaller Λ σ and larger NG. It would also be very interesting to analyze all the "heavy-lifted" SM signals [10][11][12]16], especially the signal due to the loops of massive W bosons, in the curvaton scenario that was presented in this work. Using the above and eq.…”

Section: Discussionmentioning

confidence: 99%

“…Through a careful measurement of such dependencies, one can infer the mass and spin of such heavy particles-a rare opportunity to probe on-shell physics at very high energy scales. This is the focus of the "cosmological collider physics" program [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17]. For various recent ideas in this direction see, [18][19][20][21][22][23][24][25][26][27][28].…”

Section: Introductionmentioning

confidence: 99%

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Cosmological collider physics and the curvaton

Kumar

Sundrum

2020

J. High Energ. Phys.

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Primordial non-Gaussianity signatures of extremely heavy particles are reexamined within a simple alternative to the standard inflationary paradigm, in which the primordial fluctuations and the inflationary spacetime expansion are sourced by two different fields. The curvaton scenario provides an example of this in which the distinct roles are played by the curvaton and the inflaton fields, respectively. We study couplings of the curvaton to heavy particles with masses of order the inflationary Hubble scale, and show that they can lead to non-Gaussian signals orders of magnitude larger than those in standard inflation, consistent with explicit effective field theory control of inflationary dynamics. This brings various motivated particle physics signatures, such as loops of heavy gauge-charged scalars and fermions, within future observational reach. The curvaton paradigm can be viewed as a partial UV completion of effective field theories of only inflationary fluctuations in which large non-Gaussian signals of heavy particles have also been discussed, but in which inflationary dynamics is not explicitly derived.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Cosmological collider physics and the curvaton

Kumar

Sundrum

2020

J. High Energ. Phys.

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“…We do not know much about the spectrum of massless U (1)'s and charged particles during inflation, but a naive expectation is that if inflation happens before EWSB, we have an su(3) ⊕ su(2) ⊕ u(1)'s worth of massless gauge fields to analyze 25 . The charged spectrum of the SM remains massless at tree level (getting a mass of order Hubble scale via radiative corrections [138]), which violates (4.1). We now discuss some possible ways out of this conundrum 26 :…”

Section: Phenomenological Implicationsmentioning

confidence: 99%

Festina lente:1 EFT constraints from charged black hole evaporation in de Sitter

2020

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In the Swampland philosophy of constraining EFTs from black hole mechanics we study charged black hole evaporation in de Sitter space. We establish how the black hole mass and charge change over time due to both Hawking radiation and Schwinger pair production as a function of the masses and charges of the elementary particles in the theory. We find a lower bound on the mass of charged particles by demanding that large charged black holes evaporate back to empty de Sitter space, in accordance with the thermal picture of the de Sitter static patch. This bound is satisfied by the charged spectrum of the Standard Model. We discuss phenomenological implications for the cosmological hierarchy problem and inflation. Enforcing the thermal picture also leads to a heuristic remnant argument for the Weak Gravity Conjecture in de Sitter space, where the usual kinematic arguments do not work. We also comment on a possible relation between WGC and universal bounds on equilibration times. All in all, charged black holes in de Sitter should make haste to evaporate, but they should not rush it 2 .

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“…The dark matter loop can be attached to any of the k 1 , k 2 and k 3 legs. In the squeezed can be found in [79][80][81][82], and it had also been applied to complex scalar fields in [83]. The crucial point is that although in general, loop diagrams may suffer from UV or IR divergence [84], and usually we need to introduce local counter terms to cancel the UV divergence, the clock-signal part of the contribution does not suffer from UV or IR divergence.…”

Section: Dark Matter On the Cosmological Collidermentioning

confidence: 99%

Gravitational production of superheavy dark matter and associated cosmological signatures

Nakama

Sou

et al. 2019

J. High Energ. Phys.

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We study the gravitational production of super-Hubble-mass dark matter in the very early universe. We first review the simplest scenario where dark matter is produced mainly during slow roll inflation. Then we move on to consider the cases where dark matter is produced during the transition period between inflation and the subsequent cosmological evolution. The limits of smooth and sudden transitions are studied, respectively. The relic abundances and the cosmological collider signals are calculated.

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Loop Corrections to Standard Model fields in inflation

Cited by 109 publications

References 114 publications

Cosmological collider physics and the curvaton

Cosmological collider physics and the curvaton

Festina lente:1 EFT constraints from charged black hole evaporation in de Sitter

Gravitational production of superheavy dark matter and associated cosmological signatures

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