Obstructions to Bell CMB experiments

Martin, Jérôme; Vennin, Vincent

doi:10.1103/physrevd.96.063501

Cited by 76 publications

(88 citation statements)

References 81 publications

(107 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We will examine how the RG equation can be applied to V in the WZ model. The perturbative contributions to V have been computed to one [30,31,32,33,34,35], two [36,37,38,39] and three [40] loop order, and RG summation of LL contributions also examined [41].…”

Section: The Effective Potential In the Wess-zumino Modelmentioning

confidence: 99%

The renormalization group and the effective potential in the Wess–Zumino model

McKeon

2019

Can. J. Phys.

View full text Add to dashboard Cite

We consider the effective potential V in the massless Wess-Zumino model. By using the renormalization group equation, we show that the explicit and implicit dependence of V on the renormalization mass scale µ cancels. If V has an extremum at some non-vanishing value of the background field, then it follows that V is "flat", independent of the background field. This consistent with the general requirement that V be convex. The consequences for supersymmetric gauge theories are briefly considered.

show abstract

Section: The Effective Potential In the Wess-zumino Modelmentioning

confidence: 99%

The renormalization group and the effective potential in the Wess–Zumino model

McKeon

2019

Can. J. Phys.

View full text Add to dashboard Cite

show abstract

“…As we have just seen, there two cases in which adiabatic modes have fixed time dependence: pure vector adiabatic modes in general, N V i ∝ a −1 and, in the specific but relevant case of a generic scalar field, scalar modes R ∼ const. In these cases adiabatic modes are classical in the following sense (also see [28,29]). Let us compute the only commutator that has a chance of being non-vanishing in the quantum theory of R modes (a completely analogous argument applies to N V i mutatis mutandis), namely Since we have been studying adiabatic modes at linear order, which are symmetries of the free theory 10 , we can focus on free quantum fields…”

Section: Classical and Quantum Adiabatic Modesmentioning

confidence: 99%

Systematics of adiabatic modes: flat universes

Pajer

Jazayeri

2018

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Adiabatic modes are cosmological perturbations that are locally indistinguishable from a (large) change of coordinates. At the classical level, they provide model independent solutions. At the quantum level, they lead to soft theorems for cosmological correlators. We present a systematic derivation of adiabatic modes in spatially-flat cosmological backgrounds with asymptotically-perfect fluids. We find several new adiabatic modes including vector, time-dependent tensor and time-dependent scalar modes. The new vector and tensor modes decay with time in standard cosmologies but are the leading modes in contracting universes. We present a preliminary derivation of the related soft theorems. In passing, we discuss a distinction between classical and quantum adiabatic modes, we clarify the subtle nature of Weinberg's second adiabatic mode and point out that the adiabatic nature of a perturbation is a gauge dependent statement. 2 The new scalar adiabatic mode survives only if the scalar field is shift symmetric and leads to soft theorems for Ultra Slow Roll inflation [27]. 3 We use the notation of [25].

show abstract

“…Therefore, the negativity of the Wigner function is a signal of quantum origin of the system. We also note that the positivity of the Wigner function does not guarantee the absence of the quantum effect 2 [32,33]. For instance, we may find out a Bell inequality violation even if the Wigner function is non-negative.…”

Section: Introductionmentioning

confidence: 99%

Quantum nature of Wigner function for inflationary tensor perturbations

Gong

Seo

2020

J. High Energ. Phys.

View full text Add to dashboard Cite

We study the Wigner function for the inflationary tensor perturbation defined in the real phase space. We compute explicitly the Wigner function including the contributions from the cubic self-interaction Hamiltonian of tensor perturbations. Then we argue that it is no longer an appropriate description for the probability distribution in the sense that quantum nature allows negativity around vanishing phase variables. This comes from the non-Gaussian wavefunction in the mixed state as a result of the non-linear interaction between super-and sub-horizon modes. We also show that this is related to the explicit infrared divergence in the Wigner function, in contrast to the trace of the density matrix.

show abstract

Obstructions to Bell CMB experiments

Cited by 76 publications

References 81 publications

The renormalization group and the effective potential in the Wess–Zumino model

The renormalization group and the effective potential in the Wess–Zumino model

Systematics of adiabatic modes: flat universes

Quantum nature of Wigner function for inflationary tensor perturbations

Contact Info

Product

Resources

About