Vacuum Effective Actions and Mass-Dependent Renormalization in Curved Space

Franchino-Viñas, S. A.; Netto, Tibério de Paula; Zanusso, Omar

doi:10.3390/universe5030067

Cited by 17 publications

(15 citation statements)

References 80 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…a dynamical deformation of the original spacetime by the one-loop contributions of the scalar field. A similar effect could be seen in the commutative case, where the one-loop effects of the scalar field generate new terms in the gravitational sector [35][36][37][38].…”

Section: The One-loop Effective Actionsupporting

confidence: 54%

Asymptotic freedom for $$\lambda \phi ^4_{\star }$$ QFT in Snyder–de Sitter space

Franchino-Viñas

Mignemi

2020

Eur. Phys. J. C

View full text Add to dashboard Cite

We analyze the model of a self-interacting $$\phi ^4_{\star }$$ϕ⋆4 scalar field theory in Snyder–de Sitter space. After analytically computing the one-loop beta functions in the small noncommutativity and curvature limit, we solve numerically the corresponding system of differential equations, showing that in this limit the model possesses at least one regime in which the theory is asymptotically free. Moreover, in a given region of the parameter space we also observe a peculiar running of the parameter associated to the curvature, which changes its sign and therefore can be interpreted as a transition from an IR de-Sitter space to and UV anti-de Sitter one.

show abstract

Section: The One-loop Effective Actionsupporting

confidence: 54%

Asymptotic freedom for $$\lambda \phi ^4_{\star }$$ QFT in Snyder–de Sitter space

Franchino-Viñas

Mignemi

2020

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…2 As an additional discussion of the motivations of our work, let us mention that the same formula for the running (1) follows from the hypothesis of quadratic decoupling for the cosmological constant [9,[24][25][26]. In the case of cosmological or Newton constants, this is just a well-motivated hypothesis, while for the fourth-derivative terms it can be proved by direct quantum calculations [8,[28][29][30]. It is important to note that the identification of the scaling (renormalization group) parameter μ with the Hubble parameter H has been achieved not only on the phenomenological background, but was also derived within the especially developed scale-setting procedure [31].…”

Section: Background Solutionmentioning

confidence: 71%

Primordial universe with the running cosmological constant

et al. 2020

Self Cite

View full text Add to dashboard Cite

Theoretically, the running of the cosmological constant in the IR region is not ruled out. On the other hand, from the QFT viewpoint, the energy released due to the variation of the cosmological constant in the late Universe cannot go to the matter sector. For this reason, the phenomenological bounds on such a running are not sufficiently restrictive. The situation can be different in the early Universe when the gravitational field was sufficiently strong to provide an efficient creation of particles from the vacuum. We develop a framework for systematically exploring this possibility. It is supposed that the running occurs in the epoch when the Dark Matter already decoupled and is expanding adiabatically, while the usual matter should be regarded approximately massless and can be abundantly created from vacuum due to the decay of vacuum energy. By using the handy model of Reduced Relativistic Gas for describing the warm Dark Matter, we consider the dynamics of both cosmic background and linear perturbations and evaluate the impact of the vacuum decay on the matter power spectrum and to the first CMB peak. Additionally, using the combined SNIa+BAO data, we find the best-fit values for the free parameters of the model.

show abstract

“…The constants C 1 ... 6 can be found from the initial renormalization conditions. For instance, the two well-known values which correspond to the standard choices in the massless scalar case are C 4 = − 25 6 obtained in [7] and C 2 = −3 obtained in [5] (see [2] for a more pedagogical derivation). Since this calculation of the values of C 1 ... 6 for the massive theory is rather cumbersome and there are no immediate applications, we skip it.…”

Section: Therefore We Can Writementioning

confidence: 99%

“…According to the recent discussion in Refs. [24,25] this term can be relevant in cosmology, in the periods when the inverse of the size of the horizon may be comparable with the cosmic scale. Up to some extent, the corresponding effect can lead to the change of observational predictions in both inflationary and late cosmology epochs.…”

Section: δS δϕ ϕ=Vmentioning

confidence: 99%

Renormalization of Yukawa model with sterile scalar in curved spacetime

et al. 2019

View full text Add to dashboard Cite

We explore the classical and quantum properties of a sterile scalar field coupled to N copies of Dirac fermions in an external gravitational field. We find that the self-interaction scalar potential of a model that is consistent at the quantum level, includes odd (first and third) powers of a scalar. In particular, one has to consider, besides the standard non-minimal coupling of the form ξϕ 2 R, the new type of non-minimal coupling of the form f ϕ R with new non-minimal parameter f. We study the one-loop renormalization of such a theory including renormalization of the new non-minimal coupling. Also, we calculate the one-loop effective potential using the renormalization group and show how the renormalization group analysis should be extended compared to the standard expression which was derived in 1980ies. This conclusion is supported by the direct calculation of effective potential using normal coordinates and covariant cutoff regularization. The important features of the classical theory with a sterile scalar are related to the presence of the qualitatively new terms in the induced action of gravity, coming from the odd terms. We show that this new feature of the theory may have phenomenologically relevant consequences, both in the low-energy gravitational physics and at the high energies, corresponding to inflation.

show abstract

Vacuum Effective Actions and Mass-Dependent Renormalization in Curved Space

Cited by 17 publications

References 80 publications

Asymptotic freedom for $$\lambda \phi ^4_{\star }$$ QFT in Snyder–de Sitter space

Asymptotic freedom for $$\lambda \phi ^4_{\star }$$ QFT in Snyder–de Sitter space

Primordial universe with the running cosmological constant

Renormalization of Yukawa model with sterile scalar in curved spacetime

Contact Info

Product

Resources

About