[c0987] *R.e.a.d^ Inflation in Anisotropic Scalar-Tensor Theories - National Aeronautics and Space Administration #P.D.F@
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The purpose of this talk is to convince you that •anisotropic inflation is naturally realized in supergravity •statistical anisotropy is easily produced in supergravity •there is cross correlation between scalar and tensor perturbations •inflation can constrain the gauge kinetic.
Oct 9, 2018 1some review of anisotropic inflationary models can be found in refs. Initial entanglement between the scalar and tensor modes during.
In this article we consider a scalar-tensor theory in which the matter component is a field with a anisotropic power-law inflation for the dirac-born-infeld theory inflation in anisotropic scalar-tensor theories.
The first part of the thesis is devoted to a historical introduction and a physical justification of the scalar-tensor theories and anisotropic cosmological models.
Aug 2, 2019 the behavior of a non-canonical scalar field within an anisotropic scalar and tensor spectral indices, tensor-to-scalar ratio, the running.
The λcdm (lambda cold dark matter) or lambda-cdm model is a parameterization of the big bang cosmological model in which the universe contains three major components: first, a cosmological constant denoted by lambda (greek λ) and associated with dark energy; second, the postulated cold dark matter (abbreviated cdm); and third, ordinary matter.
Anisotropic inflation in scalar–tensor gravity in order to generate anisotropic effect during inflation, we add an abelian massless gauge kinetic term. It is coupled to the inflaton field through a gauge coupling function, to the general action of scalar tensor models.
The latest released data from planck in 2018 put up tighter constraints on inflationary parameters.
Anisotropic stress reduces the wave amplitude, thus lowering the tensor-mode induced cmb anisotropy and polarization [10–13]. In this paper, we will discuss the eect of anisotropic stress on tensor modes in infla-.
Kobe-th-15-04 yuki sakakihara, jiro soda primordial gravitational waves in bimetric gravity jcap 1509 (2015) 09, 015, arxiv1504. 【2014】 kobe-th-14-14 ippei obata, takashi miura, jiro soda.
We compute the phenomenological signatures of a model (watanabe et al' 09) of anisotropic inflation driven by a scalar and a vector field.
We study the imprints of the anisotropic inflation on the cmb temperature fluctuations and polarizations. The statistical anisotropy stems not only from the direction dependence of curvature and tensor perturbations, but also from the cross-correlation between curvature and tensor perturbations, and the linear polarization of tensor perturbations.
It implies that the universe (on large scales) is isotropic and homogeneous (as with r and rµν the scalar curvature and ricci curvature tensor respectively,.
Dark matter searches with xenon1t testing dark matter and neutrino mass models from anisotropic inflation without a vector field scalar-tensor theories inflation.
Garcia-bellido and quiros [ 52] solved the problem of inflation, based on a general scalar-tensor theory of gravity. They determined a particular class of models with a brans-dicke like behavior during inflation. The result converted continuously to general relativity during the radiation and matter-dominated eras.
Statistical anisotropies in scalar and tensor power spectra in model of anisotropic hybrid inflation hassan firouzjahi.
Apr 24, 2019 inflationary potentials, with planckian field excursions, described by a 6th we identify the most likely models which yield a tensor-to-scalar ratio r wave signal in the cosmic microwave background anisotropy.
Discussiongeneral scalar tensor theory has been studied in this paper for a class of anisotropic models, considering a viscous flow with bulk viscosity. We have examined both exponential expansion and power-law form of the scale factors for these models.
Abstract the existence of an inflationary phase in anisotropic scalar-tensor theories is investigated means of a conformal transformation that allows us to the slow-roll approximation is specified for cosmological models in scalar-tensor gravity theories.
The international school for advanced studies (sissa) was founded in 1978 and was the first institution in italy to promote post-graduate courses leading to a doctor philosophiae.
Starobinsky, constant-roll inflation in scalar-tensor gravity,.
–there exists an attractor solution of the anisotropic inflation depending on the form of coupling function. (shear/ expansion o(epsilon)) –in addition to direction dependence of curvature fluc.
Anisotropic inflation from charged scalar fields jcap 1102 (2011), 005 [abstract] arxive.
The existence of an inflationary phase in anisotropic scalar-tensor theories is investigated by means of a conformal transformation that allows us to rewrite these theories as gravity minimally coupled to a scalar field with a nontrivial potential.
We find exact anisotropic power-law inflationary solutions when both the potential function for an inflaton and the gauge kinetic function are exponential type. The dynamical system analysis tells us that the anisotropic power-law inflation is an attractor for a large parameter region.
It was found recently that the anisotropies in the homogeneous bianchi i cosmology considered within the context of a specific horndeski theory are damped near the initial singularity instead of being amplified. In this work we extend the analysis of this phenomenon to cover all of the horndeski family. We find that the phenomenon is absent in the k-essence and/or kinetic gravity braiding.
May 8, 2007 mordial perturbations, even though the energy momentum tensor of the perturbations created during inflation are statistically homogeneous and isotropic to create statistically anisotropic scalar primordial perturb.
No definitive evidence for cosmic inflation is found, but support remains.
Energy part of the post-inflationary oscillations, the system is anisotropic and the because of null results, the tensor-to-scalar perturbations r is severely.
On post-inflation validity of perturbation theory in horndeski scalar-tensor models: the system is anisotropic and the newtonian potential is largely amplified.
During inflation is the scalar field, which has no anisotropic stress at first order in perturbation theory, then the equation describing the tensor perturbations.
We determine the field equations and perturbations parameters, such as the scalar power spectrum, scalar spectral index, scalar potential, and tensor-to- scalar.
Oct 18, 2016 conditions required for homogeneous and isotropic hot big bang cosmology, obtain the tensor-to-scalar ratio for single-field slow-roll inflation.
Scalar + tensor equation system more complex (q, ψ, φ, hxx). Power spectra numerical calculation of axisymmetric power spectrum kiso hini calculation of cmb anisotropies expansion has isotropized by end of inflation.
Inflation, cosmic microwave background, large-scale structure, dark matter, baryon asymmetry.
Cmb temperature and polarization anisotropies from the large-n limit of global defects.
G5x changes the dynamics of spacetimeand the anisotropic attractors emerge. For example, slow-roll inflation can satisfy the condition to approach attractors.
The existence of an inflationary phase in anisotropic scalar-tensor theories is investigated by means of a conformal transformation that allows us to rewrite these theories as gravity minimally coupled to a scalar field with a a non-trivial potential. We then use the explicit form of the potential and the no hair theorem to conclude that there is an inflationary phase in all open or flat.
As a prototype, we formulate anisotropic inflation from the perspective of eft and construct an effective action of the nambu-goldstone bosons for the broken time translation and rotation symmetries. We also calculate the statistical anisotropy in the scalar two-point correlation function for concise examples of the effective action.
Dark matter searches with xenon1t testing dark matter and neutrino mass models from anisotropic inflation without a vector field order multi-scalar-tensor.
1 is achieved when the energy of the vector is about 6-7 orders of magnitude smaller than that of the scalar during inflation. For such values of the parameters, the scalar-tensor correlation (which is in principle a distinctive signature of anisotropic spaces) is smaller than the tensor-tensor correlation.
Sriramkumar, numerical evaluation of the three-point scalar-tensor cross-correlations and the tensor bi-spectrum, jcap 1312, 037 (2013) [arxiv:1309.
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