Tamé González

Universidad de Guanajuato

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Israel Quirós

Universidad de Guanajuato

Ricardo García‐Salcedo

Instituto Politécnico Nacional

Ulises Nucamendi

Universidad Michoacana de San Nicolás de Hidalgo

Francisco Antonio Horta-Rangel

Universidad de Guanajuato

Roberto De Arcia

Universidad de Guanajuato

Rolando Cárdenas

Universidad Central "Marta Abreu" de las Villas (UCLV)

Claudia M. Moreno

University of Washington

Dania González

Universidad Central "Marta Abreu" de las Villas (UCLV)

Yoelsy Leyva

University of Tarapacá

Genly León

Universidad Católica del Norte

Cooperative Institutions

Universidad Central "Marta Abreu" de las Villas (UCLV)

Universidad de Guanajuato

Instituto Politécnico Nacional

Universidad Michoacana de San Nicolás de Hidalgo

Universidad Nacional Autónoma de México

Center for Research and Advanced Studies of the National Polytechnic Institute

Pontificia Universidad Católica de Valparaíso

Universidad de Guadalajara

Universidad Central

Autonomous University of Chiapas

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Bulk viscous matter-dominated Universes: asymptotic properties

Journal of Cosmology and Astroparticle Physics (2013)

Arturo Avelino Ricardo García‐Salcedo Tamé González Ulises Nucamendi Israel Quirós

By means of a combined use of the type Ia supernovae and H(z) data tests, together with the study of the asymptotic properties in the equivalent phase space — through the use of the dynamical systems tools — we demonstrate that the bulk viscous matter-dominated scenario is not a good model to explain the accepted cosmological paradigm, at least, under the parametrization of bulk viscosity considered in this paper. The main objection against such scenarios is the absence of conventional radiation and matter-dominated critical points in the phase space of the model. This entails that radiation and matter dominance are not generic solutions of the cosmological equations, so that these stages can be implemented only by means of unique and very specific initial conditions, i. e., of very unstable particular solutions. Such a behavior is in marked contradiction with the accepted cosmological paradigm which requires of an earlier stage dominated by relativistic species, followed by a period of conventional non-relativistic matter domination, during which the cosmic structure we see was formed. Also, we found that the bulk viscosity is positive just until very late times in the cosmic evolution, around z < 1. For earlier epochs it is negative, been in tension with the local second law of thermodynamics.

Volume viscosity

Parametrization (atmospheric modeling)

10.1088/1475-7516/2013/08/012

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Citations (16)

Dirac-Born-Infeld Field Trapped in the Braneworld

arXiv (Cornell University) (2009)

Ricardo García‐Salcedo Dania González Tamé González Claudia M. Moreno Israel Quirós

We apply the dynamical systems tools to study the (linear) cosmic dynamics of a Dirac-Born-Infeld-type field trapped in the braneworld. We focus,exclusively, in Randall-Sundrum and in Dvali-Gabadadze-Porrati brane models. We analyze the existence and stability of asymptotic solutions for the AdS throat and the quadratic potential and a particular choice of the warp factor and of the potential for the DBI field ($f(ϕ)=1/V(ϕ)$). It is demonstrated, in particular, that in the ultra-relativistic approximation matter-scaling and scalar field-dominated solutions always arise. In the first scenario the empty universe is the past attractor, while in the second model the past attractor is the matter-dominated phase.

10.48550/arxiv.0907.0185

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Power-Law NLED-Based Magnetic Universe Can Mimic Phantom Behavior

arXiv (Cornell University) (2010)

Ricardo García‐Salcedo Tamé González Claudia Moreno Israel Quirós

We study the cosmic dynamics of a magnetic universe supported by non-linear electrodynamics (NLED) Lagrangeans that are proportional to powers of the electromagnetic invariant $\propto F^{1/(1-m)}$ ($m$ is an overall constant). For simplicity we focus in the case when $F$ depends on the magnetic field alone, a case dubbed in the bibliography as ''magnetic universe''. Our results demonstrate that, depending on the values of the free parameter $m$, the magnetic field can mimic phantom field behavior, an effect previously found in other contexts. It is demonstrated that, since there are found equilibrium points in the phase space of these models that can be associated with magnetic-dominated past and future attractors, a combination of positive and negative powers of $F$ may lead to interesting cosmological behavior. In particular, a cosmological scenario where the universe might evolve from a past NLED-driven (non-inflationary) state into a future (late-time) -- also NLED-driven -- inflationary stage, transiting through a matter-dominated solution, is envisioned. The impact of braneworld gravity on the dynamics driven by such NLED Lagrangeans is also investigated. It is demonstrated that, due to phantom property at late times, the non-linear electromagnetic effects may play an important role in deciding the fate of the cosmic evolution. Randall-Sundrum brane effects, in particular, modify the nature of the starting point of the cosmic evolution, as well as the fate of the expansion: both, the big bang singularity and the big rip event -- inherent in general relativity with phantom matter source --, may be avoided.

Big Rip

Phantom energy

10.48550/arxiv.1006.2274

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The Evolution of density perturbations in two quintessence models

arXiv (Cornell University) (2004)

Tamé González Rolando Cárdenas

In this work we investigate the evolution of matter density perturbations for two different quintessence models. One of them is based on the Einstein theory of gravity, while the other is based on the Brans-Dicke scalar tensor theory. We show that it is possible to constrain the parameter space of the models using the determinations for the growth rate of perturbations derived from data of the 2-degree Field Galaxy Redshift Survey.

Quintessence

Scalar–tensor theory

Field galaxy

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The evolution of density perturbations in two quintessence models

arXiv (Cornell University) (2004)

Tamé González Rolando Cárdenas

Quintessence

Scalar–tensor theory

Field galaxy

10.48550/arxiv.astro-ph/0403031

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Dynamics of a Deformed Tachyon Field

arXiv (Cornell University) (2009)

Israel Quirós Tamé González Dania González Yunelsy N Alvarez Ricardo García‐Salcedo

Tachyon

Dynamics

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Dynamics of a self-interacting scalar field trapped in the braneworld for a wide variety of self-interaction potentials

Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D, Particles, fields, gravitation, and cosmology (2009)

Yoelsy Leyva Dania González Tamé González Tonatiuh Matos Israel Quirós

We apply the dynamical systems tools to study the linear dynamics of a self-interacting scalar field trapped in the braneworld, for a wide variety of self-interaction potentials. We focus on Randall-Sundrum and on Dvali-Gabadadze-Porrati braneworld models exclusively. These models are complementary to each other: while the Randall-Sundrum brane produces UV) corrections to general relativity, the Dvali-Gabadadze-Porrati braneworld modifies Einstein's theory at large scales, i e., produces IR modifications of general relativity. This study of the asymptotic properties of both braneworld models, shows---in the phase space---the way the dynamics of a scalar field trapped in the brane departs from standard general relativity behavior.

Randall–Sundrum model

10.1103/physrevd.80.044026

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Citations (38)

Dynamics of quintessence models of dark energy with exponential coupling to dark matter

Classical and Quantum Gravity (2006)

Tamé González Genly León Israel Quirós

We explore quintessence models of dark energy which exhibit non-minimal coupling between the dark matter and dark energy components of the cosmic fluid. The kind of coupling chosen is inspired by scalar–tensor theories of gravity. We impose a suitable dynamics of the expansion allowing us to derive exact Friedmann–Robertson–Walker solutions once the coupling function is given as input. Self-interaction potentials of single and double exponential types emerge as a result of our choice of the coupling function. The stability and existence of the solutions are discussed in some detail. Although, in general, models with appropriate interaction between the components of the cosmic mixture are useful for handling the coincidence problem, in the present study this problem cannot be avoided due to the choice of solution generating ansatz.

Quintessence

Ansatz

10.1088/0264-9381/23/9/025

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Citations (102)

Inflationary equilibrium configurations of scalar-tensor theories of gravity

Physical review. D/Physical review. D. (2020)

Israel Quirós Tamé González Roberto De Arcia Ricardo García‐Salcedo Ulises Nucamendi

In this paper we investigate the asymptotic dynamics of inflationary cosmological models that are based in scalar-tensor theories of gravity. Our main aim is to explore the global structure of the phase space in the framework of single-field inflation models. For this purpose we make emphasis in the adequate choice of the variables of the phase space. Our results indicate that, although single-field inflation is generic in the sense that the corresponding critical point in the phase space exists for a wide class of potentials, along given phase space orbits -- representing potential cosmic histories -- the occurrence of the inflationary stage is rather dependent on the initial conditions. We have been able to give quantitative estimates of the relative probability (RP) for initial conditions leading to slow-roll inflation. For the non-minimal coupling model with the $\phi^2$-potential our rough estimates yield to an almost vanishing relative probability: $10^{-13}\,\%\lesssim RP\ll 10^{-8}\,\%$. These bonds are greatly improved in the scalar-tensor models, including the Brans-Dicke theory, where the relative probability $1\,\%\lesssim RP\leq 100\,\%$. Hence slow-roll inflation is indeed a natural stage of the cosmic expansion in Brans-Dicke models of inflation. It is confirmed as well that the dynamics of vacuum Brans-Dicke theories with arbitrary potentials are non-chaotic.

Brans–Dicke theory

10.1103/physrevd.101.103518

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An issue with the classification of the most general scalar-tensor theories

arXiv (Cornell University) (2019)

Israel Quirós Francisco Antonio Horta-Rangel Roberto De Arcia Ismael Delgado Gaspar Ricardo García‐Salcedo

In the present paper we discuss on the issue that arises when one tries to classify the gravitational theories into scalar-tensor theories or general relativity with a scalar field non-minimally coupled to matter. Despite that the issue might seem like a trivial one, some confusion might arise when dealing with higher-derivatives Horndeski theories that at first sight do not look like scalar-tensor theories. To further complicate things, the discussion on the physical equivalence of the different conformal frames in which a given scalar-tensor theory may be formulated, makes even harder to achieve a correct classification.

Scalar–tensor theory

Confusion

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