Cosmology with negative potentials

By Gary N. Felder, Andrei V. Frolov, Lev Kofman, Andrei Linde. Physical Review D, 2002

203 citations recorded by the source corpus.

We investigate cosmological evolution in models where the effective potential $V(\ensuremath{\varphi})$ may become negative for some values of the field $\ensuremath{\varphi}.$ Phase portraits of such theories in the space of variables $(\ensuremath{\varphi},\stackrel{\ifmmode \dot{}\else \.{}\fi{}}{\ensuremath{\varphi}},H)$ have several qualitatively new features as compared with phase portraits in the theories with $V(\ensuremath{\varphi})g0.$ Cosmological evolution in models with potentials with a ``stable'' minimum at $V(\ensuremath{\varphi})l0$ is similar in some respects to the evolution in models with potentials unbounded from below. Instead of reaching an AdS regime dominated by the negative vacuum energy, the universe reaches a turning point where its energy density vanishes, and then it contracts to a singularity with properties that are practically independent of $V(\ensuremath{\varphi}).$ We apply our methods to investigation of the recently proposed cyclic universe scenario. We show that in addition to the singularity problem there are other problems that need to be resolved in order to realize a cyclic regime in this scenario. We propose several modifications of this scenario and conclude that the best way to improve it is to add a usual stage of inflation after the singularity and use that inflationary stage to generate perturbations in the standard way.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/504c04aac353938a3e1e9982a17e56a2ffb33e69

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Citations in the corpus

Quantum nature of the big bang: An analytical and numerical investigation (2006, background): “In the Cyclic model, collision occurs between the boundary branes [6], however it has been shown that the singularity problems persists [76].”
Beauty is attractive: Moduli trapping at enhanced symmetry points (2004, background): “ an ESP. In order to apply our results to the vacuum selection problem, we will need to know how large a range of φwe can scan over in the presence of Hubble friction. This can be obtained as follows [30]. If we are in an FRW phase, a(t) = a 0tβ (4.4) then the equation of motion for φ(ignoring any p”
Inflationary Cosmology after Planck 2013 (2014, methodology): “When we analyzed this scenario using the particular potential given in [180], and took into account the effect of particle production in the early universe, we found a very different cosmological regime [181, 182].”
Is there supernova evidence for dark energy metamorphosis (2003, background): “(11) [Models in which ρDE(z) < 0 for z < 0 and which violate the WEC in the future have been discussed in Felder et al. (2002); Kallosh et al. (2002); Alam et al. (2003).]”
Higgs Inflation (2018, background): “If they are small, Higgs inflation provides an appealing relation between the Standard Model parameters and the properties of the Universe at large scales.”
Cosmological attractors and initial conditions for inflation (2015, background): “Then, during the first stage of the field evolution, one can entirely ignore its potential energy, so that the equation becomes φ̈ = − √ 3/2 φ̇(2), with the solution [29]”