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Anisotropic powerlaw inflation
 Journal of Cosmology and Astroparticle Physics 2010 (Dec
"... Abstract. It is widely believed that anisotropy in the expansion of the universe will decay exponentially fast during inflation. This is often referred to as the cosmic nohair conjecture. However, we find a counter example to the cosmic nohair conjecture in the context of supergravity. As a demons ..."
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demonstration, we present an exact anisotropic powerlaw inflationary solution which is an attractor in the phase space. We emphasize that anisotropic inflation is quite generic in the presence of anisotropic sources which couple with an inflaton. 1.
On Power Law Inflation in DBI Models
, 2007
"... Abstract: Inflationary models in string theory which identify the inflaton with an open string modulus lead to effective field theories with noncanonical kinetic terms – DiracBornInfeld scalar field theories. In the case of a Dbrane moving in an AdS throat with a quadratic scalar field potential ..."
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potential DBI kinetic terms allow a novel realization of power law inflation. This note adresses the question of whether this behaviour is special to this particular choice of throat geometry and potential. The answer is that for any throat geometry one can explicitly find a potential which leads to power
On Power Law Inflation in DBI Models
, 2007
"... Abstract: Inflationary models in string theory which identify the inflaton with an open string modulus lead to effective field theories with noncanonical kinetic terms – DiracBornInfeld scalar field theories. In the case of a Dbrane moving in an AdS throat with a quadratic scalar field potential ..."
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potential DBI kinetic terms allow a novel realization of power law inflation. This note adresses the question of whether this behaviour is special to this particular choice of throat geometry and potential. The answer is that for any throat geometry one can explicitly find a potential which leads to power
New exact solutions for power–law inflation
, 2001
"... We consider the spatially flat Friedmann model ds 2 = dt 2 − a 2 (t)(dx 2 + dy 2 + dz 2). For a ≈ t p, especially, if p ≥ 1, this is called powerlaw inflation. For the Lagrangian L = R m with p = −(m − 1)(2m − 1)/(m − 2) powerlaw inflation is an exact solution, as it is for Einstein gravity with a ..."
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We consider the spatially flat Friedmann model ds 2 = dt 2 − a 2 (t)(dx 2 + dy 2 + dz 2). For a ≈ t p, especially, if p ≥ 1, this is called powerlaw inflation. For the Lagrangian L = R m with p = −(m − 1)(2m − 1)/(m − 2) powerlaw inflation is an exact solution, as it is for Einstein gravity
PowerLaw Inflation from the Rolling Tachyon
, 2002
"... Modeling the potential by an inverse square law in terms of the tachyon field (V (T) = βT −2) we find exact solution for spatially flat isotropic universe. We show that for β> 2 √ 3/3 the model undergoes powerlaw inflation. A way to construct other exact solutions is specified and exemplified. ..."
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Modeling the potential by an inverse square law in terms of the tachyon field (V (T) = βT −2) we find exact solution for spatially flat isotropic universe. We show that for β> 2 √ 3/3 the model undergoes powerlaw inflation. A way to construct other exact solutions is specified and exemplified
Powerlaw inflation in spacetimes without symmetry
 Commun. Math. Phys
, 2007
"... We consider models of accelerated cosmological expansion described by the Einstein equations coupled to a nonlinear scalar field with a suitable exponential potential. We show that homogeneous and isotropic solutions are stable under small nonlinear perturbations without any symmetry assumptions. Ou ..."
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We consider models of accelerated cosmological expansion described by the Einstein equations coupled to a nonlinear scalar field with a suitable exponential potential. We show that homogeneous and isotropic solutions are stable under small nonlinear perturbations without any symmetry assumptions. Our proof is based on results on the nonlinear stability of de Sitter spacetime and KaluzaKlein reduction techniques.
A Consistency Relation for Power Law Inflation in DBI models
, 2007
"... Abstract: Brane inflation in string theory leads to a new realization of power law inflation which can give rise to significant nongaussianity. This can happen for any throat geometry if the scalar potential is appropriate. This note presents a consistency relation connecting the running of the non ..."
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Abstract: Brane inflation in string theory leads to a new realization of power law inflation which can give rise to significant nongaussianity. This can happen for any throat geometry if the scalar potential is appropriate. This note presents a consistency relation connecting the running
A Consistency Relation for Power Law Inflation in DBI Models
, 2007
"... Abstract: Brane inflation in string theory leads to a new realization of power law inflation which can give rise to significant nongaussianity. This can happen for any throat geometry if the scalar potential is appropriate. This note presents a consistency relation connecting the running of the non ..."
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Abstract: Brane inflation in string theory leads to a new realization of power law inflation which can give rise to significant nongaussianity. This can happen for any throat geometry if the scalar potential is appropriate. This note presents a consistency relation connecting the running
Noncommutative Powerlaw Inflation: Mode Equation and Spectra
"... Following an elegant approach that merge the effects of the stringy spacetime uncertainty relation into primordial perturbations suggested by Brandenberger and Ho, we show the mode equation up to the first order of noncommutative parameter. A new approximation is provided to calculate the mode func ..."
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functions analytically in the noncommutative powerlaw inflation models. It turns out that noncommutativity of spacetime can provide small corrections to the power spectrum of primordial fluctuations as the firstyear results of WMAP indicate. Moreover, using the WMAP data, we obtain the value
Results 1  10
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123,846