Some constraints on inflation models with power-law potentials
نویسندگان
چکیده
منابع مشابه
on some bayesian statistical models in actuarial science with emphasis on claim count
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15 صفحه اولNew exact solutions for power–law inflation Friedmann models
We consider the spatially flat Friedmann model ds = dt − a(t)(dx + dy + dz) . For a ≈ tp, especially, if p ≥ 1, this is called power-law inflation. For the Lagrangian L = Rm with p = −(m − 1)(2m − 1)/(m − 2) power-law inflation is an exact solution, as it is for Einstein gravity with a minimally coupled scalar field Φ in an exponential potential V (Φ) = exp(μΦ) and also for the higher-dimension...
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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 power-law inflation. A way to construct other exact solutions is specified and exemplified. Several interesting attempts to reconcile the inflationary paradigm with string theories have result...
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2004
ISSN: 1550-7998,1550-2368
DOI: 10.1103/physrevd.69.021301