Resurrecting power law inflation in the light of Planck results

被引：50
|
作者：
Unnikrishnan, Sanil [1 ]
Sahni, Varun [2 ]
机构：
[1] Indian Inst Sci Educ & Res, Sch Phys, Thiruvananthapuram 695016, Kerala, India
[2] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India
来源：
JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2013年 / 10期
关键词：
inflation; non-gaussianity; physics of the early universe; COSMOLOGICAL MODELS; UNIVERSE SCENARIO; FLAT-SPECTRUM; FLUCTUATIONS; DYNAMICS; PERTURBATIONS; CONSTRAINTS; HORIZON; DBI;
D O I：
10.1088/1475-7516/2013/10/063
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
It is well known that a canonical scalar field with an exponential potential can drive power law inflation (PLI). However, the tensor-to-scalar ratio in such models turns out to be larger than the stringent limit set by recent Planck results. We propose a new model of power law inflation for which the scalar spectra index, the tensor-to-scalar ratio and the non-gaussianity parameter f(NL)(eril) are in excellent agreement with Planck results. Inflation, in this model, is driven by a non-canonical scalar field with an inverse power law potential. The Lagrangian for our model is structurally similar to that of a canonical scalar field and has a power law form for the kinetic term. A simple extension of our model resolves the graceful exit problem which usually afflicts models of power law inflation.
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收藏
页数：15
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