Difference between revisions of "Different Models of Inflation"
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| − | There is a number of inflationary models. All of them deal with potentials of scalar fields which realize the slow-roll regime during sufficiently long period of evolution, then the inflation terminates and Universe enters the hot stage. It is worth noting that the models considered below are among the simplest ones and they do not exhaust all the possibilities, however they give main idea about possible features of the evolution of | + | There is a number of inflationary models. All of them deal with potentials of scalar fields which realize the slow-roll regime during sufficiently long period of evolution, then the inflation terminates and Universe enters the hot stage. It is worth noting that the models considered below are among the simplest ones and they do not exhaust all the possibilities, however they give the main idea about possible features of the evolution of scale factor in the slow-roll regime of inflation. |
| + | |||
| + | == Chaotic Inflation (Inflation with Power Law Potential) == | ||
| + | |||
| + | \emph{\textbf{The chaotic inflation} or the inflation with high field, is considered as a rule with the power law potentials of the form | ||
| + | $$V=g\varphi^n,$$ | ||
| + | where $g$ is a dimensional constant of interaction: | ||
| + | $$[g]=(\mbox{mass})^{4-n}$$ | ||
| + | It should be noted that the slow-roll conditions for the given potential are always satisfied for sufficiently high values of the inflaton field | ||
| + | $$\varphi\gg\frac{nM_{Pl}}{4\sqrt{3\pi}},$$ | ||
| + | therefore the slow-roll takes place at field values which are great compared to Planck units.} | ||
=== Problem 1 === | === Problem 1 === | ||
Revision as of 11:42, 27 August 2013
There is a number of inflationary models. All of them deal with potentials of scalar fields which realize the slow-roll regime during sufficiently long period of evolution, then the inflation terminates and Universe enters the hot stage. It is worth noting that the models considered below are among the simplest ones and they do not exhaust all the possibilities, however they give the main idea about possible features of the evolution of scale factor in the slow-roll regime of inflation.
Contents
- 1 Chaotic Inflation (Inflation with Power Law Potential)
- 1.1 Problem 1
- 1.2 Problem 2
- 1.3 Problem 3
- 1.4 Problem 4
- 1.5 Problem 5
- 1.6 Problem 6
- 1.7 Problem 7
- 1.8 Problem 8
- 1.9 Problem 9
- 1.10 Problem 10
- 1.11 Problem 11
- 1.12 Problem 12
- 1.13 Problem 13
- 1.14 Problem 14
- 1.15 Problem 15
- 1.16 Problem 16
- 1.17 Problem 17
- 1.18 Problem 18
- 1.19 Problem 19
- 1.20 Problem 20
- 1.21 Problem 21
- 1.22 Problem 22
- 1.23 Problem 23
- 1.24 Problem 24
- 1.25 Problem 25
- 1.26 Problem 26
- 1.27 Problem 27
- 1.28 Problem 28
- 1.29 Problem 29
- 1.30 Problem 30
- 1.31 Problem 31
- 1.32 Problem 32
- 1.33 Problem 33
- 1.34 Problem 34
- 1.35 Problem 35
- 1.36 Problem 36
- 1.37 Problem 37
- 1.38 Problem 38
- 1.39 Problem 39
Chaotic Inflation (Inflation with Power Law Potential)
\emph{\textbf{The chaotic inflation} or the inflation with high field, is considered as a rule with the power law potentials of the form $$V=g\varphi^n,$$ where $g$ is a dimensional constant of interaction: $$[g]=(\mbox{mass})^{4-n}$$ It should be noted that the slow-roll conditions for the given potential are always satisfied for sufficiently high values of the inflaton field $$\varphi\gg\frac{nM_{Pl}}{4\sqrt{3\pi}},$$ therefore the slow-roll takes place at field values which are great compared to Planck units.}
Problem 1
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Problem 2
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Problem 3
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Problem 4
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Problem 5
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Problem 6
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Problem 7
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Problem 8
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Problem 9
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Problem 10
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Problem 11
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Problem 12
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Problem 13
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Problem 14
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Problem 15
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Problem 16
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Problem 17
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Problem 18
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Problem 19
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Problem 20
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Problem 21
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Problem 22
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Problem 23
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Problem 24
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Problem 25
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Problem 26
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Problem 27
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Problem 28
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Problem 29
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Problem 30
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Problem 31
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Problem 32
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Problem 33
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Problem 34
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Problem 35
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Problem 36
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Problem 37
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Problem 38
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Problem 39
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