Reheating constraints on a two-field inflationary model
Once inflation comes to an end, the Universe enters a short stage named reheating. Making coherent oscillations about the minimum of its potential, the inflaton field transforms into the particles that occupy the Universe at later times. Yet, there is no direct cosmological observables corresponding...
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doaj-a57216a88b8e4403b4112257a810c8c12020-11-25T00:47:04ZengElsevierNuclear Physics B0550-32132019-12-01949Reheating constraints on a two-field inflationary modelKosar Asadi0Kourosh Nozari1Department of Physics, Faculty of Basic Sciences, University of Mazandaran, P. O. Box 47416-95447, Babolsar, IranDepartment of Physics, Faculty of Basic Sciences, University of Mazandaran, P. O. Box 47416-95447, Babolsar, Iran; Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), P. O. Box 55134-441, Maragha, Iran; Corresponding author at: Department of Physics, Faculty of Basic Sciences, University of Mazandaran, P. O. Box 47416-95447, Babolsar, Iran.Once inflation comes to an end, the Universe enters a short stage named reheating. Making coherent oscillations about the minimum of its potential, the inflaton field transforms into the particles that occupy the Universe at later times. Yet, there is no direct cosmological observables corresponding to the reheating epoch. However, one can achieve some indirect limits, simply by taking into account cosmological evolution for observable CMB scales between the Hubble crossing time during inflation and the present time, for example. Moreover, since the reheating period takes place before the radiation dominated era, it can be modeled by an effective equation-of-state parameter, wreh. There is a limited range of reasonable values for wreh which can be regarded as the reheating period. In this paper, considering a two-field model, we investigate the reheating epoch so as to impose some constraints on the parameter space of the model. To do so, we are first required to obtain the reheating e-folds number as well as its temperature. These parameters can be written in terms of the scalar spectral index which let us perform numerical analysis in this model. Therefore, we can set some constraints on the reheating parameters which correspond to observationally viable values of the scalar spectral index.http://www.sciencedirect.com/science/article/pii/S055032131930313X |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Kosar Asadi Kourosh Nozari |
spellingShingle |
Kosar Asadi Kourosh Nozari Reheating constraints on a two-field inflationary model Nuclear Physics B |
author_facet |
Kosar Asadi Kourosh Nozari |
author_sort |
Kosar Asadi |
title |
Reheating constraints on a two-field inflationary model |
title_short |
Reheating constraints on a two-field inflationary model |
title_full |
Reheating constraints on a two-field inflationary model |
title_fullStr |
Reheating constraints on a two-field inflationary model |
title_full_unstemmed |
Reheating constraints on a two-field inflationary model |
title_sort |
reheating constraints on a two-field inflationary model |
publisher |
Elsevier |
series |
Nuclear Physics B |
issn |
0550-3213 |
publishDate |
2019-12-01 |
description |
Once inflation comes to an end, the Universe enters a short stage named reheating. Making coherent oscillations about the minimum of its potential, the inflaton field transforms into the particles that occupy the Universe at later times. Yet, there is no direct cosmological observables corresponding to the reheating epoch. However, one can achieve some indirect limits, simply by taking into account cosmological evolution for observable CMB scales between the Hubble crossing time during inflation and the present time, for example. Moreover, since the reheating period takes place before the radiation dominated era, it can be modeled by an effective equation-of-state parameter, wreh. There is a limited range of reasonable values for wreh which can be regarded as the reheating period. In this paper, considering a two-field model, we investigate the reheating epoch so as to impose some constraints on the parameter space of the model. To do so, we are first required to obtain the reheating e-folds number as well as its temperature. These parameters can be written in terms of the scalar spectral index which let us perform numerical analysis in this model. Therefore, we can set some constraints on the reheating parameters which correspond to observationally viable values of the scalar spectral index. |
url |
http://www.sciencedirect.com/science/article/pii/S055032131930313X |
work_keys_str_mv |
AT kosarasadi reheatingconstraintsonatwofieldinflationarymodel AT kouroshnozari reheatingconstraintsonatwofieldinflationarymodel |
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