Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes
It appears that having our own brane to somehow interact with other branes could give rise to quite an interesting system and that interaction could lead to some observable effects. We consider the question of whether or not these signatures of interaction between the branes can be observed. To answ...
Saved in:
| Main Author: | |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
Wiley
2020-01-01
|
| Series: | Advances in High Energy Physics |
| Online Access: | http://dx.doi.org/10.1155/2020/3963279 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1832550515454509056 |
|---|---|
| author | Aroonkumar Beesham |
| author_facet | Aroonkumar Beesham |
| author_sort | Aroonkumar Beesham |
| collection | DOAJ |
| description | It appears that having our own brane to somehow interact with other branes could give rise to quite an interesting system and that interaction could lead to some observable effects. We consider the question of whether or not these signatures of interaction between the branes can be observed. To answer this question, we investigate the effect induced by the inflaton in the WMAP7 data using the warm inflationary model. In this model, slow-roll and perturbation parameters are given in terms of the inflaton thermal distribution. We show that this distribution depends on the orbital radius of the brane motion under the interaction potential of other branes in extra dimensions. Thus, an enhancement in the brane inflation can be a signature of an orbital motion in extra dimensions, and consequently, some signals of other branes can be detected by observational data. According to experimental data, the N≃50 case leads to ns≃0.96, where N and ns are the number of e-folds and the spectral index, respectively. This standard case may be found in the range 0.01<Rtensor‐scalar<0.22, where Rtensor‐scalar is the tensor-scalar ratio. We find that at this point, the radial distance between our brane and another brane is R=1.5 GeV−1 in intermediate and R=0.02225 GeV−1 in logamediate inflation. |
| format | Article |
| id | doaj-art-b980d12635214e48bd2e12f5890c36ee |
| institution | Kabale University |
| issn | 1687-7357 1687-7365 |
| language | English |
| publishDate | 2020-01-01 |
| publisher | Wiley |
| record_format | Article |
| series | Advances in High Energy Physics |
| spelling | doaj-art-b980d12635214e48bd2e12f5890c36ee2025-02-03T06:06:38ZengWileyAdvances in High Energy Physics1687-73571687-73652020-01-01202010.1155/2020/39632793963279Emergence of Warm Inflation in Curved Space-Time between Accelerating BranesAroonkumar Beesham0Faculty of Natural Sciences, Mangosuthu University of Technology, 511 Griffiths Mxenge Highway, Umlazi, Durban 4031, South AfricaIt appears that having our own brane to somehow interact with other branes could give rise to quite an interesting system and that interaction could lead to some observable effects. We consider the question of whether or not these signatures of interaction between the branes can be observed. To answer this question, we investigate the effect induced by the inflaton in the WMAP7 data using the warm inflationary model. In this model, slow-roll and perturbation parameters are given in terms of the inflaton thermal distribution. We show that this distribution depends on the orbital radius of the brane motion under the interaction potential of other branes in extra dimensions. Thus, an enhancement in the brane inflation can be a signature of an orbital motion in extra dimensions, and consequently, some signals of other branes can be detected by observational data. According to experimental data, the N≃50 case leads to ns≃0.96, where N and ns are the number of e-folds and the spectral index, respectively. This standard case may be found in the range 0.01<Rtensor‐scalar<0.22, where Rtensor‐scalar is the tensor-scalar ratio. We find that at this point, the radial distance between our brane and another brane is R=1.5 GeV−1 in intermediate and R=0.02225 GeV−1 in logamediate inflation.http://dx.doi.org/10.1155/2020/3963279 |
| spellingShingle | Aroonkumar Beesham Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes Advances in High Energy Physics |
| title | Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes |
| title_full | Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes |
| title_fullStr | Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes |
| title_full_unstemmed | Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes |
| title_short | Emergence of Warm Inflation in Curved Space-Time between Accelerating Branes |
| title_sort | emergence of warm inflation in curved space time between accelerating branes |
| url | http://dx.doi.org/10.1155/2020/3963279 |
| work_keys_str_mv | AT aroonkumarbeesham emergenceofwarminflationincurvedspacetimebetweenacceleratingbranes |