Braneworld Quintessential Inflation and Sum of Exponentials Potentials
| dc.creator | Gardner, Carl L. | |
| dc.date | 2007-01-04 | |
| dc.date.accessioned | 2026-07-07T07:38:47Z | |
| dc.date.available | 2026-07-07T07:38:47Z | |
| dc.description | Quintessential inflation--in which a single scalar field plays the role of the inflaton and quintessence--from a sum of exponentials potential V = A (exp{5 phi}+exp{sqrt{2} phi}) or V = A (exp{5 phi}+exp{phi}) or a cosh potential V = 2A cosh(5 phi) is considered in the context of five-dimensional gravitation with standard model particles confined to our 3-brane. Reheating is accomplished via gravitational particle production and the universe undergoes a transition from primordial inflation to radiation domination well before big bang nucleosynthesis. The transition to an accelerating universe due to quintessence occurs near z = 1, as in LambdaCDM. Braneworld quintessential inflation can occur for potentials with or without a minimum, and with or without eternal acceleration and an event horizon. The low z behavior of the equation of state parameter w_phi provides a clear observable signal distinguishing quintessence from a cosmological constant. | |
| dc.description | 20 pages, 15 figures | |
| dc.identifier | https://arxiv.org/abs/hep-ph/0701036 | |
| dc.identifier | http://arxiv.org/abs/hep-ph/0701036 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/121216 | |
| dc.subject | High Energy Physics - Phenomenology | |
| dc.title | Braneworld Quintessential Inflation and Sum of Exponentials Potentials | |
| dc.type | text |