Stability of a Noncanonical Scalar Field Model during Cosmological Date
Using the noncanonical model of scalar field, the cosmological consequences of a pervasive, self-interacting, homogeneous, and rolling scalar field are studied. In this model, the scalar field potential is “nonlinear” and decreases in magnitude with increasing the value of the scalar field. A specia...
Saved in:
| Main Authors: | , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
Wiley
2016-01-01
|
| Series: | Advances in High Energy Physics |
| Online Access: | http://dx.doi.org/10.1155/2016/3047461 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1832565715705528320 |
|---|---|
| author | Z. Ossoulian T. Golanbari H. Sheikhahmadi Kh. Saaidi |
| author_facet | Z. Ossoulian T. Golanbari H. Sheikhahmadi Kh. Saaidi |
| author_sort | Z. Ossoulian |
| collection | DOAJ |
| description | Using the noncanonical model of scalar field, the cosmological consequences of a pervasive, self-interacting, homogeneous, and rolling scalar field are studied. In this model, the scalar field potential is “nonlinear” and decreases in magnitude with increasing the value of the scalar field. A special solution of the nonlinear field equations of ϕ that has time dependency as fixed point is obtained. The fixed point relies on the noncanonical term of action and γ-parameter; this parameter appeared in energy density of scalar field redshift. By means of such fixed point the different eigenvalues of the equation of motion will be obtained. In different epochs in the evolution of the Universe for different values of q and n, the potentials as a function of scalar field are attained. The behavior of baryonic perturbations in linear perturbation scenario as a considerable amount of energy density of scalar field at low redshifts prevents the growth of perturbations in the ordinary matter fluid. The energy density in the scalar field is not appreciably perturbed by nonrelativistic gravitational fields, in either the radiation or matter dominant or scalar field dominated epoch. |
| format | Article |
| id | doaj-art-5fb02b8b36dc4dbdbe82b34e417953a5 |
| institution | Kabale University |
| issn | 1687-7357 1687-7365 |
| language | English |
| publishDate | 2016-01-01 |
| publisher | Wiley |
| record_format | Article |
| series | Advances in High Energy Physics |
| spelling | doaj-art-5fb02b8b36dc4dbdbe82b34e417953a52025-02-03T01:06:56ZengWileyAdvances in High Energy Physics1687-73571687-73652016-01-01201610.1155/2016/30474613047461Stability of a Noncanonical Scalar Field Model during Cosmological DateZ. Ossoulian0T. Golanbari1H. Sheikhahmadi2Kh. Saaidi3Department of Physics, Faculty of Science, University of Kurdistan, Pasdaran Street, Sanandaj 66177-15175, IranDepartment of Physics, Faculty of Science, University of Kurdistan, Pasdaran Street, Sanandaj 66177-15175, IranDepartment of Physics, Faculty of Science, University of Kurdistan, Pasdaran Street, Sanandaj 66177-15175, IranDepartment of Physics, Faculty of Science, University of Kurdistan, Pasdaran Street, Sanandaj 66177-15175, IranUsing the noncanonical model of scalar field, the cosmological consequences of a pervasive, self-interacting, homogeneous, and rolling scalar field are studied. In this model, the scalar field potential is “nonlinear” and decreases in magnitude with increasing the value of the scalar field. A special solution of the nonlinear field equations of ϕ that has time dependency as fixed point is obtained. The fixed point relies on the noncanonical term of action and γ-parameter; this parameter appeared in energy density of scalar field redshift. By means of such fixed point the different eigenvalues of the equation of motion will be obtained. In different epochs in the evolution of the Universe for different values of q and n, the potentials as a function of scalar field are attained. The behavior of baryonic perturbations in linear perturbation scenario as a considerable amount of energy density of scalar field at low redshifts prevents the growth of perturbations in the ordinary matter fluid. The energy density in the scalar field is not appreciably perturbed by nonrelativistic gravitational fields, in either the radiation or matter dominant or scalar field dominated epoch.http://dx.doi.org/10.1155/2016/3047461 |
| spellingShingle | Z. Ossoulian T. Golanbari H. Sheikhahmadi Kh. Saaidi Stability of a Noncanonical Scalar Field Model during Cosmological Date Advances in High Energy Physics |
| title | Stability of a Noncanonical Scalar Field Model during Cosmological Date |
| title_full | Stability of a Noncanonical Scalar Field Model during Cosmological Date |
| title_fullStr | Stability of a Noncanonical Scalar Field Model during Cosmological Date |
| title_full_unstemmed | Stability of a Noncanonical Scalar Field Model during Cosmological Date |
| title_short | Stability of a Noncanonical Scalar Field Model during Cosmological Date |
| title_sort | stability of a noncanonical scalar field model during cosmological date |
| url | http://dx.doi.org/10.1155/2016/3047461 |
| work_keys_str_mv | AT zossoulian stabilityofanoncanonicalscalarfieldmodelduringcosmologicaldate AT tgolanbari stabilityofanoncanonicalscalarfieldmodelduringcosmologicaldate AT hsheikhahmadi stabilityofanoncanonicalscalarfieldmodelduringcosmologicaldate AT khsaaidi stabilityofanoncanonicalscalarfieldmodelduringcosmologicaldate |