Observational constraints on a phenomenological \(f\left( R,\partial R\right) \)
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- 作者：R. R. Cuzinatto (1)
C. A. M. de Melo (1) (2)
L. G. Medeiros (3)
P. J. Pompeia (4) (5)
1. Instituto de Ci锚ncia e Tecnologia ; Universidade Federal de Alfenas ; Rod. Jos茅 Aur茅lio Vilela (BR 267) ; km 533 ; no 11999 ; Po莽os de Caldas ; MG ; CEP 37701-970 ; Brazil
2. Instituto de F铆sica Te贸rica ; Universidade Estadual Paulista ; Rua Bento Teobaldo Ferraz 271 Bloco II ; P.O. Box 70532-2 ; S茫o Paulo ; SP ; CEP 01156-970 ; Brazil
3. Escola de Ci锚ncia e Tecnologia ; Departamento de F铆sica Te贸rica e Experimental ; Universidade Federal do Rio Grande do Norte ; Campus Universit谩rio ; s/n - Lagoa Nova ; Natal ; RN ; CEP 59078-970 ; Brazil
4. Instituto de Fomento e Coordena莽茫o Industrial ; Pra莽a Mal. Eduardo Gomes 50 ; S茫o Jos茅 dos Campos ; SP ; CEP 12228-901 ; Brazil
5. Instituto Tecnol贸gico de Aerona煤tica ; Pra莽a Mal. Eduardo Gomes 50 ; S茫o Jos茅 dos Campos ; SP ; CEP 12228-900 ; Brazil - 关键词：Modified gravity ; Dark energy ; Higher order gravity ; Cosmology
- 刊名：General Relativity and Gravitation
- 出版年：2015
- 出版时间：March 2015
- 年：2015
- 卷：47
- 期：3
- 全文大小：1,015 KB
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- 刊物主题：Physics
Mathematical and Computational Physics
Relativity and Cosmology
Differential Geometry
Quantum Physics
Astronomy, Astrophysics and Cosmology - 出版者：Springer Netherlands
- ISSN：1572-9532
文摘
This paper analyses the cosmological consequences of a modified theory of gravity whose action integral is built from a linear combination of the Ricci scalar \(R\) and a quadratic term in the covariant derivative of \(R\) . The resulting Friedmann equations are of the fifth-order in the Hubble function. These equations are solved numerically for a flat space section geometry and pressureless matter. The cosmological parameters of the higher-order model are fit using SN Ia data and X-ray gas mass fraction in galaxy clusters. The best-fit present-day \(t_{0}\) values for the deceleration parameter, jerk and snap are given. The coupling constant \(\beta \) of the model is not univocally determined by the data fit, but partially constrained by it. Density parameter \(\Omega _{m_0}\) is also determined and shows weak correlation with the other parameters. The model allows for two possible future scenarios: there may be either an eternal expansion or a Rebouncing event depending on the set of values in the space of parameters. The analysis towards the past performed with the best-fit parameters shows that the model is not able to accommodate a matter-dominated stage required to the formation of structure.