A Time-Dependent Λ and G Cosmological Model Consistent with Cosmological Constraints

Advances in Astronomy

Research Article

L. Kantha¹ 

[1] Department of Aerospace Engineering Sciences, University of Colorado Boulder, Boulder, CO 80309, USA, colorado.edu

Others  :  1236273
DOI  :  10.1155/2016/9743970

 received in 2016-01-19, accepted in 2016-05-08,  发布年份 2016

【 摘 要 】

The prevailing constant Λ-G cosmological model agrees with observational evidence including the observed red shift, Big Bang Nucleosynthesis (BBN), and the current rate of acceleration. It assumes that matter contributes 27% to the current density of the universe, with the rest (73%) coming from dark energy represented by the Einstein cosmological parameter Λ in the governing Friedmann-Robertson-Walker equations, derived from Einstein’s equations of general relativity. However, the principal problem is the extremely small value of the cosmological parameter (~10−52 m2). Moreover, the dark energy density represented by Λ is presumed to have remained unchanged as the universe expanded by 26 orders of magnitude. Attempts to overcome this deficiency often invoke a variable Λ-G model. Cosmic constraints from action principles require that either both G and Λ remain time-invariant or both vary in time. Here, we propose a variable Λ-G cosmological model consistent with the latest red shift data, the current acceleration rate, and BBN, provided the split between matter and dark energy is 18% and 82%. Λ decreases (Λ~τ-2, where τ is the normalized cosmic time) and G increases (G~τn) with cosmic time. The model results depend only on the chosen value of Λ at present and in the far future and not directly on G.

【 授权许可】

CC BY   
Copyright © 2016 L. Kantha. 2016

【 图 表 】

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【 参考文献 】

• [1]P. Langacker. (1981). Grand unified theories and proton decay. Physics Reports.72(4):185-385. DOI: 10.1016/0370-1573(81)90059-4.
• [2]N. Suzuki, D. Rubin, C. Lidman. (2012). The Hubble space telescope cluster supernova survey: V. Improving the dark-energy constraints above and Building an early-type-hosted supernova sample. The Astrophysics Journal.746(1, article 85). DOI: 10.1016/0370-1573(81)90059-4.
• [3]E. S. Abers, B. W. Lee. (1973). Gauge invariance in classical field theories. Physics Reports.9(1):6-13. DOI: 10.1016/0370-1573(81)90059-4.
• [4]P. Dirac. (1938). A new basis for cosmology. Proceedings of the Royal Society of London.165(921). DOI: 10.1016/0370-1573(81)90059-4.
• [5]P. A. Dirac. (1974). Cosmological models and the large numbers hypothesis. Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences.338(1615):439-446. DOI: 10.1016/0370-1573(81)90059-4.
• [6]C. P. Singh, A. Beesham. (2012). Particle creation in higher dimensional space-time with variable and Λ. International Journal of Theoretical Physics.51(12):3951-3962. DOI: 10.1016/0370-1573(81)90059-4.
• [7]C. P. Singh. (2006). Early universe with variable gravitational and cosmological constants. International Journal of Theoretical Physics.45(3):531-540. DOI: 10.1016/0370-1573(81)90059-4.
• [8]S. Ray, U. Mukhopadhyay, S. B. Choudhury. (2007). Dark energy models with a time-dependent gravitational constant. International Journal of Modern Physics. D. Gravitation, Astrophysics, Cosmology.16(11):1791-1802. DOI: 10.1016/0370-1573(81)90059-4.
• [9]R. Bali, M. Kumawat. (2009). -field cosmological models with variable in FRW space-time. International Journal of Theoretical Physics.48(12):3410-3415. DOI: 10.1016/0370-1573(81)90059-4.
• [10]J. Grande, J. Sola, I. L. Fabris, J. C. Shapiro. et al.(2010). Cosmic perturbations with running and. Classical Quantum Gravity.27(10):1-29. DOI: 10.1016/0370-1573(81)90059-4.
• [11]U. Mukhopadhyay, P. P. Ghosh, S. Ray. (2010). Higher dimensional dark energy investigation with variable and G. International Journal of Theoretical Physics.49(7):1622-1627. DOI: 10.1016/0370-1573(81)90059-4.
• [12]J. Grande, J. Solà, S. Basilakos, M. Plionis. et al.(2011). Hubble expansion and structure formation in the ‘running FLRW model’ of the cosmic evolution. Journal of Cosmology and Astroparticle Physics.2011(8, article 007):1-41. DOI: 10.1016/0370-1573(81)90059-4.
• [13]K. P. Singh, N. I. Singh. (2011). Viscous cosmological model with variable gravitational and cosmological constants. International Journal of Theoretical Physics.50(8):2486-2492. DOI: 10.1016/0370-1573(81)90059-4.
• [14]S. Ray, F. Rahaman, U. Mukhopadhyay, R. Sarkar. et al.(2011). Variable equation of state for generalized dark energy model. International Journal of Theoretical Physics.50(9):2687-2696. DOI: 10.1016/0370-1573(81)90059-4.
• [15]C. P. Singh. (2011). Cosmological models with time-varying gravitational and cosmological ‘constants’. Astrophysics and Space Science.331(1):337-342. DOI: 10.1016/0370-1573(81)90059-4.
• [16]C. P. Singh, A. Beesham. (2011). Early universe cosmology with particle creation: kinematics tests. Astrophysics and Space Science.336(2):469-477. DOI: 10.1016/0370-1573(81)90059-4.
• [17]M. Jamil, U. Debnath. (2011). FRW cosmology with variable and Λ. International Journal of Theoretical Physics.50(5):1602-1613. DOI: 10.1016/0370-1573(81)90059-4.
• [18]J. A. Belinchón. (2012). Bianchi I in scalar and scalar-tensor cosmologies. Central European Journal of Physics.10(4):789-798. DOI: 10.1016/0370-1573(81)90059-4.
• [19]E. Piedipalumbo, P. Scudellaro, G. Esposito, C. Rubano. et al.(2012). A matter-dominated cosmological model with variable G and and its confrontation with observational data. General Relativity and Gravitation.44(10):2477-2501. DOI: 10.1016/0370-1573(81)90059-4.
• [20]C. P. Singh, V. Singh. (2012). Power-law expansion and scalar field cosmology in higher derivative theory. International Journal of Theoretical Physics.51(6):1889-1900. DOI: 10.1016/0370-1573(81)90059-4.
• [21]S. D. Tade, M. M. Sambhe. (2012). Higher dimensional FRW cosmology with variable and Λ. International Journal of Theoretical Physics.51(2):447-454. DOI: 10.1016/0370-1573(81)90059-4.
• [22]L. Kantha. (2012). What if the gravitational constant G is not a true constant?. Physics Essays.25(2):282-289. DOI: 10.1016/0370-1573(81)90059-4.
• [23]E. L. D. Perico, J. A. S. Lima, S. Basilakos, J. Solà. et al.(2013). Complete cosmic history with a dynamical =(H) term. Physical Review D.88. DOI: 10.1016/0370-1573(81)90059-4.
• [24]J. Sadeghi, B. Pourhassan, M. Khurshudyan, H. Farahani. et al.(2014). Time-dependent density of modified cosmic chaplygin gas with variable cosmological constant in non-flat universe. International Journal of Theoretical Physics.53(3):911-920. DOI: 10.1016/0370-1573(81)90059-4.
• [25]A. Narimani, A. Moss, D. Scott. (2012). Dimensionless cosmology. Astrophysics and Space Science.341(2):617-629. DOI: 10.1016/0370-1573(81)90059-4.
• [26]K. D. Krori, S. Chaudhury, A. Mukherjee. (2000). Cosmologies with variable and Λ from action principle. General Relativity and Gravitation.32(8):1439-1447. DOI: 10.1016/0370-1573(81)90059-4.
• [27]P. G. Bergmann. (1968). Comments on the scalar-tensor theory. International Journal of Theoretical Physics.1(1):25-36. DOI: 10.1016/0370-1573(81)90059-4.
• [28]B. Boisseau, G. Esposito-Farèse, D. Polarski, A. A. Starobinsky. et al.(2000). Reconstruction of a scalar-tensor theory of gravity in an accelerating universe. Physical Review Letters.85(11):2236-2239. DOI: 10.1016/0370-1573(81)90059-4.
• [29]G. Esposito-Farèse, D. Polarski. (2001). Scalar-tensor gravity in an accelerating universe. Physical Review D.63(6)-20. DOI: 10.1016/0370-1573(81)90059-4.
• [30]A. Riazuelo, J.-P. Uzan. (2002). Cosmological observations in scalar-tensor quintessence. Physical Review D.66. DOI: 10.1016/0370-1573(81)90059-4.
• [31]G. F. R. Ellis, J.-P. Uzan. (2005). c is the speed of light, isn't it?. American Journal of Physics.73(3):240-247. DOI: 10.1016/0370-1573(81)90059-4.
• [32]R. R. Caldwell, R. Dave, P. J. Steinhardt. (1998). Cosmological imprint of an energy component with general equation of state. Physical Review Letters.80(8):1582-1585. DOI: 10.1016/0370-1573(81)90059-4.
• [33]D. N. Spergel, L. Verde, H. V. Peiris. (2003). First-year Wilkinson Microwave Anisotropy Probe (WMAP): observations: determination of cosmological parameters. The Astrophysical Journal.148(1, article 175). DOI: 10.1016/0370-1573(81)90059-4.
• [34]J. A. Frieman, M. S. Turner, D. Huterer. (2008). Dark energy and the accelerating universe. Annual Review of Astronomy and Astrophysics.46:385-432. DOI: 10.1016/0370-1573(81)90059-4.
• [35]G. Steigman. Light element nucleosynthesis. . DOI: 10.1016/0370-1573(81)90059-4.
• [36]G. Steigman. (2007). Primordial nucleosynthesis in the precision cosmology era. Annual Review of Nuclear and Particle Science.57:463-491. DOI: 10.1016/0370-1573(81)90059-4.
• [37]K. A. Olive, G. Steigman, T. P. Walker. (2000). Primordial nucleosynthesis: theory and observations. Physics Reports.333-334:389-407. DOI: 10.1016/0370-1573(81)90059-4.
• [38]N. Yoshida, T. Hosokawa, K. Omukai. (2012). Formation of the first stars in the universe. Progress in Theoretical and Experimental Physics. DOI: 10.1016/0370-1573(81)90059-4.