Abstract
Motivated by some previous works of Rudra et al. we set to explore the background dynamics when dark energy in the form of New Variable Modified Chaplygin gas is coupled to dark matter with a suitable interaction in the universe described by brane cosmology. The main idea is to find out the efficiency of New variable modified Chaplygin gas to play the role of DE. As a result we resort to the technique of comparison with standard dark energy models. Here the RSII brane model have been considered as the gravity theory. An interacting model is considered in order to search for a possible solution of the cosmic coincidence problem. A dynamical system analysis is performed because of the high complexity of the system. The statefinder parameters are also calculated to classify the dark energy model. Graphs and phase diagrams are drawn to study the variations of these parameters and get an insight into the effectiveness of the dark energy model. It is also seen that the background dynamics of New Variable Modified Chaplygin gas is consistent with the late cosmic acceleration. After performing an extensive mathematical analysis, we are able to constrain the parameters of new variable modified Chaplygin gas as m<n to produce the best possible results. Future singularities are studied and it is found that the model has a tendency to result in such singularities unlike the case of generalized cosmic Chaplygin gas. Our investigation leads us to the fact that New Variable Modified Chaplygin gas is not as effective as other Chaplygin gas models to play the role of dark energy.
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Notes
In the presence of a scalar field the transition from a universe filled with matter to an exponentially expanding universe is justified.
References
Alam, U., Sahni, V., Saini, T.D., Starobinsky, A.A.: Mon. Not. R. Astron. Soc. 344, 1057 (2003)
Alcaniz, J.S., Lima, J.A.S.: Phys. Rev. D 72, 063516 (2005)
Barreiro, T., Sen, A.A.: Phys. Rev. D 70, 124013 (2004)
Bento, M.C., Bertolami, O., Sen, A.A.: Phys. Rev. D 66, 043507 (2002)
Berger, M.S., Shojae, H.: Phys. Rev. D 73, 083528 (2006). arXiv:gr-qc/0601086
Brax, P., et al.: Rep. Prog. Phys. 67, 2183 (2004). arXiv:hep-th/0404011
Caldwell, R.R., Kamiokowsky, M., Weinberg, N.N.: Phys. Rev. Lett. 91, 071301 (2003)
Carturan, D., Finelli, F.: Phys. Rev. D 68, 103501 (2003)
Chakraborty, W., Debnath, U.: Gravit. Cosmol. 16, 223 (2010)
Chowdhury, R., Rudra, P.: Int. J. Theor. Phys. 52, 489 (2013)
Dalal, N., Abazajian, K., Jenkins, E., Manohar, A.V.: Phys. Rev. Lett. 87, 141302 (2001). arXiv:astro-ph/0105317v1
Debnath, U.: Astrophys. Space Sci. 312, 295299 (2007)
Debnath, U., Banerjee, A., Chakraborty, S.: Class. Quantum Gravity 21, 5609 (2004)
del Campo, S., Herrera, R., Pavon, D.: J. Cosmol. Astropart. Phys. 0901, 020 (2009). arXiv:0812.2210 [gr-qc]
Feng, C., et al.: Phys. Lett. B 665, 111 (2008)
González-Diaz, P.F.: Phys. Rev. D 68, 021303(R) (2003)
Gorini, V., Kamenshchik, A., Moschella, U.: Phys. Rev. D 67, 063509 (2003)
Gorini, V., Kamenshchik, A., Moschella, U., Pasquier, V.: arXiv:gr-qc/0403062 (2004)
Guo, Z.-K., Zhang, Y.-Z.: Phys. Rev. D 71, 023501 (2005)
Hu, B., Ling, Y.: Phys. Rev. D 73, 123510 (2006)
Jamil, M., Saridakis, E.N., Setare, M.R.: Phys. Rev. D 81, 023007 (2010)
Jamil, M., Momeni, D., Rashid, M.A.: Eur. Phys. J. C 71, 1711 (2011). arXiv:1107.1558v1 [physics.gen-ph]
Kamenshchik, A., Moschella, U., Pasquier, V.: Phys. Lett. B 511, 265 (2001)
Maartens, R.: Living Rev. Relativ. 7, 7 (2004). arXiv:gr-qc/0312059
Maeda, K., Wands, D.: Phys. Rev. D 62, 124009 (2000)
Nojiri, S., Odintsov, S.D.: Phys. Rev. D 70, 103522 (2004)
Nojiri, S., Oditsov, S.D.: Phys. Rep. 505, 59 (2011)
Nojiri, S., Oditsov, S.D., Tsujikawa, S.: Phys. Rev. D 71, 063004 (2005)
Perlmutter, S., et al. (Supernova Cosmology Project Collaboration): Astrophys. J. 517, 565 (1999). arXiv:astro-ph/9812133
Randall, L., Sundrum, R.: Phys. Rev. Lett. 83, 3770 (1999a)
Randall, L., Sundrum, R.: Phys. Rev. Lett. 83, 4690 (1999b)
Riess, A.G., et al. (Supernova Search Team Collaboration): Astrophys. J. 607, 665 (2004). arXiv:astro-ph/0402512
Rubakov, V.A.: Phys. Usp. 44, 871 (2001). arXiv:hep-th/0104152
Rudra, P.: Astrophys. Space Sci. 342, 579 (2012)
Rudra, P., Debnath, U., Biswas, R.: Astrophys. Space Sci. 339, 53 (2012). arXiv:1109.1481 [gr-qc]
Sahni, V., et al.: J. Exp. Theor. Phys. 77, 201 (2003)
Sasaki, M., Shiromizu, T., Maeda, K.: Phys. Rev. D 62, 024008 (2000)
Setare, M.R.: Phys. Lett. B 642, 1 (2006)
Setare, M.R.: Eur. Phys. J. C 50, 991 (2007)
Shiromizu, T., Maeda, K., Sasaki, M.: Phys. Rev. D 62, 024012 (2000)
Spergel, D.N., et al. (WMAP Collaboration): Astron. Astrophys. Suppl. Ser. 148, 175 (2003). arXiv:astro-ph/0302209
Wu, P., Yu, H.: Class. Quantum Gravity 24, 4661 (2007)
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The authors sincerely acknowledge the facilities provided by the Inter-University Centre for Astronomy and Astrophysics (IUCAA), Pune, India where a part of the work was carried out.
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Rudra, P., Ranjit, C. & Kundu, S. How effective is new variable modified Chaplygin gas to play the role of dark energy—a dynamical system analysis in RS II brane model. Astrophys Space Sci 347, 433–444 (2013). https://doi.org/10.1007/s10509-013-1531-1
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DOI: https://doi.org/10.1007/s10509-013-1531-1