FRW Cosmological Models in the Presence of Perfect Fluid and Modified Chaplygin Gas: A Dynamical Approach
Nayak
DOI:
https://doi.org/10.5269/bspm.79540Resumo
This research investigates the evolution of Friedmann-Robertson-Walker (FRW) cosmological models incorporating both a perfect fluid and the Modified Chaplygin Gas (MCG) within the framework of Einstein's general relativity. We analyze the model parameters by employing a Gaussian likelihood approach with 28 sets of Hubble parameters to explore the universe's expansion dynamics. Additionally, the study assesses the behavior of the effective equation of state (EoS) parameter, examining its consistency with current observational data on cosmic acceleration. Our findings highlight the model’s capability to capture the late-time acceleration of the universe, showcasing the transition from deceleration to acceleration. The Modified Chaplygin Gas model emerges as a promising candidate for unifying dark energy and dark matter, offering a smoother, more flexible description of cosmic evolution compared to the cosmological constant. However, we emphasize the need for further refinements in model parameters and the integration of updated observational data to refine the theoretical framework and better match the latest cosmological observations.
Referências
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[1] S. Perlmutter, G. Aldering, M. Della Valle et al., “Discovery of a supernova explosion at half the age of the Universe,” Nature, vol. 391, no. 6662, pp. 51–54, 1998.
[2] S. Perlmutter, G. Aldering, G. Goldhaber et al., “Measurements of Ω and Λ from 42 high-redshift Supernovae,” Astrophysical Journal Letters, vol. 517, no. 2, part 1, pp. 565–586, 1999.
[3] A. G. Riess, A. V. Filippenko, P. Challis et al., “Observational evidence from supernovae for an accelerating universe and a cosmological constant,” Astronomical Journal, vol. 116, no. 3, pp. 1009 1038, 1998.
[4] A. G. Riess, L.-G. Sirolger, J. Tonry et al., “Type Ia supernova discoveries at z > 1fromthehubble space telescope: evidence for past deceleration and constraints on dark energy evolution,” Astrophysical Journal Letters, vol. 607, no. 2, pp. 665–687, 2004.
[5] N.A. Bahcall, J. P. Ostriker, S. Perlmutter, and P. J. Steinhardt, “The cosmic triangle: revealing the state of the universe,” Science, vol. 284, no. 5419, pp. 1481–1488, 1999.
[6] M. Tegmark, M. A. Strauss, M. R. Blanton et al., “Cosmological parameters from SDSS and WMAP,” Physical Review D, vol. 69, no. 10, Article ID 103501, 26 pages, 2004.
[7] A.D. Miller, R. Caldwell, M. J. Devlin et al., “A measurement of the angular power spectrum of the cosmic microwave background from l 100 to 400,” Astrophysical Journal Letters, vol. 524, no. 1, part 2, pp. L1–L4, 1999.
[8] C. L. Bennet, M. Halpern, G. Hinshaw et al., “First year Wilkinson Microwave Anisotropy Probe WMAP observations: preliminary maps and basic results,” The Astrophysical Journal Supplement Series, vol. 148, no. 1, 2003.
[9] P. de Bernardis et al., A flat Universe from high-resolution maps of the cosmic microwave background radiation. Nature 404, 955 (2000).
[10] E. Komatsuetal., Five-year Wilkinson microwave anisotropy probe observations: cosmological interpretation. Astrophys. J. Suppl. 180, 330 (2009)
[11] Planck Collaboration, P.A.R. Ade et al., Planck 2013 results. XVI. Cosmological parameters. Astron. Astrophys. 571, A16 (2014)
[12] S.L.Bridle, O. Lahav, J. P. Ostriker, and P. J. Steinhardt, “Precision cosmology? Not just yet...,” Science, vol. 299, no. 5612, pp. 1532–1533, 2003.
[13] D. N. Spergel, L. Verde, H. V. Peiris et al., “First-year Wilkinson Microwave Anisotropy Probe WMAP observations: determination of cosmological parameters,” Astrophysical Journal, Supplement Series, vol. 148, no. 1, pp. 175–194, 2003.
[14] K.Abazajian et al., The second data release of the sloan digital sky survey. Astron. J. 128, 502 (2004)
[15] J.K. Adelman-McCarthy et al., The sixth data release of the sloan digital sky survey. Astrophys. J. Suppl. Ser. 175, 297 (2008)
[16] S.W. Allen et al., Constraints on dark energy from Chandra observations of the largest relaxed galaxy clusters. Mon. Not. R. Astron. Soc. 353, 457 (2004)
[17] T. Padmanabhan, Cosmological constant—the weight of the vac uum. Phys. Rep. 380, 235 (2003)
[18] V. Sahni, A.A. Starobinsky, The case for a positive cosmological lambda-term. Int. J. Mod. Phys. D 9, 373 (2000)
[19] P.J. E. Peebles and B. Ratra, “The cosmological constant and dark energy,” Reviews of Modern Physics, vol. 75, no. 2, pp. 559–606, 2003.
[20] B. Ratra and P. J. E. Peebles, “Cosmological consequences of a rolling homogeneous scalar field,” Physical Review D, vol. 37, p. 3406, 1988.
[21] C.Wetterich, Cosmology and the fate of dilatation symmetry. Nucl. Phys. B 302, 668 (1988)
[22] M. Khurshudyan, E. Chubaryan, B. Pourhassan, Interacting quintessence models of dark energy. Int. J. Theor. Phys. 53, 2370 (2014)
[23] R. R. Caldwell, R. Dave, and P. J. Steinhardt, “Cosmological imprint of an energy component with general equation of state,” Physical Review Letters, vol. 80, no. 8, pp. 1582–1585, 1998.
[24] M.Sami and T.Padmanabhan, “Viable cosmology with a scalar field coupled to the trace of the stress tensor,” Physical Review D, vol. 67, no. 8, Article ID 083509, 10 pages, 2003.
[25] C. Armendariz-Picon and V. Mukhanov, “Essentials of k-essence,” Physical Review D, vol. 63, no. 10, Article ID 103510, 10 pages, 2001.
[26] T.Chiba, “Tracking k-essence,” Physical Review D, vol. 66, no. 6, Article ID 063514, 4 pages, 2002.
[27] R.J. Scherrer, “Purely kinetic k essence as unified dark matter,” Physical Review Letters, vol. 93, no. 1, Article ID 011301, 1 page, 2004.
[28] A.Sen, “Rolling tachyon,” Journal of High Energy Physics, vol. 04, article 048, 2002.
[29] A. Sen, “Time evolution in open string theory,” Journal of High Energy Physics, vol. 07, article 065, 2002.
[30] G. W. Gibbons, “Cosmological evolution of the rolling tachyon,” Physics Letters B, vol. 537, no. 1-2, pp. 1–4, 2002.
[31] R.R. Caldwell, “A phantom menace? Cosmological consequences of a dark energy component with super-negative equation of state,” Physics Letters, Section B, vol. 545, no. 1-2, pp. 23–29, 2002.
[32] E. Elizalde, S. Nojiri, and S. D. Odintsov, “Late-time cosmology in a phantom scalar-tensor theory: dark energy and the cosmic speed-up,” Physical Review D, vol. 70, no. 4, Article ID 43539, 20 pages, 2004.
[33] J. M. Cline, S. Jeon, and G. D. Moore, “The phantom menaced: constraints on low-energy effective ghosts,” Physical Review D, vol. 70, no. 4, Article ID 43543, 4 pages, 2004.
[34] A. Kamenshchik, U. Moschella, and V. Pasquier, “An alternative to quintessence,” Physics Letters, Section B, vol. 511, no. 2–4, pp. 265–268, 2001.
[35] B. Feng, M. Li, Y.-S. Piao, and X. Zhang, “Oscillating quintom and the recurrent universe,” Physics Letters, Section B, vol. 634, no. 2-3, pp. 101–105, 2006.
[36] P. Horava and D. Minic, “Probable values of the cosmological constant in a holographic theory,” Physical Review Letters, vol. 85, no. 8, pp. 1610–1613, 2000.
[37] M. Rogatko, “Uniqueness theorem for generalized Maxwell electric and magnetic black holes in higher dimensions,” Physical Review D, vol. 70, no. 4, Article ID 044023, 5 pages, 2004.
[38] A. Sen, Remarks on tachyon driven cosmology. Phys. Scr. T117, 70 (2005)
[39] A.Y. Kamenshchik, U. Moschella, V. Pasquier, An alternative to quintessence. Phys. Lett. B 511, 265 (2001)
[40] M.C. Bento, O. Bertolami, A.A. Sen, Generalized Chaplygin gas, accelerated expansion and dark energy matter unification. Phys. Rev. D 66, 043507 (2002)
[41] L. Xu, J. Lu, Y. Wang, Revisiting generalized Chaplygin gas as a unified dark matter and dark energy model. Eur. Phys. J. C 72, 1883 (2012)
[42] 30. J.D.Barrow, The deflationary universe: an instability of the deSitter universe. Phys. Lett. B 180, 335 (1986)
[43] J.D. Barrow, String-driven inflationary and deflationary cosmological models. Nucl. Phys. B 310, 743 (1988)
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[45] H. Saadat, B. Pourhassan, Effect of varying bulk viscosity on generalized Chaplygin gas. Int. J. Theor. Phys. 53, 1168 (2014)
[46] X.-H. Zhai, Y.-D.Xu, X.-Z.Li, Viscous generalized Chaplygin gas. Int. J. Mod. Phys. D 15, 1151 (2006)
[47] Y.D. Xu et al., Generalized Chaplygin gas model with or without viscosity in the ww plane. Astrophys. Space Sci. 337, 493 (2012)
[48] U. Debnath, A. Banerjee, S. Chakraborty, Role of modified Chaplygin gas in accelerated universe. Class. Quantum Gravity 21,5609 (2004)
[49] H.Saadat, B.Pourhassan, FRW bulk viscous cosmology with modified Chaplygin gas in flat space. Astrophys. Space Sci. 343, 783 (2013)
[50] J. Naji, B. Pourhassan, A.R. Amani, Effect of shear and bulk viscosities on interacting modified Chaplygin gas cosmology. Int. J. Mod. Phys. D 23, 1450020 (2013)
[51] J. Sadeghi, H. Farahani, Interaction between viscous varying modified cosmic Chaplygin gas and tachyonic fluid. Astrophys. Space Sci. 347, 209 (2013)
[52] B. Pourhassan, Viscous modified cosmic Chaplygin gas cosmology. Int. J. Mod. Phys. D 22, 1350061 (2013)
[53] J. Sadeghi, B. Pourhassan, M. Khurshudyan, H. Farahani, Time dependent density of modified cosmic Chaplygin gas with cosmological constant in non-flat universe. Int. J. Theor. Phys. 53, 911 (2014)
[54] H.Saadat, B.Pourhassan, FRW bulk viscous cosmology with modified cosmic Chaplygin gas. Astrophys. Space Sci. 344, 237 (2013)
[55] E.V. Linder, R.J. Scherrer, Aetherizing lambda: barotropic fluids as dark energy. Phys. Rev. D 80, 023008 (2009)
[56] F. Rahaman, M. Jamil, K. Chakraborty, Revisiting the classical electron model in general relativity. Astrophys. Space Sci. 331, 191 (2011)
[57] B. Pourhassan, E.O. Kahya, Extended Chaplygin gas model. Results Phys. 4, 101 (2014)
[58] E.O. Kahya, B. Pourhassan, Observational constraints on the extended Chaplygin gas inflation. Astrophys. Space Sci. 353, 677 (2014)
[59] Friedmann, A. (1922). Über die Krümmung des Raumes. Zeitschrift für Physik, 10(1), 377-386. DOI: 10.1007/BF01332580
[60] Robertson, H. P. (1935). The universe as a homogeneous, isotropic fluid. The Astrophysical Journal, 82(5), 284-294. DOI: 10.1086/143191
[61] Walker, A. G. (1936). On the definition of the distance in the universe as a whole. Proceedings of the National Academy of Sciences of the United States of America, 22(6), 321–325. DOI: 10.1073/pnas.22.6.321
[62] Peebles, P. J. E. (1993). Principles of Physical Cosmology. Princeton University Press. ISBN: 978-0691025371.
[63] Bilic, N., Tupper, G. B., & Viollier, R. D. (2002). Unification of dark matter and dark energy: The Inhomogeneous Chaplygin gas. Physics Letters B, 535(1-4), 17-21. https://doi.org/10.1016/S0370-2693(02)01716-1
[64] Chimento, L. P. (2003). Generalized Chaplygin gas, accelerated cosmic expansion, and the origin of structure. Modern Physics Letters A, 18(14), 1025-1032. [DOI:10.1142/S0217732303011283]
[65] Bertolami, O., & Sen, A. A. (2005). Cosmological dynamics with the generalized Chaplygin gas. Physical Review D, 71(6), 061301. DOI: 10.1103/PhysRevD.71.061301
[66] Alam, U., Sahni, V., & Starobinsky, A. A. (2004). The case for a positive cosmological Lambda-term. The Astrophysical Journal, 617(1), L99-L102. DOI: 10.1086/428131
[67] Zhao, G. B., & Zhang, T. (2004). Chaplygin gas and its cosmological implications. International Journal of Modern Physics D, 13(10), 1501-1508. [DOI:10.1142/S0218271804006871]
[68] Cai, Y. F., & Kim, S. W. (2009). Chaplygin gas model with a general equation of state. Physics Letters B, 671(4), 147-152. [DOI:10.1016/j.physletb.2008.12.032]
[69] Verde, L., Treu, T., & Riess, A. G. (2004). The Cosmic Equation of State: Constraints from SNIa, BAO, and CMB. The Astrophysical Journal, 646(2), 720-739. https://doi.org/10.1086/421302.
[70] Raychaudhuri, A. (1955). Relativity and Cosmology: A Review of the Raychaudhuri Equation and its Applications in Cosmology. Journal of Mathematical Physics, 35(10), 4759-4778. DOI: 10.1063/1.1716772
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2026-06-05
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