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Advances in High Energy Physics
Volume 2012 (2012), Article ID 357802, 12 pages
Modified Chaplygin Gas Cosmology
Mathematics and Natural Sciences Department, Prince Mohammad Bin Fahd University, Al-Khobar 31952, Saudi Arabia
Received 25 May 2012; Revised 30 September 2012; Accepted 14 October 2012
Academic Editor: Vlad Popa
Copyright © 2012 H. B. Benaoum. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Modified Chaplygin gas as an exotic fluid has been introduced by H. B. Benaoum (2002). Essential features of the modified Chaplygin gas as a cosmological model are discussed. Observational constraints on the parameters of the model have been included. The relationship between the modified Chaplygin gas and a homogeneous minimally coupled scalar field is reevaluated by constructing its self-interacting potential. In addition, we study the role of the tachyonic field in the modified Chaplygin gas cosmological model and the mapping between scalar field and tachyonic field is also considered.
Astronomical and cosmological observations, such as type Ia supernovae (SNe Ia) [1–4], large-scale redshift surveys structure (LSS) [5, 6], the cosmic microwave background (CMB) [7, 8], and Wilkinson Microwave Anisotropy Probe (WMAP) [9, 10], indicate that the observable universe experiences an accelerated expansion. These observations suggest also that the universe is nearly flat and dominated by a nonbaryonic substratum. The source of this acceleration is usually attributed to an exotic type of fluid with negative pressure called commonly dark energy.
Various kinds of dark energy models have been proposed such as cosmological constant , quintessence [12–14], -essence [15–17], tachyon [18–20], phantom [21–23], Chaplygin gas , quintom , holographic dark energy , and extra dimensions . The nature of the dark sector of the universe (i.e., dark energy and dark matter) remains a mystery. An economical and attractive idea to unify the dark sector of the universe is to consider it as a single component that acts as both dark energy and dark matter. One way to achieve the unification of dark energy and dark matter is by using the so-called Chaplygin gas. The pure Chaplygin gas or generalized Chaplygin gas is a perfect fluid which behaves like a pressureless fluid at an early stage and a cosmological constant at a later stage.
Pure Chaplygin gas with an exotic equation of state is characterized by a negative pressure , where is the pressure, is the energy density, and is a positive parameter.
The pure Chaplygin gas has been extended to the so-called generalized Chaplygin gas with the following equation of state : It is clear that the pure Chaplygin gas is recovered for the case .
The interesting feature of the Chaplygin gas is its connection to the string theory. It can be obtained from the Nambu-Goto action for a -brane moving in a ()-dimensional spacetime in the light cone parametrization [29–33].
The outline of this paper is as follows. In the next section, we study the cosmological model of the modified Chaplygin gas which was introduced by the author in . We show that the modified Chaplygin gas model interpolates between an epoch with a soft equation of state and a de Sitter phase. In Section 3, the relationships between the modified Chaplygin gas and a cosmological scalar field are reevaluated. In Section 4, a tachyonic field is considered as a candidate for the modified Chaplygin gas model. The correspondence between minimally coupled scalar field and the tachyon field is also investigated.
2. FRW Cosmology from the Modified Chaplygin Gas Model
Within the framework of Friedmann-Robertson-Walker (FRW) cosmology, a model called modified Chaplygin gas has been proposed by the author . This model includes an initial phase of radiation and it is based on the following equation of state: where , and are constant parameters.
When , we recover the equation of state of perfect fluid, that is, . For , it reduces to the generalized Chaplygin gas.
In (2.1), the two terms start to be of the same order when the pressure vanishes (i.e., . In this case, the fluid has pressureless density , corresponding to some scale factor , The metric of -dimensional FRW spacetime is where is the scale factor and is the metric of the maximally symmetric -space with curvature .
The Friedmann equation which governs the evolution of the scale factor is given by where is the Hubble parameter.
In the FRW framework, a fluid with an energy density and a pressure must satisfy the conservation law:
The latter two equations imply that
By defining and a rescaled density , (2.5) becomes This equation can be easily integrated leading to where is an integration constant.
The density will be The constant of integration can be expressed in terms of the cosmological scale , (i.e.,) where the fluid has a vanishing pressure: The energy density will be where .
For large-scale factor , that is, , we have which correspond to an empty universe with a cosmological constant (i.e., a de Sitter space).
Also for small-scale factor , that is, , we have which correspond to universe dominated by an equation of state . This shows that this model interpolates between a universe dominated by matter phase with equation of state and a de Sitter phase .
Moreover, expanding (2.11) and (2.1) to the subleading terms at large cosmological constant, we obtain the following expressions for the energy and the pressure: These correspond to the mixture of a cosmological constant and a type of matter described by an equation of state: The equation of state parameter takes the form: which ranges over , depending on the cosmological scale , The speed of sound is defined as Now by computing , we obtain which for the modified Chaplygin gas gives the following expression for the speed of sound: implying that is always positive and hence there is no concern about imaginary speed of sound.
Moreover, it has the following asymptotic limit, The speed of sound never exceeds that of light for smaller-scale or scale of the order of where the pressure vanishes, provided that and will exceed it for large scale compared to .
The constraints from the astrophysical and cosmological observables on the modified Chaplygin gas have been studied by many authors [35–40]. The permissible values of the parameters , and have been explored from the observed data.
Using data from different observations, namely, observational Hubble Data (OHD), baryon acoustic oscillation (BAO), and CMB shift parameters data, the allowed values for some of the parameters of the modified Chaplygin gas have been extracted. In the light of the 182 Gold SNe Ia, the 3-year WMAP and the SDSS data, the best fits correspond to and . This result was obtained by decomposing the modified Chaplygin gas into two components, that is, dark matter and dark energy component.
However, by using Markov chain Monte Carlo method with the observational data from the SN Ia Union 2, OHD, cluster X-ray gas mass fraction (CBF), BAO, and CMB data, the best fits of the modified Chaplygin gas parameters give and .
Moreover, a perturbative analysis of the modified Chaplygin gas shows that the power spectrum observational data restricts the value of  such that the modified Chaplygin gas is disfavored.
3. Modified Chaplygin Gas as a Scalar Field
Following [41–45], we describe the modified Chaplygin gas cosmological model by introducing a scalar fields having a self-interacting potential with the Lagrangian: Both the energy density and the pressure of the modified Chaplygin gas can be related to the scalar through the following transformation equations: The kinetic energy of the scalar field and its corresponding potential are where .
Now since where the prime denotes derivation with respect to and , we get Here, we have used (2.4) for the Hubble constant and guided by the cosmic microwave background CMB data which is strongly consistent with a flat universe and restricted ourselves to the flat case .
By using (2.16), we get The first equation can be integrated easily which gives where and .
We note that for larger scales, the scalar field asymptotically approaches to the constant field and becomes infinite (i.e., ) for small scales.
Next, by substituting the latter expression in (3.2), we can write all our physical quantities , and in terms of the scalar field as Notice that these physical quantities do not depend on the intermediate constant (i.e., constant of integration .
Finally, we get the following potential which has a simple form:
4. Modified Chaplygin Gas as Tachyonic Field
The importance of tachyon in cosmology is inspired by string theory [18, 19]. The action of the homogeneous tachyon condensate of string theory in a gravitational background is given by where is the scalar curvature. For a tachyonic field with tachyonic potential , the relativistic Lagrangian can be expressed as The corresponding energy-momentum tensor for the tachyonic field is where the velocity is with .
It follows that the energy density and the pressure of the tachyonic field are given by The equation of state parameter is The condition of accelerating universe (i.e.,) requires that and the rolling tachyon has an interesting equation of state whose parameter interpolates between and .
The evolution of the tachyonic field is driven by with the constraint equation for the Hubble parameter given by By combining the last two equations, the tachyonic field and the potential can be expressed as Note that the knowledge of and (i.e., cosmological scale factor ) completely determines the tachyonic field and its corresponding potential .
By mapping the pressure and the energy density for the scalar field with the corresponding tachyon field and , we obtain that Cosmological correspondence between the tachyonic field and a minimally coupled scalar field has been noted by [34, 46]. Such correspondence was also investigated by  where it was demonstrated explicitly that distinct scalar field and tachyonic models may give rise to the same cosmological evolution for a particular choice of initial conditions.
Now by using (3.7), an exact integration to the first equation in (4.11) can be performed without any approximation as follows: where is the hypergeometric function given by with as the Pochhammer symbol.
To find the scalar field and its potential in terms of the tachyon field and its potential , one has to perform the inverse transformation:
In the slow-rolling approximation, the tachyon field potential and the scalar field potential are approximately the same. To see this, we expand (4.10) up to the first order in and use (2.4) and (2.6) to get: Now to rewrite the potential in terms of , we first expand (4.14) to the first order in : and then substitute it in (4.16) to finally get: where and are constant parameters depending on , and .
One approach in modern cosmology consists in supposing that dark energy and dark matter are different manifestations of a single entity. Following such an idea, this work (see also ) presents a cosmological model based on the modified Chaplygin gas that acts as a single component. It is shown that the equation of state of the modified Chaplygin gas interpolates from matter-dominated era to a cosmological constant-dominated era. Astronomical and cosmological constraints on the parameters , and of the modified Chaplygin have been investigated and still no basic agreement is reached on their values.
In addition, from the theoretical point of view, the modified Chaplygin gas model is equivalent to that of a scalar field having self-interacting potential . Such a description has been explored and its self-interacting potential has been determined.
Furthermore, it has been shown that the modified Chaplygin gas can also be described by a tachyonic field having a potential . Correspondence between scalar field and tachyonic field descriptions has been investigated. The transformations between the scalar field and tachyonic field and between their corresponding potentials have been determined. Such a correspondence has been applied to derive the exact expression of the tachyonic field in terms of the scalar field for the modified Chaplygin gas. Finally, in the slow-rolling approximation, we have expressed the the potential in terms of the tachyonic field .
The author would like to express his gratitude to the anonymous referees for very helpful and detailed comments.
- 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.
- 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.
- 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.
- A. G. Riess, L.-G. Sirolger, J. Tonry et al., “Type Ia supernova discoveries at z > 1 from the hubble space telescope: evidence for past deceleration and constraints on dark energy evolution,” Astrophysical Journal Letters, vol. 607, no. 2, pp. 665–687, 2004.
- 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.
- 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.
- 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.
- 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.
- 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.
- 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.
- 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.
- B. Ratra and P. J. E. Peebles, “Cosmological consequences of a rolling homogeneous scalar field,” Physical Review D, vol. 37, p. 3406, 1988.
- 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.
- 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.
- C. Armendariz-Picon and V. Mukhanov, “Essentials of k-essence,” Physical Review D, vol. 63, no. 10, Article ID 103510, 10 pages, 2001.
- T. Chiba, “Tracking k-essence,” Physical Review D, vol. 66, no. 6, Article ID 063514, 4 pages, 2002.
- R. J. Scherrer, “Purely kinetic k essence as unified dark matter,” Physical Review Letters, vol. 93, no. 1, Article ID 011301, 1 pages, 2004.
- A. Sen, “Rolling tachyon,” Journal of High Energy Physics, vol. 04, article 048, 2002.
- A. Sen, “Time evolution in open string theory,” Journal of High Energy Physics, vol. 07, article 065, 2002.
- G. W. Gibbons, “Cosmological evolution of the rolling tachyon,” Physics Letters B, vol. 537, no. 1-2, pp. 1–4, 2002.
- 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.
- 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.
- 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.
- A. Kamenshchik, U. Moschella, and V. Pasquier, “An alternative to quintessence,” Physics Letters, Section B, vol. 511, no. 2–4, pp. 265–268, 2001.
- 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.
- P. Hořava and D. Minic, “Probable values of the cosmological constant in a holographic theory,” Physical Review Letters, vol. 85, no. 8, pp. 1610–1613, 2000.
- 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.
- M. C. Bento, O. Bertolami, and A. A. Sen, “The Revival of the unified dark energy—dark matter model?” Physical Review D, vol. 70, Article ID 083519, 2004.
- J. C. Fabris, S. V. B. Gonçalves, and P. E. De Souza, “Density perturbations in a universe dominated by the Chaplygin gas,” General Relativity and Gravitation, vol. 34, no. 1, pp. 53–63, 2002.
- N. Bili, G. B. Tupper, and R. D. Viollier, “Unification of dark matter and dark energy: the inhomogeneous Chaplygin gas,” Physics Letters, Section B, vol. 535, no. 1–4, pp. 17–21, 2002.
- A. Hayashigaki, “Chaplygin-like gas and branes in black hole bulks,” Physics Letters, Section B, vol. 487, no. 1-2, pp. 7–13, 2000.
- R. Jackiw, “A particle field theorist’s lectures on supersymmetric, non-Abelian fluid mechanics and d-branes,” http://arxiv.org/abs/physics/0010042.
- N. Ogawa, “Remark on the classical solution of the Chaplygin gas as d-branes,” Physical Review D, vol. 62, no. 8, Article ID 085023, 8 pages, 2000.
- H. B. Benaoum, “Accelerated universe from modified chaplygin gas and tachyonic fluid,” http://arxiv.org/abs/hep-th/0205140.
- J. Lu, L. Xu, J. Li, B. Chang, Y. Gui, and H. Liu, “Constraints on modified Chaplygin gas from recent observations and a comparison of its status with other models,” Physics Letters, Section B, vol. 662, no. 2, pp. 87–91, 2008.
- J. Lu, L. Xu, Y. Wu, and M. Liu, “Combined constraints on modified Chaplygin gas model from cosmological observed data: markov Chain Monte Carlo approach,” General Relativity and Gravitation, vol. 43, no. 3, pp. 819–832, 2011.
- L. Xu, Y. Wang, and H. Noh, “Modified Chaplygin gas as a unified dark matter and dark energy model and cosmic constraints,” European Physical Journal C, vol. 72, no. 3, article 1931, 2012.
- P. Thakur, S. Ghose, and B. C. Paul, “Modified Chaplygin gas and constraints on its B parameter from cold dark matter and unified dark matter energy cosmological models,” Monthly Notices of the Royal Astronomical Society, vol. 397, no. 4, pp. 1935–1939, 2009.
- B. C. Paul, P. Thakur, and A. Saha, “Modified Chaplygin gas in Horava-Lifshitz gravity and constraints on its B parameter,” Physical Review D, vol. 85, no. 2, Article ID 024039, 9 pages, 2012.
- J. C. Fabris, H. E. S. Velten, C. Ogouyandjou, and J. Tossa, “Ruling out the Modified Chaplygin Gas cosmologies,” Physics Letters, Section B, vol. 694, no. 4-5, pp. 289–293, 2011.
- J. D. Barrow, “Graduated inflationary universes,” Physics Letters B, vol. 235, no. 1-2, pp. 40–43, 1990.
- J. D. Barrow and P. Saich, “Scalar-field cosmologies,” Classical and Quantum Gravity, vol. 10, no. 2, pp. 279–283, 1993.
- A. A. Starobinsky, “How to determine an effective potential for a variable cosmological term,” JETP Letters, vol. 68, no. 10, pp. 757–763, 1998.
- D. Huterer and M. S. Turner, “Prospects for probing the dark energy via supernova distance measurements,” Physical Review D, vol. 60, no. 8, Article ID 081301, 5 pages, 1999.
- T. Nakamura and T. Chiba, “Determining the equation of state of the expanding Universe: inverse problem in cosmology,” Monthly Notices of the Royal Astronomical Society, vol. 306, no. 3, pp. 696–700, 1999.
- T. Padmanabhan, “Accelerated expansion of the universe driven by tachyonic matter,” Physical Review D, vol. 66, no. 2, Article ID 021301, 4 pages, 2002.
- V. Gorini, A. Kamenshchik, U. Moschella, and V. Pasquier, “Tachyons, scalar fields, and cosmology,” Physical Review D, vol. 69, no. 12, Article ID 123512, 16 pages, 2004.