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Tphysicsletters/4587/890/Dark matter and radiation production during warm inflation in a curved universe-an irreversible thermodynamic approach
Monday, March 13, 2023 at 6:30:00 AM UTC
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PTL LOCKED
Dark matter and radiation production during warm inflation in a curved universe-an irreversible thermodynamic approach
TEODORA MATEI
Theoretical Physics Letters
2023 ° 01(01) ° 987.-6986
https://www.wikipt.org/tphysicsletters
DOI: 10.1490/6987750.433tpl
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Abstract
We investigate the creation of dark matter particles as a result of the decay of the scalar field in the framework of warm inflationary models, by using the irreversible thermodynamics of open systems with matter creation/annihilation. We consider the scalar fields, radiation and dark matter as an interacting three component cosmological fluid in a homogeneous and isotropic Friedmann-Lemaitre-Robertson-Walker (FLRW) Universe, in the presence of the curvature terms. The thermodynamics of open systems as applied together with the gravitational field equations to the three component cosmological fluid leads to a generalization of the elementary scalar field-radiation interaction model, which is the theoretical basis of warm inflationary models. Moreover, the decay (creation) pressures describing matter production are explicitly considered as parts of the cosmological fluid energy-momentum tensor. A specific theoretical model, describing coherently oscillating scalar waves, is considered. In particular, we investigate the role of the curvature terms in the dynamical evolution of the early Universe, by considering numerical solutions of the gravitational field equations. Our results indicate that despite the fact that the Universe becomes flat at the end of the inflationary era, the curvature terms, if present, may still play an important role in the very first stages of the evolution of the Universe.
Introduction
The question of the homogeneity settled over far apart regions in space, respectively the queries concerning the horizon and the flatness problems of the Universe, are beautifully answered by the theory of inflation, introduced in Guth (1981). Alan Guth’s “old inflation” requires the existence of a scalar field, whose energymomentum tensor mimics that of an ideal fluid. For a detailed discussion of the properties of scalar fields see Mukhanov (2005) and Nojiri et al. (2017), respectively. Later on, a “new inflation” scenario was proposed, in which the self-interacting potential V (φ) of the scalar field was set to be nearly flat at its minimum, where it un Bucharest, 2022 2 Teodora MATEI et al. 2 dergoes oscillatory fluctuations (Linde, 1982; Albrecht and Steinhardt, 1982). Due to multiple complications raised by this model, the chaotic inflationary scenario was developed in Linde (1983) and Linde (1994), respectively. In the chaotic inflation model one considers a region in space where at the initial time t = t0 the scalar field is very large, and approximately homogeneous. The energy-momentum tensor of the scalar field is dominated by the large potential, thus leading to an equation of state pφ ≈ −ρφ, and to an inflationary expansion.
Conclusion
The present paper aims to address from an open thermodynamical system perspective the problem of the creation of particles in a warm inflationary scenario by considering a three-component dynamical system composed of a scalar field, radiation, and dark matter, respectively. Moreover, we have assumed that the Universe may have had an initial curvature at the moment of its very beginning, and we have explored the role this curvature may have had on the evolution of the physical properties of the cosmological system. The work conducted in this paper intends to enlarge the approach of Harko and Sheikhahmadi (2020), by including a dark matter and a curvature component into the cosmological field equations of the warm inflationary formalism. In our study we have considered the early Universe as an open thermodynamic systems in which entropy and particle creation occurs (Prigogine et al., 1988). The time evolution of the dynamically interacting cosmological fluid consisting of a scalar field, radiation and dark matter has been investigated in the curved FLRW geometry, with the effects of the geometric curvature terms fully taken into account. Some important features of this model can be observed from the behaviour of the physical and geometrical parameters, as obtained in the previous Section. As the scalar field decays into the newly created radiation and dark matter particles (see Fig. 1), the temperature of the early Universe is bound to increase, in the case of a flat, k = 0, open, k = −1, or closed, k = 1, geometry, from a zero value to a maximum 12 Teodora MATEI et al. 12 value. After reaching its maximum, the temperature decreases, due to the accelerated expansion of the Universe. Buy to read more.
References
Albrecht A., Steinhardt P.J. , Turner M.S., Wilczek F.: 1982, Phys. Rev. Lett. 48, 1437.
Albrecht A., Steinhardt P.J.: 1982, Phys. Rev. Lett. 48, 1220.
Antusch S., Nolde D., Orani S.: 2015, J. Cosmol. Astropart. Phys. 06, 009.
Bastero-Gil M., Berera A., Ramos R.O.: 2011, J. Cosmol. Astropart. Phys. 1107, 030.
Berera A., Fang L.-Z.: 1995, Phys. Rev. Lett. 74 1912.
Berera A., Moss I. G. and Ramos R. O.: 2009, Reports on Progress in Physics 72, 026901.
Berera A.: 1996, Phys. Rev. D 54, 2519.
Berera A.: 1995, Phys. Rev. Lett. 75, 3218.
B¨ohmer C. G., Harko T.: 2007, JCAP 0706, 025.
Calv˜ao M., Lima J., Waga I.: 1992, Phys. Lett. B 162, 223.
Chakraborty S., Saha S.: 2014, Phys. Rev. D 90, 123505.
Chakraborty S.: 2014, Phys. Lett. B 732, 81.
De Oliveira H.P., Jor´as S.E.: 2001, Phys.Rev. D 64, 063513.
Dentler M., Marsh D.J.E., Hloˇzek R., Lagu¨e A., Rogers K.K., Grin D.:2022, Monthly Notices of the
Royal Astronomical Society 515, arXiv:2111.01199.
Gleiser M. and Ramos R. O.: 1994, Phys. Rev. D 50, 2441.
Guth A.: 1981, Phys. Rev. D 23, 347.
Hall L.M.H., Moss I.G., Berera A.: 2004, Phys. Rev. D 69, 083525.
Harko T. and Sheikhahmadi H.: 2020, Physics of the Dark Universe 28, 100521.
Harko T. and Sheikhahmadi H.: 2021, Eur. Phys. J. C, 81, 165.
Harko T., Liang P., Liang S.-D., and Mocanu G.:2015, JCAP 11, 027.
Harko T., Lobo F.S.N.: 2013, Phys. Rev. D 87, 044018.
Harko T.: 2014, Phys. Rev. D 90, 044067.
Kofman L., Linde A., Starobinsky A.A.: 1994, Phys. Rev. Lett. 73, 3195.
Liddle P. P. A. R. and Barrow J. D.: 1994, Phys. Rev. D 50, 7222.
Lima J.A.S., Baranov I.: 2014, Phys. Rev. D 90, 043515.
Lima J.A.S., Basilakos S., Sol`a J.: 2016, Eur. Phys. J. C 76, 228.
Linde A.: 1982, Phys. Lett. B 108, 389.
Linde A.: 1983, Phys. Lett. B 129, 177.
Linde A.: 1994, Phys. Rev. D 49, 748.
Modak S.K., Singleton D.: 2012, Phys. Rev. D 86, 123515.
Mukhanov V.: 2005, Physical Foundations of Cosmology, Cambridge University Press, Cambridge,
UK.
Nojiri S., Odintsov S.D., Oikonomou V.K.: 2017, Phys. Rep. 692, 1.
Nunes R.C., Pan S.: 2016, Mon. Not. R. Astron. Soc. 459, 673.
Pigozzo C., Carneiro S., Alcaniz J.S. , Borges H.A., Fabris J.C.: 2016, J. Cosmol. Astropart. Phys. 05,
022.
Pinto M. A. S., Harko T., and Lobo F. S. N.:2022, Phys. Rev. D 106, 044043.
Prigogine I., Geheniau J., Gunzig E., Nardone P.: 1988, Proc. Natl. Acad. Sci. 85, 7428.
17 Dark matter and radiation in warm inflation 17
Qiang Y., Zhang T.-J., Yi Z.-L.: 2007, Astrophys. Space Sci. 311, 407.
Stewart E. D.: 2002, Phys. Rev. D 65, 103508.
Su J., Harko T., Liang S.-D.: 2017, Adv. High Energy Phys. 2017, 76502398.
Zimdahl W., Triginer J., Pavon D.: 1996, Phys. Rev. D 54, 6101.
Abstract
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