Thermodynamic constraints on the dark sector
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Thermodynamic constraints on the dark sector W. J. C. da Silva1,a
, J. E. Gonzalez1,b , R. Silva1,2,c , J. S. Alcaniz3,d
1 Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, Rio Grande do Norte
59072-970, Brasil
2 Departamento de Física, Universidade do Estado do Rio Grande do Norte, Mossoró, Rio Grande do Norte
59610-210, Brasil
3 Observatório Nacional, Rio de Janeiro, Rio de Janeiro 20921-400, Brasil
Received: 22 September 2020 / Accepted: 11 November 2020 © Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2020
Abstract In this paper, we present a unified scheme based on the fluid description of the dark sector of the universe. The scheme captures models with interaction between dark energy and dark matter, being the core of generalization the time-varying equation-of-state parameter ω(a) and the time-dependent interactions through the interaction function (a), where a is the scale factor. Furthermore, we propose thermodynamics constraints on this generalized class of models using the laws of thermodynamics which are combined with observational data. In order to test the observational viability of the unified model, we perform a Bayesian analysis using cosmic chronometers, type Ia supernovae, cosmic microwave background, and angular baryon acoustic oscillation measurements.
1 Introduction Observational and theoretical effort in modern cosmology has successfully revealed a picture of the universe which is very well realized through the standard model of cosmology, the + Cold Dark Matter (CDM) model. The component is responsible for a repulsive gravitational force at cosmological scales which accelerates the universe, whereas the dark matter provides explanation at galaxy and galaxy cluster scales for some gravitational phenomena, e.g., the observed rotation curves of galaxies and structure formation [1–3]. Despite the success of the standard model, our understanding of the universe still lacks a plausible explanation of the theoretical and observational issues associated with the late-time accelerated cosmic expansion of the universe [4]. These open questions have motivated some approaches which can be divided into two classes: extensions of general relativity (GR) [5] and dark energy models [6]. The former one considers infrared modifications to GR, leading to a weakening of gravity on cosmological scales, whereas the latter adds an exotic component of dark energy, e.g., a scalar field to the r.h.s of Einstein field equations. Within this context, the dark energy component can also be
a e-mail: [email protected] (corresponding author) b e-mail: [email protected] c e-mail: [email protected] d e-mail: [email protected]
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described through a fluid approach, with thermodynamics playing an important role in such a description (see, e.g., [7–13] and references therein). Thermodynamic considerations have been combined with observational d
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