Inflation with a graceful exit and entrance driven by Hawking radiation

Modak, Sujoy K.; Singleton, Douglas

doi:10.1103/physrevd.86.123515

Cited by 69 publications

(57 citation statements)

References 25 publications

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“…Thus we see that in the radiation era (i.e., γ = 4 3 ), we have ρ ∝ T 4 , i.e., the Universe as a thermodynamical system behaves as a black body [37,38].…”

Section: Cosmological Solutions Behaviour Of the Thermodynamicamentioning

confidence: 99%

Particle production and universal thermodynamics

Saha

Chakraborty

2015

Gen Relativ Gravit

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In the present work, particle creation mechanism has been employed to the Universe as a thermodynamical system. The Universe is considered to be a spatially flat FRW model and cosmic fluid is chosen as a perfect fluid with a barotropic equation of statep = (γ − 1)ρ. By proper choice of the particle creation rate, expressions for the entropy and temperature have been determined at various stages of evolution of the Universe. Finally, using the deceleration parameter q as a function of the redshift parameter z based on recent observations, the particle creation rate has been evaluated and its variation at different epochs have been shown graphically.

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“…Thus we see that in the radiation era (i.e., γ = 4 3 ), we have ρ ∝ T 4 , i.e., the Universe as a thermodynamical system behaves as a black body [37,38].…”

Section: Cosmological Solutions Behaviour Of the Thermodynamicamentioning

confidence: 99%

Particle production and universal thermodynamics

Saha

Chakraborty

2015

Gen Relativ Gravit

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“…Further, due to isotropy of the FRW space-time, the radiation is isotropic from all directions. Thus in case of BH there is a loss of energy while for the FRW space-time, the universe gains energy which can be expressed by the Stephen-Boltzmann radiation law as [40] …”

Section: Particle Creation As a Phenomenon Of Hawking Radiationmentioning

confidence: 99%

Complete cosmic scenario from inflation to late time acceleration: Nonequilibrium thermodynamics in the context of particle creation

Chakraborty

Saha

2014

Phys. Rev. D

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The paper deals with the mechanism of particle creation in the framework of irreversible thermodynamics. The second order non-equilibrium thermodynamical prescription of Israel and Stewart has been presented with particle creation rate, treated as the dissipative effect.In the background of a flat FRW model, we assume the non-equilibrium thermodynamical process to be isentropic so that the entropy per particle does not change and consequently the dissipative pressure can be expressed linearly in terms of the particle creation rate. Here the dissipative pressure behaves as a dynamical variable having a non-linear inhomogeneous evolution equation and the entropy flow vector satisfies the second law of thermodynamics.Further, using the Friedmann equations and by proper choice of the particle creation rate as a function of the Hubble parameter, it is possible to show (separately) a transition from the inflationary phase to the radiation era and also from matter dominated era to late time acceleration. Also, in analogy to analytic continuation, it is possible to show a continuous cosmic evolution from inflation to late time acceleration by adjusting the parameters. It is found that in the de Sitter phase, the comoving entropy increases exponentially with time, keeping entropy per particle unchanged. Subsequently, the above cosmological scenarios has been described from field theoretic point of view by introducing a scalar field having self interacting potential. Finally, we make an attempt to show the cosmological phenomenon of particle creation as Hawking radiation, particularly during the inflationary era.

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“…Dividing this equation by dt gives the following differential form of the first law of thermodynamics [59]:…”

Section: A Continuity Equation From the First Law Of Thermodynamicsmentioning

confidence: 99%

“…(20), suppose a sphere of arbitrary radius r [59]. The volume of the sphere is given by V ¼ 4πr 3 =3.…”

Section: A Continuity Equation From the First Law Of Thermodynamicsmentioning

confidence: 99%

General form of entropy on the horizon of the universe in entropic cosmology

Komatsu

2016

Phys. Rev. D

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Entropic cosmology assumes several forms of entropy on the horizon of the universe, where the entropy can be considered to behave as if it were related to the exchange (the transfer) of energy. To discuss this exchangeability, the consistency of the two continuity equations obtained from two different methods is examined, focusing on a homogeneous, isotropic, spatially flat, and matter-dominated universe. The first continuity equation is derived from the first law of thermodynamics, whereas the second equation is from the Friedmann and acceleration equations. To study the influence of forms of entropy on the consistency, a phenomenological entropic-force model is examined, using a general form of entropy proportional to the nth power of the Hubble horizon. In this formulation, the Bekenstein entropy (an area entropy), the Tsallis-Cirto black-hole entropy (a volume entropy), and a quartic entropy are represented by n ¼ 2, 3, and 4, respectively. The two continuity equations for the present model are found to be consistent with each other, especially when n ¼ 2, i.e., the Bekenstein entropy. The exchange of energy between the bulk (the universe) and the boundary (the horizon of the universe) should be a viable scenario consistent with the holographic principle.

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Inflation with a graceful exit and entrance driven by Hawking radiation

Cited by 69 publications

References 25 publications

Particle production and universal thermodynamics

Particle production and universal thermodynamics

Complete cosmic scenario from inflation to late time acceleration: Nonequilibrium thermodynamics in the context of particle creation

General form of entropy on the horizon of the universe in entropic cosmology

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