False vacuum decay in a brane world cosmological model

Demetrian, Michal

doi:10.1007/s10714-006-0275-4

Cited by 27 publications

(24 citation statements)

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“…The false vacuum decay via the HM instanton describes the inflaton that jumps at the top of the potential barrier within the horizon-size domain, [10], [2], and afterwards rolls down-hill to the true vacuum. The semiclassical theory of the false vacuum decay by the instantons can be formulated also in the brane world scenarios, for further details se [4], [5] and [6]. The equations for the CdL instantons in the Randall-Sundrum type II scenario have the form [5] …”

Section: Introductionmentioning

confidence: 99%

“…The action (2) of the CdL instanton is considerably simplified by using the equations of motion (1), [6] …”

Section: Introductionmentioning

confidence: 99%

“…(An analogical situation is also in the standard Einstein's theory of relativity, with only changeĤ M → H M , [12], [13], [14] and [17]). In the case l = 1 the situation has been studied extensively in [6], where the approximative formulas for the first order CdL instanton and its action have been found in the mentioned limit (7). Let us recall the main results briefly.…”

Section: Introductionmentioning

confidence: 99%

“…If we introduce the notation y = Φ − Φ M , then in the limit (7) we have the CdL instanton that is close to the HM instanton (the limit CdL instanton) and in the lowest order we can write y = k cos(Ĥ M τ ) and the constant k (the inflaton amplitude) can be determined perturbatively. The result is [6] …”

Section: Introductionmentioning

confidence: 99%

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Coleman–de Luccia Instanton of the Second Order in a Brane World

Demetrian

2006

Int J Theor Phys

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Section: Introductionmentioning

confidence: 99%

“…The action (2) of the CdL instanton is considerably simplified by using the equations of motion (1), [6] …”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Coleman–de Luccia Instanton of the Second Order in a Brane World

Demetrian

2006

Int J Theor Phys

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“…To do so, one can generalize the Einstein field equations to obtain a modified version of gravity. There are different branches of modified gravity with various motivations, such as brane world cosmology [20][21][22], Lovelock gravity [23-27], scalar-tensor theories [28][29][30][31][32][33][34][35], and F (R) gravity [36][37][38][39][40][41][42][43][44][45][46][47][48][49][50][51].Modifying general relativity opens a new way to a large class of alternative theories of gravity ranging from higher dimensional physics [52-54] to non-minimally coupled (scalar) fields [55][56][57][58]. Regarding various models of modified gravity, we will be interested in F (R) gravity [59-65] based on replacing the scalar curvature R with a generic analytic function F (R) in the Hilbert-Einstein action.…”

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confidence: 99%

F(R)Gravity’s Rainbow and Its Einstein Counterpart

Hendi

Panah

Panahiyan

et al. 2016

Advances in High Energy Physics

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Motivated by UV completion of general relativity with a modification of a geometry at high energy scale, it is expected to have an energy dependent geometry. In this paper, we introduce charged black hole solutions with power Maxwell invariant source in the context of gravity's rainbow. In addition, we investigate two classes of F (R) gravity's rainbow solutions. At first, we study energy dependent F (R) gravity without energy momentum tensor, and then we obtain F (R) gravity's rainbow in the presence of conformally invariant Maxwell source. We study geometrical properties of the mentioned solutions and compare their results. We also give some related comments regarding to thermodynamical behavior of the obtained solutions and discuss thermal stability of the solutions. I. INTRODUCTIONAn accelerated expansion of the Universe was confirmed by various observational evidences. The luminosity distance of Supernovae type Ia [1,2], the anisotropy of cosmic microwave background radiation [3], and also wide surveys on galaxies [4] confirm such accelerated expansion. On the other hand, baryon oscillations [5], large scale structure formation [6], and weak lensing [7] also propose such an accelerated expansion of the Universe.After discovery of such an expansion in 1998, understanding its theoretical reasons presents one of the fundamental open questions in physics. Identifying the cause of this late time acceleration is a challenging problem in cosmology. Physicists are interested in considering this accelerated expansion in a gravitational background and they proposed some candidates to explain it. For example, a positive cosmological constant leads to an accelerated expansion, but it is plagued by the fine tuning problem [8][9][10][11][12]. In other words, the left hand side of Einstein equations can modify by the cosmological constant as a geometrical modification or it can be interpreted as a kinematic term on the right hand side with the equation of state parameter w = −1. By considering w < −1/3 for a source term, it is possible to further modify this approach. This consideration has interpretation of Dark Energy which has been investigated in literature [13][14][15][16][17][18][19]. In dark energy models, the acceleration expansion of the universe is due to an unknown ingredient added to the cosmic pie. The effects of this unknown ingredient is extracted by modifying the stress energy tensor of the Einstein equation with a matter which is different from than the usual matter and radiation components.On the other hand, it is proposed that the presence of accelerated expansion of the universe indicate that the standard general relativity requires modification. To do so, one can generalize the Einstein field equations to obtain a modified version of gravity. There are different branches of modified gravity with various motivations, such as brane world cosmology [20][21][22], Lovelock gravity [23-27], scalar-tensor theories [28][29][30][31][32][33][34][35], and F (R) gravity [36][37][38][39][40][41][42][43][44][45][46]...

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Phase transition of charged black holes in massive gravity through new methods

et al. 2016

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Motivated by providing preliminary steps to understand the conception of quantum gravity, in this paper, we study the phase structure of a semiclassical gravitational system. We investigate the stability conditions and phase transition of charged black holes in massive gravity via canonical and geometrical thermodynamic approaches. We point out the effects of massive parameter on stability conditions of these black holes and show how massive coefficients affect the phase transition points of these black holes. We also study the effects of boundary topology on thermodynamical behavior of the system. In addition, we give some arguments regarding the role of higher dimensions and highlight the effect of the electric charge in thermodynamical behavior. Then, we extend our study to geometrical thermodynamic approach and show that it can be a successful method for studying the black hole phase transition. At last, by employing the relation between thermodynamical pressure and cosmological constant, critical behavior of the system and the effects of different parameters on critical values are investigated.

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False vacuum decay in a brane world cosmological model

Cited by 27 publications

References 20 publications

Coleman–de Luccia Instanton of the Second Order in a Brane World

Coleman–de Luccia Instanton of the Second Order in a Brane World

F(R)Gravity’s Rainbow and Its Einstein Counterpart

Phase transition of charged black holes in massive gravity through new methods

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