Stable singularity-free cosmological solutions in nonprojectable Hořava-Lifshitz gravity

Fukushima, Mitsuhiro; Misonoh, Yosuke; Miyashita, Shoichiro; Sato, Seiga

doi:10.1103/physrevd.99.064004

Cited by 7 publications

(7 citation statements)

References 148 publications

(164 reference statements)

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“…In low energy regime (λ → ∞), the evolution equation (31) of the TT tensor mode reduces to the standard one in general relativity as expected, i.e.,…”

Section: Equations Of Motionsupporting

confidence: 59%

“…b) If γ = 1 4 ± 2 3 , then K 1 = 48 and K 2 = 0. Now, the asymptotic behavior of the evolution equation (31) reduces tö…”

Section: Solution IImentioning

confidence: 99%

“…From the evolution equation (31), one can see that the perturbation dynamics of tensor mode are influenced by the coefficients F 0 , F 1 , and F 2 , where F 2 is relevant to the kinetic term of the graviton and a negativesigned F 2 causes a ghost instability, and a negativesigned of F 0 is related to the gradient instability. For convenience, we recast (31) as…”

Section: Equations Of Motionmentioning

confidence: 99%

“…Moreover, if the effective squared mass M 2 is negative, there may exist undesirable exponential growth. However, whether the system is unstable or not, it also depends on which one of F and M 2 is dominant in the evolution[31]. Here, some possible stabilities and instabilities of tensor evolution are classified as follows: a) If F 2 < 0, the theory suffers a ghost instability, which leads to a fatal collapse of vacuum in perturba-tions.…”

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confidence: 99%

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Tensor stability in Born-Infeld determinantal gravity

2019

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We consider the transverse-traceless tensor perturbation of a spatial flat homogeneous and isotropic spacetime in Born-Infeld determinantal gravity, and investigate the evolution of the tensor mode for two solutions in the early universe. For the first solution where the initial singularity is replaced by a regular geometric de Sitter inflation of infinite duration, the evolution of the tensor mode is stable for the parameter spaces α < −1, ω ≥ −1/3 and α = −1, ω > 0. For the second solution where the initial singularity is replaced by a primordial brusque bounce, which suffers a sudden singularity at the bouncing point, the evolution of the tensor mode is stable for all regions of the parameter space. Our calculation suggests that the tensor evolution can hold stability in large parameter spaces, which is a remarkable property of Born-Infeld determinantal gravity. We also constrain the theoretical parameter |λ| ≥ 10 −38 m −2 by resorting to the current bound on the speed of the gravitational waves.

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“…In low energy regime (λ → ∞), the evolution equation (31) of the TT tensor mode reduces to the standard one in general relativity as expected, i.e.,…”

Section: Equations Of Motionsupporting

confidence: 59%

“…b) If γ = 1 4 ± 2 3 , then K 1 = 48 and K 2 = 0. Now, the asymptotic behavior of the evolution equation (31) reduces tö…”

Section: Solution IImentioning

confidence: 99%

Section: Equations Of Motionmentioning

confidence: 99%

mentioning

confidence: 99%

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Tensor stability in Born-Infeld determinantal gravity

2019

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“…In [9] the authors found that HL cosmology provide an alternative to inflation and that the universe can be singularity-free, for reviews of HL cosmology we refer the reader to [10,11]. Very few exact solutions exists in HL cosmology with or without any matter source [12][13][14][15][16], however, according to our knowledge the are not known analytical solutions in HL cosmology when a minimally scalar field contributes to the total evolution of the universe.…”

Section: Introductionmentioning

confidence: 99%

Cosmological solutions in Hořava-Lifshitz gravity

Paliathanasis,

Leon

2019

Preprint

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We perform a detailed study on the integrability of the Hořava-Lifshitz scalar field cosmology in a Friedmann-Lemaître-Robertson-Walker background spacetime. The approach we follow to determine the integrability is that of the Singularity Analysis. More specifically, we test if the gravitational field equations possesses the Painlevé property. For the exponential potential of the scalar field we are able to perform an analytic explicit integration of the field equations and write the solution in terms of Laurent expansion and more specifically write the solution in terms of Right Painlevé series.

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A phase space description of the FLRW quantum cosmology in Hořava–Lifshitz type gravity

2019

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Quantum cosmology of the Friedmann-Lemaître-Robertson-Walker model with cosmological constant in the Hořava-Lifshitz type gravity is studied in the phase space by means of the Wigner function. The modification of the usual general relativity description by the Hořava-Lifshitz type gravity induces a new scenario for the origin of the Universe with an embryonic era where the Universe can exist classically before the tunneling process takes place and which gives rise to the current evolution of the Universe. The Wigner functions corresponding to the Hartle-Hawking, Vilenkin and Linde boundary conditions are obtained by means of numerical calculations. In particular three cases were studied for the potential of the Wheeler-DeWitt equation: tunneling barrier with and without embryonic era and when the potential barrier is not present. The quantum behavior of these three cases are analyzed using the Wigner function for the three boundary conditions considered. *

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Stable singularity-free cosmological solutions in nonprojectable Hořava-Lifshitz gravity

Cited by 7 publications

References 148 publications

Tensor stability in Born-Infeld determinantal gravity

Tensor stability in Born-Infeld determinantal gravity

Cosmological solutions in Hořava-Lifshitz gravity

A phase space description of the FLRW quantum cosmology in Hořava–Lifshitz type gravity

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