Black holes and stars in the Horava-Lifshitz theory with the projectability condition

Greenwald, Jared; Papazoglou, Antonios; Wang, Anzhong

doi:10.1103/physrevd.81.084046

Cited by 54 publications

(41 citation statements)

References 132 publications

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“…In [38], it was showed explicitly that metric (3.9) is related to metric (3.1) by the coordinate transformations,…”

Section: A (Anti-) De Sitter Schwarzschild Solutionsmentioning

confidence: 99%

Singularities in Horava–Lifshitz theory

Cai¹,

Wang²

2010

Physics Letters B

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Singularities in (3 + 1)-dimensional Horava-Lifshitz (HL) theory of gravity are studied. These singularities can be divided into scalar, non-scalar curvature, and coordinate singularities. Because of the foliation-preserving diffeomorphisms of the theory, the number of scalars that can be constructed from the extrinsic curvature tensor Kij , the 3-dimensional Riemann tensor and their derivatives is much large than that constructed from the 4-dimesnional Riemann tensor and its derivatives in general relativity (GR). As a result, even for the same spacetime, it may be singular in the HL theory but not in GR. Two representative families of solutions with projectability condition are studied, one is the (anti-) de Sitter Schwarzschild solutions, and the other is the Lu-Mei-Pope (LMP) solutions written in a form satisfying the projectability condition -the generalized LMP solutions. The (anti-) de Sitter Schwarzschild solutions are vacuum solutions of both HL theory and GR, while the LMP solutions with projectability condition satisfy the HL equations coupled with an anisotropic fluid with heat flow. It is found that the scalars K and Kij K ij are singular only at the center for the de Sitter Schwarzschild solution, but singular at both the center and r = (3M/|Λ|)for the anti-de Sitter Schwarzschild solution. The singularity at r = (3M/|Λ|) 1/3 is absent in GR. In addition, all the generalized LMP solutions have two scalar curvature singularities, located at either r = 0 and r = rs > 0, or r = r1 and r = r2 with r2 > r1 > 0, or r = rs > 0 and r = ∞, depending on the choice of the free parameter λ.PACS numbers: 98.80.Cq; 98.80.Bp

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“…In [38], it was showed explicitly that metric (3.9) is related to metric (3.1) by the coordinate transformations,…”

Section: A (Anti-) De Sitter Schwarzschild Solutionsmentioning

confidence: 99%

Singularities in Horava–Lifshitz theory

Cai¹,

Wang²

2010

Physics Letters B

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“…Note that in [11,13,45], the constant c, representing the speed of light, was absorbed into N . The ADM form (2.1) is preserved by the types of coordinate transformations,…”

Section: A the Svw Setupmentioning

confidence: 99%

Stability of spin-0 graviton and strong coupling in Horava-Lifshitz theory of gravity

Wang

2011

Phys. Rev. D

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In this paper, we consider two different issues, stability and strong coupling, raised lately in the newly-proposed Horava-Lifshitz (HL) theory of quantum gravity with projectability condition. We find that all the scalar modes are stable in the de Sitter background, due to two different kinds of effects, one from high-order derivatives of the spacetime curvature, and the other from the exponential expansion of the de Sitter space. Combining these effects properly, one can make the instability found in the Minkowski background never appear even for small-scale modes, provided that the IR limit is sufficiently closed to the relativistic fixed point. At the fixed point, all the modes become stabilized. We also show that the instability of Minkowski spacetime can be cured by introducing mass to the spin-0 graviton. The strong coupling problem is investigated following the effective field theory approach, and found that it cannot be cured by the Blas-Pujolas-Sibiryakov mechanism, initially designed for the case without projectability condition, but might be circumvented by the Vainshtein mechanism, due to the non-linear effects. In fact, we construct a class of exact solutions, and show explicitly that it reduces smoothly to the de Sitter spacetime in the relativistic limit.PACS numbers: 98.80.Cq; 98.80.Bp

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“…Thus, this theory leads to a modification of the Einstein's general relativity at high energies producing interesting features in cosmology. Furthermore Horava-Lifshitz gravity has been studied and extended in detail [29][30][31][32][33][34][35][36] and applied as a cosmological frame work of the universe [37][38][39][40][41][42][43][44][45][46]. Recently, different dark energy models have been studied in the framework of Horava-Lifshitz cosmology using different infrared cut-offs.…”

Section: Introductionmentioning

confidence: 99%

Generalized ghost dark energy in Horava–Lifshitz cosmology

Borah

Ansari

2014

J Theor Appl Phys

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Purpose of this paper is to study generalized quantum chromodynamics ghost dark energy (GDE) in the frame work of Horava-Lifshitz cosmology. Considering interacting and non-interacting scenario of GDE with dark matter in a spatially non-flat universe, we investigate the cosmological implications of this model in detail. We obtain equation of state parameter, deceleration parameter and the evolution of dark energy density to explain the expansion of the universe. Also, we show that the results we calculate have a good compatibility with previous work and restore it in limiting case. Further, we investigate validity of generalized second law of thermodynamics in this scenario. Finally, we find out a cosmological application of our work by evaluating a relation for the equation of state of dark energy for law redshifts.

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Black holes and stars in the Horava-Lifshitz theory with the projectability condition

Cited by 54 publications

References 132 publications

Singularities in Horava–Lifshitz theory

Singularities in Horava–Lifshitz theory

Stability of spin-0 graviton and strong coupling in Horava-Lifshitz theory of gravity

Generalized ghost dark energy in Horava–Lifshitz cosmology

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