On Resolutions of Cosmological Singularities in Higher-Spin Gravity

Burrington, Benjamin A.; Zayas, Leopoldo A. Pando; Rombes, Nicholas

doi:10.48550/arxiv.1309.1087

Cited by 5 publications

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“…Some recent papers dealing with cosmologies and singularities in a higher spin set up can be found in [22][23][24]. In [23] a cosmological sinularity resolution was done, but in the context of dS 3 (higher spin) gravity.…”

Section: Introduction and Conclusionmentioning

confidence: 99%

Desingularization of the Milne Universe

Krishnan

Roy

2014

Physics Letters B

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Resolution of cosmological singularities is an important problem in any full theory of quantum gravity. The Milne orbifold is a cosmology with a big-bang/big-crunch singularity, but being a quotient of flat space it holds potential for resolution in string theory. It is known however, that some perturbative string amplitudes diverge in the Milne geometry. Here we show that flat space higher spin theories can effect a simple resolution of the Milne singularity when one embeds the latter in 2+1 dimensions. We explain how to reconcile this with the expectation that non-perturbative string effects are required for resolving Milne. Along the way, we introduce a Grassmann realization of the \.{I}n\"on\"u-Wigner contraction to export much of the AdS technology to our flat space computation.Comment: 4 pages, revtex, v2: minor clarifications/corrections, refs added, v3: minor error corrected, v4: published PLB version (essentially

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Section: Introduction and Conclusionmentioning

confidence: 99%

Desingularization of the Milne Universe

Krishnan

Roy

2014

Physics Letters B

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“…It has also been shown that once the asymptotic conditions ( 40) are expressed in a suitable "decoupling" gauge choice, they admit a consistent vanishing cosmological constant limit, so that the asymptotic symmetries are spanned by a higher spin extension of the BMS 3 algebra with an appropriate central extension [35] (see also [36]). Related results along these lines, including Hamiltonian reduction [37], unitarity [38], and the analysis of cosmologies endowed with higher spin fields have been discussed in [39], [40], [41], [42]).…”

Section: Higher Spin Gravity In 3dmentioning

confidence: 99%

“…However, it should be stressed that identifying the integration constants L and W with global charges, appears to be very counterintuitive from the point of view of the canonical formalism. This is because, in spite of the fact that the components of the gauge fields along dx ± for the black hole solution (50) agree with the ones of the asymptotic fall-off in (40), once a nonvanishing constant μ is included, the additional terms along dx ∓ amount to a severe modification of the asymptotic form of the dynamical fields a ± θ , so that the expression for the global charges in eq. ( 47) no longer applies for this class of black hole solutions.…”

Section: B Higher Spin Black Hole Proposal and Its Thermodynamicsmentioning

confidence: 99%

“…This can be seen as follows. At a slice of fixed time, according to (40), the asymptotic behaviour of the dynamical fields is of the form…”

Section: Solving the Puzzles: Asymptotic Conditions Revisited And Dif...mentioning

confidence: 99%

“…where ν ± , µ ± stand for arbitrary fixed functions of t, θ without variation (δν ± = δµ ± = 0), that correspond to the chemical potentials. Note that, since the asymptotic form of the dynamical fields (66) is unchanged as compared with (40), the expression for the global charges remains the same, i.e., at a fixed t slice, the global charges are again given by (47), so that the asymptotic symmetries are still generated by two copies of the W 3 algebra.…”

Section: Solving the Puzzles: Asymptotic Conditions Revisited And Dif...mentioning

confidence: 99%

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Brief review on higher spin black holes

Perez,

Tempo,

Troncoso

2014

Preprint

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Higher spin extension of cosmological spacetimes in 3D: asymptotically flat behaviour with chemical potentials and thermodynamics

Matulich

Pérez

Tempo

et al. 2015

J. High Energ. Phys.

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A generalized set of asymptotic conditions for higher spin gravity without cosmological constant in three spacetime dimensions is constructed. They include the most general temporal components of the gauge fields that manifestly preserve the original asymptotic higher spin extension of the BMS 3 algebra, with the same central charge. By virtue of a suitable permissible gauge choice, it is shown that this set can be directly recovered as a limit of the boundary conditions that have been recently constructed in the case of negative cosmological constant, whose asymptotic symmetries are spanned by two copies of the centrally-extended W 3 algebra. Since the generalized asymptotic conditions allow to incorporate chemical potentials conjugated to the higher spin charges, a higher spin extension of locally flat cosmological spacetimes becomes naturally included within the set. It is shown that their thermodynamic properties can be successfully obtained exclusively in terms of gauge fields and the topology of the Euclidean manifold, which is shown to be the one of a solid torus, but with reversed orientation as compared with the one of black holes. It is also worth highlighting that regularity of the fields can be ensured through a procedure that does not require an explicit matrix representation of the entire gauge group. In few words, we show that the temporal components of generalized dreibeins can be consistently gauged away, which partially fixes the chemical potentials, so that the remaining conditions can just be obtained by requiring the holonomy of the generalized spin connection along a thermal circle to be trivial. The extension of the generalized asymptotically flat behaviour to the case of spins s ≥ 2 is also discussed.

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On Resolutions of Cosmological Singularities in Higher-Spin Gravity

Cited by 5 publications

References 0 publications

Desingularization of the Milne Universe

Desingularization of the Milne Universe

Brief review on higher spin black holes

Higher spin extension of cosmological spacetimes in 3D: asymptotically flat behaviour with chemical potentials and thermodynamics

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