Holographic Fluctuations from Unitary de Sitter Invariant Field Theory

Banks, Tom; Fischler, Willy; Torres, T. J.; Wainwright, Carroll L.

doi:10.48550/arxiv.1306.3999

Cited by 8 publications

(9 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In [79] we showed the approximate SO(1, 4) invariance and the general rules of cosmological perturbation theory, including Maldacena's [80] squeezed limit theorem, was enough to reproduce the data. This general framework predicts a nearly scale invariant scalar two point function, and a small, equilateral scalar three point function, which is probably below the limits of near future observations.…”

Section: The Variables Satisfymentioning

confidence: 88%

Supersymmetry Breaking and the Cosmological Constant

Banks

2014

Preprint

View full text Add to dashboard Cite

I review three attempts to explain the small value of the cosmological constant, and their connection to SUSY breaking. They are The String Landscape, Supersymmetric Large Extra Dimensions (SLED), and the Holographic Space-time Formalism invented by Fischler and myself.try 2 and a discrete R symmetry larger than Z 2 3 , . Generically, in supergravity (SUGRA), SUSY alone implies a negative c.c. . However, in a conventional effective field theory approach, any attempt to correlate the small positive value of the c.c. with a small breaking of SUSY, seems doomed to failure. Experiment tells us that the breaking of SUSY in the particle spectrum takes place at the scale of hundreds of GeV. Dimensional analysis alone would then suggest a c.c. of order Λ 1/4 ∼ 10 10 GeV, which is 57 orders of magnitude larger than the observational bound. Calculations of Feynman diagrams in QU(antum) E(ffective) F(ield) T(heory), reproduce this value generically, though there are special models where somewhat smaller values can be obtained. However, there is a subtlety in these calculations. SUGRA contains an extra constant,W 0 , the value of the superpotential at the minimum of the effective potential, which is invisible in the M P → ∞ limit. For any given size of SUSY breaking in the particle spectrum, we can tune W 0 to make the c.c. as small as we wish. In QUEFT this appears to be "unnatural fine tuning". When the c.c. is (close to) zero, the gravitino mass is proportional to W 0 . This is because both W 0 and the gravitino mass, break any discrete complex R symmetry.The present review is idiosyncratic. It discusses some, but not all, attempts to understand how the small value of the c.c. is related to the breaking of SUSY. Many such attempts are admitted by their authors to be failures. It did not seem to be worthwhile discussing them. I will concentrate on the following list of alternatives• The String Landscape -Here one decides to separate the two problems from the outset.The c.c. is assumed to be chosen, for anthropic reasons, at random, without regard to SUSY. The question at issue is whether there is any reason to expect the SUSY breaking scale to be smaller than the Planck scale. The answer depends on both the person answering, and the year.7 This picturesque understanding of F-theory is fraught with difficulties. Models of gravity in 2+1 dimensional Minkowski space do not have S-matrix observables, since any scattering process creates a deficit angle in the geometry at infinity, which depends on the c.m. energy. So it is not clear what object in the hypothetical 2 + 1 dimensional model converges to the F-theory S-matrix. The duality is probably valid for a non-compact CY 4 .

show abstract

Section: The Variables Satisfymentioning

confidence: 88%

Supersymmetry Breaking and the Cosmological Constant

Banks

2014

Preprint

View full text Add to dashboard Cite

show abstract

“…The gauge/gravity duality in the inflationary setup is discussed, e.g., in Refs. [3,4,15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,36,37,38,39,40,41,42,43,44,45].…”

Section: ζ Correlators From Holographymentioning

confidence: 99%

Consistency relations and conservation of ζ in holographic inflation

Garriga

Urakawa

2016

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

It is well known that, in single clock inflation, the curvature perturbation ζ is constant in time on superhorizon scales. In the standard bulk description this follows quite simply from the local conservation of the energy momentum tensor in the bulk. On the other hand, in a holographic description, the constancy of the curvature perturbation must be related to the properties of the RG flow in the boundary theory. Here, we show that, in single clock holographic inflation, the time independence of correlators of ζ follows from the cut-off independence of correlators of the energy momentum tensor in the boundary theory, and from the so-called consistency relations for vertex functions with a soft leg.

show abstract

“…Work of Maldacena and others [14] has shown that current data on the CMB can be explained in a very simple framework, with no assumptions about particular models. Indeed, it was shown in [15] that the even the assumption that fluctuations originate from quantized fields is unnecessary. All one needs is the approximate SO(1, 4) invariance we will demonstrate below.…”

Section: So(1 4) Invariancementioning

confidence: 99%

Holographic Inflation and the Low Entropy of the Early Universe

Banks

2015

Preprint

Self Cite

View full text Add to dashboard Cite

This is a completely rewritten version of the talk I gave at the Philosophy of Cosmology conference in Tenerife, September 2014, which incorporates elements of my IFT Madrid Anthropics Conference talk. The original was too technical. The current version uses intuitive notions from black hole physics to explain the model of inflationary cosmology based on the Holographic Space Time formalism. The reason that the initial state of the universe had low entropy is that more generic states have no localized excitations, since in HST, localized excitations are defined by constraints on the fundamental variables. The only way to obtain a radiation dominated era, is for each time-like geodesic to see an almost uniform gas of small black holes as its horizon expands, such that the holes evaporate into radiation before they collide and coalesce. Comparing the time slicing that follows causal diamonds along a trajectory, with the global FRW slicing, one sees that systems outside the horizon had to undergo inflation, with a number of e-folds fixed by the present and inflationary cosmological constants, and the black hole number density on FRW slices just after inflation ends. These parameters also determine the size of scalar and tensor metric perturbations and the reheat temperature of the universe. I sketch a class of explicit finite quantum mechanical models of cosmology, which have these properties. Physicists interested in the details of those models should consult a recent paper [1].

show abstract

Holographic Fluctuations from Unitary de Sitter Invariant Field Theory

Cited by 8 publications

References 14 publications

Supersymmetry Breaking and the Cosmological Constant

Supersymmetry Breaking and the Cosmological Constant

Consistency relations and conservation of ζ in holographic inflation

Holographic Inflation and the Low Entropy of the Early Universe

Contact Info

Product

Resources

About