Holographic Weyl entropy bounds

Chamblin, Andrew; Erlich, Joshua

doi:10.1103/physrevd.70.044001

Cited by 7 publications

(13 citation statements)

References 20 publications

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“…The LHC will also collide two lead nuclei at √ s = 5.5 TeV per nucleon to produce quarkgluon plasma [2,3,37,38]. Since the total energy in the two lead nuclei collisions at LHC will be ∼1150 TeV, we may expect to see new physics [4] in the nuclear collisions at LHC as well.…”

Section: Discussionmentioning

confidence: 99%

String theory at LHC using Higgs production and decay from string balls

Nayak

2011

J. High Energ. Phys.

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If extra dimensions are found in the second run of LHC in the pp collisions at √ s = 14 TeV then the string scale can be ∼ TeV, and we should produce string balls at LHC. In this paper we study supersymmetry (squark and gluino) production from string balls at LHC in pp collisions at √ s = 14 TeV and compare that with the parton fusion results using pQCD. We find significant squark and gluino production from string balls at LHC which is comparable to parton fusion pQCD results. Hence, in the absence of black hole production at LHC, an enhancement in supersymmetry production can be a signature of TeV scale string physics at LHC.

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Section: Discussionmentioning

confidence: 99%

String theory at LHC using Higgs production and decay from string balls

Nayak

2011

J. High Energ. Phys.

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“…In essence, one may regard conditions (1) and (2) as the 'definition' of an acceptable entropy flux vector 1 . Crudely, the stress-energy part of the entropy flux is generated by 'matter' degrees of freedom, whereas the shear part corresponds to purely gravitational degrees of freedom [10]. Finally, we point out that there have been some criticisms of the covariant entropy bound and of the holographic principle more generally, see e.g., [11], [12], [17] and [14] as examples.…”

Section: Introductionmentioning

confidence: 92%

Twistors and holography

Chamblin¹

2004

Class. Quantum Grav.

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We extend Bousso's notion of a lightsheet -a surface where entropy can be defined in a way so that the entropy bound is satisfied -to more general surfaces. Intuitively, these surfaces may be regarded as deformations of the Bousso choice; in general, these deformations will be timelike and so we refer to them as 'timesheets'. We show that a timesheet corresponds to a section of a certain twistor bundle over a given spacelike two-surface B. We further argue that increasing the entropy flux through a given region of spacetime corresponds to increasing the volume of certain regions in twistor space. Put another way, it would seem that entropy in spacetime corresponds to volume in twistor space. We argue that this formulation may point a way towards a version of the covariant entropy bound which allows for quantum fluctuations of the lightsheet. We also point out that in twistor space, it might be possible to give a purely topological characterization of a lightsheet, at least for suitably simple spacetimes. I. INTRODUCTIONThroughout history [1], one of the central problems faced by philosophers and scientists has been the simple query: How does one define the concepts of space and time? Are they merely abstractions which we have introduced in order to facilitate a description of the interrelationship between things which actually 'exist' (e.g., such as material bodies)? Or do space and time 'exist' in and of themselves, without any reference to observable consequences? Although such Machian musings may seem esoteric, they actually take on a new and exciting life when viewed in the light of modern ideas coming from theoretical physics, especially quantum gravity. Indeed, most theoretical physicists today would probably agree that 'space' and 'time' will be effective concepts which only emerge at low energies. At scales past the Planck energy, 'space' and 'time' will simply cease to have any operational meaning, and some more fundamental ideas (comprising quantum gravity) will have to take over.Of course, at first it seems nonsensical to assert that the 'ultimate theory' should be constructed without invoking the use of the words 'space' or 'time'. After all, from our earliest days of undergraduate physics, we were all weaned on physical theories which simply would not make any sense without reference to these concepts. More precisely, theories such as classical or quantum mechanics are useful precisely because they are bodies of knowledge which allow us to predict, with at least some probability, the nature of future events given some knowledge about present or past events. One of the conceptual obstructions to constructing a quantum theory of gravity is that it is unclear what the theory will have to do with prediction; although certain quantum gravity models do yield predictions (such as the No Boundary Proposal), much more work on connecting quantum gravity with the low energy world around us is needed.On the aesthetic level, however, the construction of a quantum theory of gravity may be the most beautiful way o...

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“…We shall compare our results and extend the evaluation of the specific heats with the approach of Ref. [7] and comment on other references [6,7], where different choices for the definition of the thermodynamical observables are employed.…”

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confidence: 99%

“…One such model is given by a thin spherical shell of matter in a de Sitter space-time, since it may represent a collection of D-branes forming the so called D-Sitter space-time of Ref. [5], or can be used as a tool for the study of the entropy bound in a very simplified physical environment [6]. Finally, one may also consider the "operational" approach to black hole entropy, as illustrated in Ref.…”

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Thermodynamics of a collapsing shell in an expanding universe

2004

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We describe the quasi-static collapse of a radiating, spherical shell of matter in de Sitter space-time using a thermodynamical formalism. It is found that the specific heat at constant area and other thermodynamical quantities exhibit singularities related to phase transitions during the collapse.Because of the paradigm of inflation, de Sitter space-time has recently become the subject of great research interest. One aspect of research has been the conjectured dS-CFT correspondence [1] which is the analogue of Maldacena's AdS-CFT conjecture [2] for the case of a spacetime with a positive cosmological constant. As in the latter case, the "gravitational" (dS) side of the correspondence is expected to yield the macroscopic description of the system, whereas the CFT (conformal field theory) should be able to describe the microphysics. A well known example for the AdS-CFT is given by the microscopical description of the thermodynamical laws of black holes [3]. Furthermore, applications of the de Sitter space Bousso bound [4], related to the Bekenstein bound for flat space-times, have also drawn much interest.The dS-CFT correspondence has not yet reached the degree of comprehension of the AdS-CFT, since the corresponding CFT has not been completely identified. Therefore, one usually proceeds by studying simplified "gravitational" models in order to obtain general features that the relevant CFT is required to possess. One such model is given by a thin spherical shell of matter in a de Sitter space-time, since it may represent a collection of D-branes forming the so called D-Sitter space-time of Ref. [5], or can be used as a tool for the study of the entropy bound in a very simplified physical environment [6]. Finally, one may also consider the "operational" approach to black hole entropy, as illustrated in Ref. [7], which leads one to the conclusion that the entropy of a black hole is the same as that stored in a shell of matter sitting just outside its Schwartzschild radius after it has collapsed from infinity. According to the AdS-CFT correspondence, a black hole is represented by a thermal state and its formation by the approach to such a state. A thermodynamical description of the gravitational collapse should thus be useful in the de Sitter case as well. *

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Holographic Weyl entropy bounds

Cited by 7 publications

References 20 publications

String theory at LHC using Higgs production and decay from string balls

String theory at LHC using Higgs production and decay from string balls

Twistors and holography

Thermodynamics of a collapsing shell in an expanding universe

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