Black hole discharge in massive electrodynamics and black hole disappearance in massive gravity

Mirbabayi, Mehrdad; Gruzinov, Andrei

doi:10.1103/physrevd.88.064008

Cited by 21 publications

(22 citation statements)

References 53 publications

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“…How close can we take it to zero before running into a problem? One estimate is to use the discharge rate of a black hole in a theory of a massive photon [72],…”

Section: Jhep07(2019)181mentioning

confidence: 99%

Photon masses in the landscape and the swampland

Reece

2019

J. High Energ. Phys.

110

158

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In effective quantum field theory, a spin-vector boson can have a technically natural small mass that does not originate from the Higgs mechanism. For such theories, which may be written in Stückelberg form, there is no point in field space at which the mass is exactly zero. I argue that quantum gravity differs from, and constrains, effective field theory: arbitrarily small Stückelberg masses are forbidden. In particular, the limit in which the mass goes to zero lies at infinite distance in field space, and this distance is correlated with a tower of modes becoming light according to the Swampland Distance Conjecture. Application of Tower or Sublattice variants of the Weak Gravity Conjecture makes this statement more precise: for a spinvector boson with coupling constant e and Stückelberg mass m, local quantum field theory breaks down at energies at or below Λ UV = min((mM Pl /e) 1/2 , e 1/3 M Pl ). Combined with phenomenological constraints, this argument implies that the Standard Model photon must be exactly massless. It also implies that much of the parameter space for light dark photons, which are the target of many experimental searches, is compatible only with Higgs and not Stückelberg mass terms. This significantly affects the experimental limits and cosmological histories of such theories. I explain various caveats and weak points of the arguments, including loopholes that could be targets for model-building. arXiv:1808.09966v2 [hep-th] 6 Aug 2019This is a mild over-simplification; after reading the argument below the interested reader can consult Appendix A for a more careful statement about the case of dynamical symmetry breaking.

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“…How close can we take it to zero before running into a problem? One estimate is to use the discharge rate of a black hole in a theory of a massive photon [72],…”

Section: Jhep07(2019)181mentioning

confidence: 99%

Photon masses in the landscape and the swampland

Reece

2019

J. High Energ. Phys.

110

158

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“…• It was argued in Ref. [86] that another type of instability of black holes in massive gravity (with one fixed metric) should exist. Such a process would be similar to the discharge of a collapsing charged star, but in this case the black hole's mass would decrease in a finite time (even classically).…”

Section: Conclusion and Open Issuesmentioning

confidence: 99%

Black holes in massive gravity

Babichev

Brito

2015

Class. Quantum Grav.

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We review the black hole solutions of the ghost-free massive gravity theory and its bimetric extension and outline the main results on the stability of these solutions against small perturbations. Massive (bi)-gravity accommodates exact black hole solutions, analogous to those of General Relativity. In addition to these solutions, hairy black holes -solutions with no correspondent in General Relativityhave been found numerically, whose existence is a natural consequence of the absence of Birkhoff's theorem in these theories. The existence of extra propagating degrees of freedom, makes the stability properties of these black holes richer and more complex than those of General Relativity. In particular, the bi-Schwarzschild black hole exhibits an unstable spherically symmetric mode, while the bi-Kerr geometry is also generically unstable, both against the spherical mode and against superradiant instabilities. If astrophysical black holes are described by these solutions, the superradiant instability of the Kerr solution imposes stringent bounds on the graviton mass. arXiv:1503.07529v2 [gr-qc] 15 Jul 2015 ‡ A settled term often used in the literature to refer to dRGT theory and its extensions is the "ghost-free massive gravity". This name should be used with care, since dRGT theory is free from the Boulware-Deser ghost (or Ostrogradski ghost), but the other degrees of freedom are not necessary healthy for particular solutions. Therefore the right term should rather be "Boulware-Deser ghost free massive gravity" or "Ostrogradski ghost free massive gravity", although we will also sometimes refer to dRGT theory and its extension simply as "ghost free massive gravity", keeping in mind the above reservation.

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“…In [217,218], de Rham, Gabadadze and Tolley (dRGT) found a loophole and constructed a theory that is free of this pathological sixth mode (this was shown conclusively in [634]). Much work has gone into studying this massive gravity theory: for example studies of cosmological solutions [635][636][637][638][639][640][641][642][643][644][645][646] and black holes [638,[647][648][649][650][651][652] have been undertaken. The theory can also be cast in a vielbein language, as opposed to as a theory of a metric [216,[653][654][655][656][657].…”

Section: A Brief History Of Massive Gravitymentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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After a decade and a half of research motivated by the accelerating universe, theory and experiment have a reached a certain level of maturity. The development of theoretical models beyond Λ or smooth dark energy, often called modified gravity, has led to broader insights into a path forward, and a host of observational and experimental tests have been developed. In this review we present the current state of the field and describe a framework for anticipating developments in the next decade. We identify the guiding principles for rigorous and consistent modifications of the standard model, and discuss the prospects for empirical tests.We begin by reviewing recent attempts to consistently modify Einstein gravity in the infrared, focusing on the notion that additional degrees of freedom introduced by the modification must "screen" themselves from local tests of gravity. We categorize screening mechanisms into three broad classes: mechanisms which become active in regions of high Newtonian potential, those in which first derivatives of the field become important, and those for which second derivatives of the field are important. Examples of the first class, such as f (R) gravity, employ the familiar chameleon or symmetron mechanisms, whereas examples of the last class are galileon and massive gravity theories, employing the Vainshtein mechanism. In each case, we describe the theories as effective theories and discuss prospects for completion in a more fundamental theory. We describe experimental tests of each class of theories, summarizing laboratory and solar system tests and describing in some detail astrophysical and cosmological tests. Finally, we discuss prospects for future tests which will be sensitive to different signatures of new physics in the gravitational sector.The review is structured so that those parts that are more relevant to theorists vs. observers/experimentalists are clearly indicated, in the hope that this will serve as a useful reference for both audiences, as well as helping those interested in bridging the gap between them.

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Black hole discharge in massive electrodynamics and black hole disappearance in massive gravity

Cited by 21 publications

References 53 publications

Photon masses in the landscape and the swampland

Photon masses in the landscape and the swampland

Black holes in massive gravity

Beyond the cosmological standard model

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