Massive Gravity
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Graviton J = 2
Citation: M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98, 030001 (2018) graviton J = 2 graviton MASS Van Dam and Veltman (VANDAM 70), Iwasaki (IWASAKI 70), and Za- kharov (ZAKHAROV 70) almost simultanously showed that “... there is a discrete difference between the theory with zero-mass and a theory with finite mass, no matter how small as compared to all external momenta.” The resolution of this ”vDVZ discontinuity” has to do with whether the linear approximation is valid. De Rham etal. (DE-RHAM 11) have shown that nonlinear effects not captured in their linear treatment can give rise to a screening mechanism, allowing for massive gravity theories. See also GOLDHABER 10 and DE-RHAM 17 and references therein. Experimental limits have been set based on a Yukawa potential or signal dispersion. h0 − − is the Hubble constant in units of 100 kms 1 Mpc 1. − The following conversions are useful: 1 eV = 1.783 × 10 33 g = 1.957 × −6 × −7 × 10 me ; λ¯C = (1.973 10 m) (1 eV/mg ). VALUE (eV) DOCUMENT ID TECN COMMENT − <6 × 10 32 1 CHOUDHURY 04 YUKA Weak gravitational lensing ••• We do not use the following data for averages, fits, limits, etc. ••• − <7 × 10 23 2 ABBOTT 17 DISP Combined dispersion limit from three BH mergers − <1.2 × 10 22 2 ABBOTT 16 DISP Combined dispersion limit from two BH mergers − <5 × 10 23 3 BRITO 13 Spinningblackholesbounds − <4 × 10 25 4 BASKARAN 08 Graviton phase velocity fluctua- − tions <6 × 10 32 5 GRUZINOV 05 YUKA Solar System observations − <9.0 × 10 34 6 GERSHTEIN 04 From Ω value assuming RTG − tot >6 × 10 34 7 DVALI 03 Horizon scales − <8 × 10 20 8,9 FINN 02 DISP Binary pulsar orbital period de- crease 9,10 DAMOUR 91 Binary pulsar PSR 1913+16 − <7 × 10 23 TALMADGE 88 YUKA Solar system planetary astrometric data − − < 2 × 10 29 h 1 GOLDHABER 74 Rich clusters − 0 <7 × 10 28 HARE 73 Galaxy <8 × 104 HARE 73 2γ decay 1 CHOUDHURY 04 concludes from a study of weak-lensing data that masses heavier than about the inverse of 100 Mpc seem to be ruled out if the gravitation field has the Yukawa form. -
Graviton J = 2
Citation: P.A. Zyla et al. (Particle Data Group), Prog. Theor. Exp. Phys. 2020, 083C01 (2020) graviton J = 2 graviton MASS Van Dam and Veltman (VANDAM 70), Iwasaki (IWASAKI 70), and Za- kharov (ZAKHAROV 70) almost simultanously showed that “... there is a discrete difference between the theory with zero-mass and a theory with finite mass, no matter how small as compared to all external momenta.” The resolution of this ”vDVZ discontinuity” has to do with whether the linear approximation is valid. De Rham etal. (DE-RHAM 11) have shown that nonlinear effects not captured in their linear treatment can give rise to a screening mechanism, allowing for massive gravity theories. See also GOLDHABER 10 and DE-RHAM 17 and references therein. Experimental limits have been set based on a Yukawa potential or signal dispersion. h0 − − is the Hubble constant in units of 100 kms 1 Mpc 1. − The following conversions are useful: 1 eV = 1.783 × 10 33 g = 1.957 × −6 × −7 × 10 me ; λ¯C = (1.973 10 m) (1 eV/mg ). VALUE (eV) DOCUMENT ID TECN COMMENT − <6 × 10 32 1 CHOUDHURY 04 YUKA Weak gravitational lensing • • • We do not use the following data for averages, fits, limits, etc. • • • − <6.8 × 10 23 BERNUS 19 YUKA Planetary ephemeris INPOP17b − <1.4 × 10 29 2 DESAI 18 YUKA Gal cluster Abell 1689 − <5 × 10 30 3 GUPTA 18 YUKA SPT-SZ − <3 × 10 30 3 GUPTA 18 YUKA Planck all-sky SZ − <1.3 × 10 29 3 GUPTA 18 YUKA redMaPPer SDSS-DR8 − <6 × 10 30 4 RANA 18 YUKA Weak lensing in massive clusters − <8 × 10 30 5 RANA 18 YUKA SZ effect in massive clusters − <7 × 10 23 6 ABBOTT -
Beyond the Cosmological Standard Model
Beyond the Cosmological Standard Model a;b; b; b; b; Austin Joyce, ∗ Bhuvnesh Jain, y Justin Khoury z and Mark Trodden x aEnrico Fermi Institute and Kavli Institute for Cosmological Physics University of Chicago, Chicago, IL 60637 bCenter for Particle Cosmology, Department of Physics and Astronomy University of Pennsylvania, Philadelphia, PA 19104 Abstract After a decade and a half of research motivated by the accelerating universe, theory and experi- ment 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 in- frared, 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 deriva- tives 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. -
Curriculum Vitae Markus Amadeus Luty
Curriculum Vitae Markus Amadeus Luty University of Maryland Department of Physics College Park, Maryland 20742 301-405-6018 e-mail: [email protected] Education Ph.D. in physics, University of Chicago, 1991 Honors B.S. in physics, B.S. in mathematics, University of Utah, 1987 Academic Honors Alfred P. Sloan Fellow (1997–1998) National Science Foundation Graduate Fellowship (1988–1991) Phi Beta Kappa, Phi Kappa Phi (1987) Kenneth Browning Memorial Scholarship (1986) National Merit Scholarship (1982–1986) Academic Positions 2001–present tenured associate professor, University of Maryland 1996–2001 assistant professor, University of Maryland 1994–1995 post-doctoral researcher, Massachusetts Institute of Technology 1991–1994 post-doctoral researcher, Lawrence Berkeley National Laboratory 1988–1991 graduate research assistant (with Y. Nambu), University of Chicago 1987–1988 graduate teaching assistant, University of Chicago 1985–1986 undergraduate teaching assistant, University of Utah 1 Recent Invited Conference/Workshop Talks • June 2003, SUSY 2003 (Tuscon) plenary talk: “Supersymmetry without Super- gravity.” • January 2003, PASCOS (Mumbai, India) plenary talk: “New ideas in super- symmetry breaking” • October 2002, Workshop on Frontiers Beyond the Standard Model (Mineapolis): “Supersymmetry without supergravity.” • August 2002, Santa Fe Workshop on Extra Dimensions and Beyond: “Super- symmetry without Supergravity.” • January 2002, ITP Brane World Workshop: “Anomaly Mediated Supersymme- try Breaking.” • April 2001, APS Division of Particles -
Conformally Coupled General Relativity
universe Article Conformally Coupled General Relativity Andrej Arbuzov 1,* and Boris Latosh 2 ID 1 Bogoliubov Laboratory for Theoretical Physics, JINR, Dubna 141980, Russia 2 Dubna State University, Department of Fundamental Problems of Microworld Physics, Universitetskaya str. 19, Dubna 141982, Russia; [email protected] * Correspondence: [email protected] Received: 28 December 2017; Accepted: 7 February 2018; Published: 14 February 2018 Abstract: The gravity model developed in the series of papers (Arbuzov et al. 2009; 2010), (Pervushin et al. 2012) is revisited. The model is based on the Ogievetsky theorem, which specifies the structure of the general coordinate transformation group. The theorem is implemented in the context of the Noether theorem with the use of the nonlinear representation technique. The canonical quantization is performed with the use of reparametrization-invariant time and Arnowitt– Deser–Misner foliation techniques. Basic quantum features of the models are discussed. Mistakes appearing in the previous papers are corrected. Keywords: models of quantum gravity; spacetime symmetries; higher spin symmetry 1. Introduction General relativity forms our understanding of spacetime. It is verified by the Solar System and cosmological tests [1,2]. The recent discovery of gravitational waves provided further evidence supporting the theory’s viability in the classical regime [3–6]. Despite these successes, there are reasons to believe that general relativity is unable to provide an adequate description of gravitational phenomena in the high energy regime and should be either modified or replaced by a new theory of gravity [7–11]. One of the main issues is the phenomenon of inflation. It appears that an inflationary phase of expansion is necessary for a self-consistent cosmological model [12–14]. -
Ads₄/CFT₃ and Quantum Gravity
AdS/CFT and quantum gravity Ioannis Lavdas To cite this version: Ioannis Lavdas. AdS/CFT and quantum gravity. Mathematical Physics [math-ph]. Université Paris sciences et lettres, 2019. English. NNT : 2019PSLEE041. tel-02966558 HAL Id: tel-02966558 https://tel.archives-ouvertes.fr/tel-02966558 Submitted on 14 Oct 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Prepar´ ee´ a` l’Ecole´ Normale Superieure´ AdS4/CF T3 and Quantum Gravity Soutenue par Composition du jury : Ioannis Lavdas Costas BACHAS Le 03 octobre 2019 Ecole´ Normale Superieure Directeur de These Guillaume BOSSARD Ecole´ Polytechnique Membre du Jury o Ecole´ doctorale n 564 Elias KIRITSIS Universite´ Paris-Diderot et Universite´ de Rapporteur Physique en ˆIle-de-France Crete´ Michela PETRINI Sorbonne Universite´ President´ du Jury Nicholas WARNER University of Southern California Membre du Jury Specialit´ e´ Alberto ZAFFARONI Physique Theorique´ Universita´ Milano-Bicocca Rapporteur Contents Introduction 1 I 3d N = 4 Superconformal Theories and type IIB Supergravity Duals6 1 3d N = 4 Superconformal Theories7 1.1 N = 4 supersymmetric gauge theories in three dimensions..............7 1.2 Linear quivers and their Brane Realizations...................... 10 1.3 Moduli Space and Symmetries............................ -
Classical and Quantum Consistency of the DGP Model
IFT-UAM/CSIC-04-13 CERN-PH-TH/2004-063 Classical and Quantum Consistency of the DGP Model Alberto Nicolis a and Riccardo Rattazzi b aInstituto de F´ısica Te´orica, C–XVI, UAM, 28049 Madrid, Spain bPhysics Department, Theory Division, CERN, CH–1211 Geneva 23, Switzerland Abstract We study the Dvali-Gabadadze-Porrati model by the method of the boundary effective action. The truncation of this action to the bending mode π consistently describes physics in a wide range of regimes both at the classical and at the quantum level. The Vainshtein effect, which restores agreement with precise tests of general relativity, follows straightforwardly. We give a simple and general proof of stability, i.e. absence of ghosts in the fluctuations, valid for most of the relevant cases, like for instance the spherical source in asymptotically flat space. However we confirm that around certain interesting self-accelerating cosmological solutions there is a ghost. We consider the issue of quantum corrections. Around flat space π becomes strongly coupled below a macroscopic length of 1000 km, thus impairing the predictivity of the model. Indeed the tower of higher dimensional operators which is expected by a generic UV completion of the model limits predictivity at even larger length scales. We outline a non-generic but consistent choice of counterterms for which this disaster does not happen and for which the model remains calculable and successful in all the astrophysical situations of interest. By this choice, the extrinsic curvature Kµν acts roughly like a dilaton field controlling the strength of the interaction and the cut-off scale at each space-time point. -
Cosmologies of Extended Massive Gravity
Cosmologies of extended massive gravity Kurt Hinterbichler, James Stokes, and Mark Trodden Center for Particle Cosmology, Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA (Dated: June 15, 2021) We study the background cosmology of two extensions of dRGT massive gravity. The first is variable mass massive gravity, where the fixed graviton mass of dRGT is replaced by the expectation value of a scalar field. We ask whether self-inflation can be driven by the self-accelerated branch of this theory, and we find that, while such solutions can exist for a short period, they cannot be sustained for a cosmologically useful time. Furthermore, we demonstrate that there generally exist future curvature singularities of the “big brake” form in cosmological solutions to these theories. The second extension is the covariant coupling of galileons to massive gravity. We find that, as in pure dRGT gravity, flat FRW solutions do not exist. Open FRW solutions do exist – they consist of a branch of self-accelerating solutions that are identical to those of dRGT, and a new second branch of solutions which do not appear in dRGT. INTRODUCTION AND OUTLINE be sustained for a cosmologically relevant length of time. In addition, we show that non-inflationary cosmological An interacting theory of a massive graviton, free of solutions to this theory may exhibit future curvature sin- the Boulware-Deser mode [1], has recently been discov- gularities of the “big brake” type. ered [2, 3] (the dRGT theory, see [4] for a review), al- In the second half of this letter (which can be read lowing for the possibility of addressing questions of in- independently from the first), we consider the covariant terest in cosmology. -
Milgrom's Law and Lambda's Shadow: How Massive Gravity
Journal of the Korean Astronomical Society preprint - no DOI assigned 00: 1 ∼ 4, 2015 June pISSN: 1225-4614 · eISSN: 2288-890X The Korean Astronomical Society (2015) http://jkas.kas.org MILGROM'S LAW AND Λ'S SHADOW: HOW MASSIVE GRAVITY CONNECTS GALACTIC AND COSMIC DYNAMICS Sascha Trippe Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea; [email protected] Received March 11, 2015; accepted June 2, 2015 Abstract: Massive gravity provides a natural solution for the dark energy problem of cosmology and is also a candidate for resolving the dark matter problem. I demonstrate that, assuming reasonable scaling relations, massive gravity can provide for Milgrom’s law of gravity (or “modified Newtonian dynamics”) which is known to remove the need for particle dark matter from galactic dynamics. Milgrom’s law comes with a characteristic acceleration, Milgrom’s constant, which is observationally constrained to a0 1.1 10−10 ms−2. In the derivation presented here, this constant arises naturally from the cosmologically≈ × required mass of gravitons like a0 c√Λ cH0√3ΩΛ, with Λ, H0, and ΩΛ being the cosmological constant, the Hubble constant, and the∝ third cosmological∝ parameter, respectively. My derivation suggests that massive gravity could be the mechanism behind both, dark matter and dark energy. Key words: gravitation — cosmology — dark matter — dark energy 1. INTRODUCTION On smaller scales, the dynamics of galaxies is in ex- cellent agreement with a modification of Newtonian dy- Modern standard cosmology suffers from two criti- namics (the MOND paradigm) in the limit of small ac- cal issues: the dark matter problem and the dark celeration (or gravitational field strength) g, expressed energy problem. -
Massive Supergravity
1 Massive Supergravity Taichiro Kugo Maskawa Institute, Kyoto Sangyo University Nov. 8 { 9, 2014 第4回日大理工・益川塾連携 素粒子物理学シンポジウム in collaboration with Nobuyoshi Ohta Kinki University 2 1 Introduction Cosmological Constant Problem: Higgs Condensation ∼ ( 100 GeV )4 QCD Chiral Condensation ∼ ( 100 MeV )4 (1) These seem not contributing to the Cosmological Constant! =) Massive Gravity: an idea toward resolving it However, Massive Gravity has its own problems: • van Dam-Veltman-Zakharov (vDVZ) discontinuity Its m ! 0 limit does not coincides with the Einstein gravity. • Boulware-Deser ghost − |{z}10 |(1{z + 3)} = 6 =|{z} 5 + |{z}1 (2) hµν i N=h00;N =h0i massive spin2 BD ghost We focus on the BD ghost problem here. 3 In addition, we believe that any theory should eventually be made super- symmetric, that is, Supergravity (SUGRA). This may be of help also for the problem that the dRGT massive gravity allows no stable homogeneous isotropic universe solution. In this talk, we 1. explain the dRGT theory 2. massive supergravity 2 Fierz-Pauli massive gravity (linearized) Einstein-Hilbert action p LEH = −gR (3) [ ] h i 2 L L −m 2 − 2 = EH + (hµν ah ) (4) quadratic part in hµν | 4 {z } Lmass = FP (a = 1) gµν = ηµν + hµν (5) 4 In Fierz-Pauli theory with a = 1, there are only 5 modes describing properly massive spin 2 particle. : ) No time derivative appears for h00; h0i in LEH !LEH is linear in N; Ni. Lmass ∼ If a = 1, the mass term FP is also clearly linear in N h00 ! =) • Ni can be solved algebraically and be eliminated. -
Three-Dimensional Teleparallel Chern-Simons Supergravity Theory
Three-dimensional teleparallel Chern-Simons supergravity theory Ricardo Caroca∗, Patrick Concha∗, Diego Pe˜nafiel‡, Evelyn Rodr´ıguez, ∗Departamento de Matem´atica y F´ısica Aplicadas, Universidad Cat´olica de la Sant´ısima Concepci´on, Alonso de Ribera 2850, Concepci´on, Chile. ‡Facultad de Ciencias, Universidad Arturo Prat, Iquique, Chile. [email protected], [email protected], [email protected], [email protected], Abstract In this work we present a gauge-invariant three-dimensional teleparallel supergravity theory using the Chern-Simons formalism. The present construction is based on a supersymmetric extension of a particular deformation of the Poincar´ealgebra. At the bosonic level the theory describes a non-Riemannian geometry with a non-vanishing torsion. In presence of supersym- metry, the teleparallel supergravity theory is characterized by a non-vanishing super-torsion in which the cosmological constant can be seen as a source for the torsion. We show that the teleparallel supergravity theory presented here reproduces the Poincar´esupergravity in the van- ishing cosmological limit. The extension of our results to N = p + q supersymmetries is also explored. arXiv:2103.06717v1 [hep-th] 11 Mar 2021 1 Introduction Teleparallel gravity is an alternative theory of gravity known to be considered equivalent to General Relativity. However, they are conceptually quite different. In particular, the teleparallel formulation of gravity is described by a vanishing curvature and a non-vanishing torsion which characterizes the parallel transport [1–5]. In such case, the geometry is no more Riemannian but corresponds to the so-called Riemannian-Cartan (Weizenb¨ock) geometry. In three spacetime dimensions, there has been an interest in exploring black hole solutions and boundary symmetries of gravity theories with torsion [6–12]. -
Cosmological Implications of Modified Gravity: Spherical Collapse and Higher Order Correlations
University of Pennsylvania ScholarlyCommons Publicly Accessible Penn Dissertations Fall 2009 COSMOLOGICAL IMPLICATIONS OF MODIFIED GRAVITY: SPHERICAL COLLAPSE AND HIGHER ORDER CORRELATIONS Alexander Borisov University of Pennsylvania, [email protected] Follow this and additional works at: https://repository.upenn.edu/edissertations Part of the Cosmology, Relativity, and Gravity Commons Recommended Citation Borisov, Alexander, "COSMOLOGICAL IMPLICATIONS OF MODIFIED GRAVITY: SPHERICAL COLLAPSE AND HIGHER ORDER CORRELATIONS" (2009). Publicly Accessible Penn Dissertations. 47. https://repository.upenn.edu/edissertations/47 This paper is posted at ScholarlyCommons. https://repository.upenn.edu/edissertations/47 For more information, please contact [email protected]. COSMOLOGICAL IMPLICATIONS OF MODIFIED GRAVITY: SPHERICAL COLLAPSE AND HIGHER ORDER CORRELATIONS Abstract In the Standard Model of Cosmology the nature of the Dark Energy has become one of the most significant and conceptual challenges ot be resolved. One of the possible approaches to solving it is to introduce modifications ot General Relativity, that include Chameleon effects, which allow for a change in the strength of gravity based on the environment. This can provide for a consistent explanation of both large-scale observations and Solar system experiments. In the task to distinguish them from the LCDM model of gravity, or any other competing explanation, we need to study the consequences of these modifications for the growth of perturbations. In this thesis a recently developed Chameleon f(R) modification ot gravity is explored. We study its consequences for the distribution of matter on large scale using the Bispectrum. Using 1D simulations we examine the formation of galaxy and cluster halos and its observational effects. Finally we present an investigation of a method for studying gravitational lensing.