Gravitational anomaly and fundamental forces

Similar documents
Gravity, Strings and Branes

Yet Another Alternative to Compactification by Heterotic Five-branes

Gravity, Strings and Branes

Yet Another Alternative to Compactification

Quantum Dynamics of Supergravity

Curiosités géométriques et physique de l'univers

On Special Geometry of Generalized G Structures and Flux Compactifications. Hu Sen, USTC. Hangzhou-Zhengzhou, 2007

Lecture 9: RR-sector and D-branes

String Phenomenology ???

Quantum Fields in Curved Spacetime

Some simple exact solutions to d = 5 Einstein Gauss Bonnet Gravity

Exact solutions in supergravity

Inflation and Cosmic Strings in Heterotic M-theory

Solutions to gauge hierarchy problem. SS 10, Uli Haisch

Theoretical Explanations for Cosmic Acceleration

SUPERSTRING REALIZATIONS OF SUPERGRAVITY IN TEN AND LOWER DIMENSIONS. John H. Schwarz. Dedicated to the memory of Joël Scherk

Gauge-Higgs Unification on Flat Space Revised

Heterotic Torsional Backgrounds, from Supergravity to CFT

NEW KALUZA-KLEIN THEORY

Dynamics of Multiple Kaluza-Klein Monopoles in M- and String Theory

The Correct Interpretation of the Kaluza-Klein Theory

Generalized N = 1 orientifold compactifications

Exploring Universal Extra-Dimensions at the LHC

Introduction to Inflation

Fuzzy extra dimensions and particle physics models

Particles and Strings Probing the Structure of Matter and Space-Time

8.821 String Theory Fall 2008

Scale symmetry a link from quantum gravity to cosmology

Spectral Action from Anomalies

Observing the Dimensionality of Our Parent Vacuum

An extended standard model and its Higgs geometry from the matrix model

The Search for the Complete History of the Cosmos. Neil Turok

κ = f (r 0 ) k µ µ k ν = κk ν (5)

Introduction to the Beyond the Standard Model session

Chern-Simons Theory and Its Applications. The 10 th Summer Institute for Theoretical Physics Ki-Myeong Lee

Final Exam: Sat. Dec. 18, 2:45-4:45 pm, 1300 Sterling Exam is cumulative, covering all material. From last time

One of the problems in modern physics

BPS Solitons and Killing Spinors in Three Dimensional N =2Supergravity

The cosmological constant puzzle

PHY 475/375. Lecture 5. (April 9, 2012)

String Theory Compactifications with Background Fluxes

Continuity of the Deconfinement Transition in (Super) Yang Mills Theory

Théorie des cordes: quelques applications. Cours IV: 11 février 2011

The Cosmological Principle

Superstring in the plane-wave background with RR-flux as a conformal field theory

8.821 String Theory Fall 2008

Entropy of asymptotically flat black holes in gauged supergravit

Katrin Becker, Texas A&M University. Strings 2016, YMSC,Tsinghua University

Introduction. How did the universe evolve to what it is today?

Exact Solution of an Ekpyrotic Fluid and a Primordial Magnetic Field in an Anisotropic Cosmological Space-Time of Petrov D

Heterotic Geometry and Fluxes

Twistor Strings, Gauge Theory and Gravity. Abou Zeid, Hull and Mason hep-th/

Brane world scenarios

Cordes et Branes: des outils pour la cosmologie primordiale. Strings & branes: tools for primordial cosmology. Dan Israël, iap

Galaxies 626. Lecture 3: From the CMBR to the first star

MIFPA PiTP Lectures. Katrin Becker 1. Department of Physics, Texas A&M University, College Station, TX 77843, USA. 1

Zhong-Zhi Xianyu (CMSA Harvard) Tsinghua June 30, 2016

NTNU Trondheim, Institutt for fysikk

WHY BLACK HOLES PHYSICS?

PoS(LAT2005)324. D-branes and Topological Charge in QCD. H. B. Thacker University of Virginia

Continuity of the Deconfinement Transition in (Super) Yang Mills Theory

A sky without qualities

Beyond the standard model? From last time. What does the SM say? Grand Unified Theories. Unifications: now and the future

A Landscape of Field Theories

Inflationary cosmology from higher-derivative gravity

New Fundamental Wave Equation on Curved Space-Time and its Cosmological Applications

Thick Brane World. Seyen Kouwn Korea Astronomy and Space Science Institute Korea

M-Theory and Matrix Models

String-Theory: Open-closed String Moduli Spaces

String Theory II GEORGE SIOPSIS AND STUDENTS

Cosmology. Jörn Wilms Department of Physics University of Warwick.

Pietro Fre' SISSA-Trieste. Paolo Soriani University degli Studi di Milano. From Calabi-Yau manifolds to topological field theories

Potential Discoveries at the Large Hadron Collider. Chris Quigg

Elementary particles and typical scales in high energy physics

Citation for published version (APA): de Wit, T. C. (2003). Domain-walls and gauged supergravities Groningen: s.n.

TOPIC V BLACK HOLES IN STRING THEORY

String Theory. Three String Theories STRING THEORY 1. John H. Schwarz

Lecturer: Bengt E W Nilsson

Observational evidence and cosmological constant. Kazuya Koyama University of Portsmouth

Some PPPs (particle physics puzzles)

QUANTUM FIELD THEORY. A Modern Introduction MICHIO KAKU. Department of Physics City College of the City University of New York

Neutron Stars in the Braneworld

Anomaly and gaugino mediation

A Comment on String Solitons

HIGGS-GRAVITATIONAL INTERATIONS! IN PARTICLE PHYSICS & COSMOLOGY

Cosmological Issues. Consider the stress tensor of a fluid in the local orthonormal frame where the metric is η ab

A Higher Derivative Extension of the Salam-Sezgin Model from Superconformal Methods

Introduction. Chapter Why string theory?

XIII. The Very Early Universe and Inflation. ASTR378 Cosmology : XIII. The Very Early Universe and Inflation 171

A glimpse on Cosmology: Mathematics meets the Data

Theoretical Aspects of the Equivalence Principle

Espansione a grandi N per la gravità e 'softening' ultravioletto

arxiv: v1 [hep-ph] 7 May 2009

arxiv:hep-th/ v1 13 Feb 2001

Searching for Extra Space Dimensions at the LHC. M.A.Parker Cavendish Laboratory Cambridge

What is the Universe Made Of?

GRANGIAN QUANTIZATION OF THE HETEROTIC STRING IN THE BOSONIC FORMULAT

Dark Energy vs. Dark Matter: Towards a unifying scalar field?

What ideas/theories are physicists exploring today?

F-theory effective physics via M-theory. Thomas W. Grimm!! Max Planck Institute for Physics (Werner-Heisenberg-Institut)! Munich

Transcription:

Gravitational anomaly and fundamental forces J. J. van der Bij Institut für Physik Albert-Ludwigs Universität Freiburg Corfu, September 9, 2009

Is there a reason for the choice of gauge group and representations? Phys. Rev. D76, 121702 (R) (2007) I. Rabi: Who ordered that? on the discovery of the muon A. Einstein: Did God have a choice when he created the world?

Leukippos, Demokritos Emptiness space Fullness atoms Plato, Empedokles, Aristoteles Elements Tetrahedron Octahedron Icosahedron Cube (fire) (air) (water) (earth) Dodekahedron fifth element (quintessence) prediction of the theory mathematical basis

Space Spacetime with structure: R µναβ and dynamic: R µν = κt µν (Einstein) Matter: gauge theories (symmetry) Groups and representations Many possibilities Constraint: anomaly cancellation Symmetry breaking (Higgs): not considered here

Ellis, Gaillard, Zumino (1980) N = 8 Supergravity SO(8) symmetry too small Hidden SU(8) assumption 1: SU(8) becomes dynamical assumption 2: also superpartners dynamical assumption 3: anomaly free subset of SU(5) assumption 4: non-chiral part mass to Planck mass Leaves 3(5 + 5) + 9(1) and supersymmetry, which has to be broken Nowadays N = 8 supergravity is not anymore considered fundamental (non-renormalizable).

Gross, Harvey, Martinec, Rohm (1985) Heterotic string Anomaly free superstring 10 dimensions Gauge group E(8) E(8) assumption 1: compactification to 4-D assumption 2: one E(8) disappears assumption 3: Calabi-Yau manifold to break E(8) assumption 4: topology to get 3 generations assumption 5: some form of supersymmetry breaking Nowadays string theory has many vacua and no unique gauge theory is expected.

What do we learn? Assuming one knows the fundamental laws of physics and only has to construct the standard model out of these is not very promising. Therefore use experiment. anomalies are important topology is important

Vector bosons gauge group seen: SU(3) SU(2) U(1) natural embedding in SU(5) SU(3) SU(2) = +2 U(1) = +2 +2 No sign for a higher rank gauge group 3 3

Fitting analysis: χ 2 plot (I) Significance plot for the parameter space a Y,a BY for P 10 (χ 2 ). The contours acumulate 68%, 90% and 95% CL. The three dots correspond to the models best point: SM at origin a Y at x-axis, a Y,a BY at contour center ab Y 10 4 8 6 4 2 6 4 2 2 4 6 8 2 ay 10 4 4 6 Klausurtagung: Feldberg, 16-18 Oct 2006 A. Lorca: The Z reconsidered

Fermions (lefthanded) under SU(5) 10 = 5 = d d d e ν e 0 ū ū u d 0 ū u d 0 u d 0 e + 0 1 = ν e 10 + 5 + 1 = 16 of SO(10) Therefore automatically (chiral) anomaly free

we have to explain Vektorbosons SU(5) Fermions SO(10) 3 generations of fermions Z ν ν δρ δm Z The only known indication is an anomaly, possibly related to topology

Example of topology in the universe Higher dimensional Kaluza-Klein universe Example: M 4 U(1) n with radius of U(1) going to zero Difficult in practice Therefore we try the opposite and assume that the universe was three dimensional

Supernova Cosmology Project 3 No Big Bang Knop et al. (2003) Spergel et al. (2003) Allen et al. (2002) 2 Supernovae 1 Ω Λ 0 Clusters CMB expands forever recollapses eventually closed -1 open flat 0 1 2 3 Ω M

Cosmic topology multiple images: difficult, evolution cosmic microwave background: circles in the sky (lack of power in quadrupole??) Theory: In flat space, topology can always be at too large a scale to be seen directly I I

Bianchi-I universes Flat, homogeneous, non-isotropic Pancake picture ds 2 = dt 2 + a 2 (t)(dx 2 + dy 2 ) + b 2 (t)dz 2 dx,dy topology R 2 ; dz topology S 1 Late in time ȧ ḃ a b, therefore isotropy This is generically true when there is a positive cosmological constant (Wald s theorem 1983) So present day isotropy says little about the (very) early universe.

At small t approximate Kasner solution (1925) ds 2 = dt 2 + dx 2 + dy 2 + t 2 dz 2 therefore the third dimension gets compactified to zero at early times For instance exact dust universe (λ = 0) g zz = M 1/3 t/(t + Σ) 1/3 g xx = g yy = M 2/3 (t + Σ) 2/3 M and Σ are integration constants

Suggested topology of the universe M 3 S 1 S 1 The radius may be too large to see the topology at the present time However a preferred direction may be visible There appears to be an allignment of low multipoles along a preferred axis in the data This could be explained in an inflationary Bianchi-I model

3 dimensional Yang-Mills theory L = 1 2 Tr F µνf µν i m ɛ µνρ Tr(A µ ν A ρ + A µ AνAρ) F µν = µ A ν ν A µ + g[a µ, A ν ] There is a gauge invariance under A µ U 1 ( µ /g + A µ )U Under large gauge transformations the action shifts by 8π 2 im/g 2 So full invariance leads to a quantization condition g YM = 4πm g 2 must be integer

Renormalization q ren YM = q 0 YM + C(G) + sign(m f )N f C(R) SU(N): C(G) = N fundamental fermion: C(R) = 1/2 So one needs an even number of fermions. This stays true even when m f = 0. In four dimensions there is a similar effect when one starts with Weyl-fermions in a M 3 S 1 spacetime. There a Chern-Simons like term is generated L CSlike = m ph n α ɛ αµνρ A µ F νρ

L = (1/κ 2 ) gr Three dimensional gravity i 4κ 2 µ ɛµνλ (R µνab ωλ ab + 2 3 ωb µaωνbω c λc). a q gr = 6π µκ 2 must be integer Renormalization q ren gr = q 0 gr + 1 8 N g sign(m g ) 1 16 N f sign(m f ) N g is the number of vector bosons N f is the number of fermions assume q gr = 0 (Einstein equations) consistency: N f 2N g = 0 mod(16)

isotropization: q ren gr = 0 Stronger conditions vectors and fermions separately consistent: N g = 0 mod(8) N f = 0 mod(16) In combination vectors SU(5): 24 fermions SO(10): 16 2 24 3 16 = 0 Basically unique if also: 1) fermions automatically anomaly free, i.e. no SU(n): 2) fermions in fundamental representation

Speculations Symmetry breaking: SU(5) decomposition: 16 = 10 + 5 + 1. SU(3) +, SU(2), U(1) + 10 +, 5, 1 2 (8 3 + 1) 3 (10 5 1) = 0 possible: SU(5) SU(3) SU(2) U(1) impossible: SU(5) SU(4) U(1) more conditions other compactifications underlying structure quantum gravity

Rabi s question: who ordered that? Answer: the early universe. Einstein s question: did God have a choice? Answer: no, because He has to use perfect symmetry. However the devil may have had something to do with the Higgs sector.