POST-INFLATIONARY HIGGS RELAXATION AND THE ORIGIN OF MATTER- ANTIMATTER ASYMMETRY
|
|
- Cameron Adams
- 6 years ago
- Views:
Transcription
1 POST-INFLATIONARY HIGGS RELAXATION AND THE ORIGIN OF MATTER- ANTIMATTER ASYMMETRY LOUIS YANG ( 楊智軒 ) UNIVERSITY OF CALIFORNIA, LOS ANGELES (UCLA) DEC 30, TH INTERNATIONAL WORKSHOP ON DARK MATTER, DARK ENERGY AND MATTER-ANTIMATTER ASYMMETRY
2 OUTLINE The Higgs Potential Quantum Fluctuation During Inflation Higgs Relaxation After Inflation Leptogenesis via Higgs Field Relaxation Summary Based on: A. Kusenko, L. Pearce, LY, Phys.Rev.Lett. 114 (2015) 6, L. Pearce, LY, A. Kusenko, M. Peloso, Phys.Rev. D92 (2015) 2, LY, L. Pearce, A. Kusenko, Phys.Rev. D92 (2015)
3 THE HIGGS POTENTIAL 3
4 THE HIGGS BOSON In 2012, LHC has found the Higgs boson. V Φ = m 2 Φ + Φ + λ Φ + Φ, where Φ = v + h. Higgs boson mass: M h = ± ± GeV. A mass smaller than expected! A small quartic coupling λ μ = M t M h 2 2v V(φ) v h Electroweak Vacuum φ C. Patrignani et al.(particle Data Group), Chin. Phys. C, 40, (2016). 4
5 RUNNING OF λ J. Elias-Miro et al., Phys. Lett. B709, 222 (2012) G. Degrassi et al., JHEP 1208, 098 (2012) D. Buttazzo et al., arxiv: [hep-ph] QFT: Coupling constants changes with energy scale μ β λ = y t 4 + Due to large top mass m t = 1 2 y tv If no new physics, λ h becomes very small and turns negative at μ GeV. Figure from D. Buttazzo et al., arxiv: [hep-ph] 5
6 THE HIGGS EFFECTIVE POTENTIAL Another minimum in the potential: Planckain vacuum!! Much lower than the electroweak vacuum. Our universe can tunnel into the Planckain vacuum and end in a big crunch! ssss V lll V φ Planckian Vacuum h lll φ Our Electroweak Vacuum ~ GeV h 6
7 META-STABILITY OF OUR VACUUM J. Elias-Miro et al., Phys. Lett. B709, 222 (2012) G. Degrassi et al., JHEP 1208, 098 (2012) D. Buttazzo et al., arxiv: [hep-ph] Our universe seems to be right on the meta-stable region. 7
8 THE HIGGS EFFECTIVE POTENTIAL What does it imply? A shallow Higgs potential at large scale A large Higgs VEV during inflation ssss V lll V φ Planckian Vacuum h lll φ Our Electroweak Vacuum ~ GeV 8
9 QUANTUM FLUCTUATION DURING INFLATION 9
10 QUANTUM FLUCTUATION DURING INFLATION During inflation, quantum fluctuations get amplified. They becomes classical when the wavelength exits the horizon. φ(t) jumps randomly like Brownian motion. Horizon Horizon φ(x) Quantum fluctuation Inflation φ 0 0 Becomes classical 10
11 QUANTUM FLUCTUATION DURING INFLATION Quantum fluctuation brings the field to non-zero value. Classical rolling down follows φ + 3H I φ = V φ, which requires t rrr ~ d2 V φ dφ = 1 m φ If m φ H I, insufficient time to relax (slow-rolling). A non-zero VEV of the scalar field is building up. V(ϕ) ϕ min Quantum Jump Bunch, Davies (1978); Linde (1982); Hawking, Moss (1982); Starobinsky (1982); Vilenkin, Ford (1982); Starobinsky, Yokoyama (1994). Can t Roll Down Classically ϕ 11
12 LARGE INITIAL VEV OF SCALAR FIELDS A. A. Starobinsky (1982) A. Vilenkin (1982) Fokker-Planck equation: P c φ,t = j c where j c = P c φ, t : probability distribution of φ H 3 P c 8π 2 + P c H Massless scalar, the field undergoes random walks φ 0 φ 2 H I t = H I 22 Massive case V φ = 1 2 m2 φ 2 : φ 0 3 H I 8π 2 m For V(φ) = λ 4 φ4 : φ H I /λ 1/4 In general, V φ 0 ~ H I 4 dd dd N, N: number of e-folds 2 12
13 LARGE HIGGS VEV DURING INFLATION Higgs has a shallow potential at large scale (small λ). Large Higgs vacuum expectation value (VEV) during inflation. For inflationary scale Λ I = GeV, the Hubble rate Λ I 2 H I = ~10 11 GeV, and λ~0. 00, the Higgs VEV after 3M pp inflation is φ H I /λ 1/4 ~ GeV. For such a large VEV, the Higgs field can be sensitive to higher dimensional operators. 13
14 HIGGS FIELD RELAXATION 14
15 POST-INFLATIONARY HIGGS RELAXATION As the inflation end, the H drops. When H < m φ,eff, the Higgs field can relax classically φ t + 33 t φ t + V eff φ, T t = 0 φ V eff (φ, T) is the finite temperature effective potential. Higgs field oscillates with decreasing amplitude due to the Hubble friction. Relaxation time /3 1 t rrr = t RR if thermal mass dominates V a T T RR t α RR 2 T 2 T 2 φ 2 t rrr = 6. 99/ λφ 0 if the zero T dominates V λφ 4 /4 Typically during reheating or right after reheating. 15
16 POST-INFLATIONARY HIGGS RELAXATION Thermal mass dominated Zero T potential dominated What can this do for us? Breaks time reversal symmetry, and provides the out of thermal equilibrium condition. An important epoch for the matter-antimatter asymmetry! 16
17 POST-INFLATIONARY HIGGS RELAXATION If the thermal mass dominates, V φ, T 1 2 α T 2 T 2 φ 2 where α T λ g g y t at μ = GeV. The equation of motion is approximately A solution: φ t + 2 t φ t + α T 2 T RR φ t = φ 0 Γ J 2 3 where β = T RR t RR and x = t/t RR. 2 t t RR 4α T β 3 φ t = 0 4 x3 1 α T β 2 3 x 17
18 LEPTOGENESIS VIA THE RELAXATION OF THE HIGGS FIELD 18
19 SAKHAROV CONDITIONS Andrei D. Sakharov (1967) Successfully Leptogenesis requires: 1. Deviation from thermal equilibrium Post-inflationary Higgs relaxation 2. C and CC violations CC phase in the quark sector (not enough), higher dimensional operator, 3. Lepton number violation Right-handed Majorana neutrino, others 19
20 EFFECTIVE OPERATOR M. E. Shaposhnikov (1987), M. E. Shaposhnikov (1988) Consider the effective operator: O 6 = 1 Λ n 2 φ2 g 2 WW g 2 BB, W and B: SS 2 L and U 1 Y gauge fields W : dual tensor of W Λ n : energy scale when the operator is relevant In standard model, integrating out a loop with all 6 quarks: But suppressed by small Yukawa and small CC phase 20
21 EFFECTIVE OPERATOR O 6 = 1 Λ n 2 φ2 g 2 WW g 2 BB Replace the SM fermions by heavy states that carry SS 2 charge. Scale: Λ n = M n mass (must not from the SM Higgs) or Λ n = T temperature 21
22 EFFECTIVE CHEMICAL POTENTIAL Dine et. al. (1991) Cohen, Kaplan, Nelson (1991) O 6 = 1 Λ n 2 φ2 g 2 WW g 2 BB Using electroweak anomaly equation, we have O 6 = 1 2 Λ φ 2 μ μ j B+L, n μ where j B+L is the B + L fermion current. Integration by part: O 6 = 1 Λ n 2 μ φ 2 μ j B+L Similar to the one use by spontaneous baryogenesis. Breaks CPT spontaneously while φ is changing! Sakharov conditions doesn t have to be satisfied explicitly in this form. 22
23 EFFECTIVE CHEMICAL POTENTIAL O 6 = 1 Λ n 2 μ φ 2 μ j B+L Effective chemical potential for baryon and lepton number: μ eff = 1 Λ n 2 t φ 2 Shifts the energy levels between fermions and anti-fermions while Higgs is rolling down (φ 0). V(ϕ) Scalar VEV Rolls Down Reheating Leads to l, q l, q ϕ 23
24 LEPTON NUMBER VIOLATION Last ingredient: Right-handed neutrino N R with Majorana mass term M R. The processes for ΔΔ = 2: ν L h 0 ν L h 0 ν L ν L h 0 h 0 ν L ν L h 0 h 0 For m ν ~0. 1 ev, σ R ~ Σ 2 im ν,i ~10 33 GeV v EE 24
25 EVOLUTION OF LEPTON ASYMMETRY LY, Pearce, Kusenko Phys. Rev. D92 (2015) Boltzman equation: n L + 33n L 2 π 2 T3 σ R n L 2 π 2 μ eeet 2 Λ I = GeV, Γ I = 10 8 GeV, T RR = GeV, and φ 0 = GeV. For μ eff M n 2 case, choose M n = GeV. Could be the origin of matter-antimatter asymmetry! 25
26 SUMMARY Our universe seems to be right on the meta-stable region. The quartic coupling of the Higgs potential turns negative giving a shallow potential. Higgs can obtain large vacuum expectation during inflation. The relaxation of the Higgs VEV happens during reheating. Higgs relaxation provides the out of thermal equilibrium condition and breaks T invariant. Leptogenesis via the Higgs relaxation is possible. Higgs relaxation is an important epoch in the early universe. Thanks for your listening! 26
POST-INFLATIONARY HIGGS RELAXATION AND THE ORIGIN OF MATTER- ANTIMATTER ASYMMETRY
POST-INFLATIONARY HIGGS RELAXATION AND THE ORIGIN OF MATTER- ANTIMATTER ASYMMETRY LOUIS YANG ( 楊智軒 ) UNIVERSITY OF CALIFORNIA, LOS ANGELES (UCLA) DEC 27, 2016 NATIONAL TSING HUA UNIVERSITY OUTLINE Big
More informationPost-Inflationary Higgs Relaxation and Leptogenesis. Louis Yang Kavli IPMU PACIFIC 2018 February 17, 2018
Post-Inflationary Higgs Relaxation and Leptogenesis Louis Yang Kavli IPMU PACIFIC 2018 February 17, 2018 Outline Motivation: the Higgs potential Quantum fluctuation during inflation Post-inflationary Higgs
More informationPostinflationary Higgs Relaxation and the Origin of Matter
Postinflationary Higgs Relaxation and the Origin of Matter Louis Yang University of California, Los Angeles Ph.D. Final Oral Presentation May 16, 2017 Outline Motivation: the Higgs potential Quantum Fluctuation
More informationLeptogenesis via Higgs Condensate Relaxation
The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Leptogenesis via Higgs Condensate Relaxation Louis Yang Department of Physics and Astronomy University of California, Los Angeles
More informationEvolution of Scalar Fields in the Early Universe
Evolution of Scalar Fields in the Early Universe Louis Yang Department of Physics and Astronomy University of California, Los Angeles PACIFIC 2015 September 17th, 2015 Advisor: Alexander Kusenko Collaborator:
More informationLeptogenesis via the Relaxation of Higgs and other Scalar Fields
Leptogenesis via the Relaxation of Higgs and other Scalar Fields Louis Yang Department of Physics and Astronomy University of California, Los Angeles PACIFIC 2016 September 13th, 2016 Collaborators: Alex
More informationTesting Higgs Relaxation Leptogenesis: Why Isocurvature Is More Promising Than CP Violation
Testing Higgs Relaxation Leptogenesis: Why Isocurvature Is More Promising Than CP Violation Lauren Pearce University of Illinois, Urbana-Champaign Based on: Alexander Kusenko, LP, Louis Yang, Phys.Rev.Lett.
More informationThe Matter-Antimatter Asymmetry and New Interactions
The Matter-Antimatter Asymmetry and New Interactions The baryon (matter) asymmetry The Sakharov conditions Possible mechanisms A new very weak interaction Recent Reviews M. Trodden, Electroweak baryogenesis,
More informationPostinflationary Higgs relaxation and the origin of matter-antimatter asymmetry
Postinflationary Higgs relaxation and the origin of matter-antimatter asymmetry Alexander Kusenko, 1, 2 Lauren Pearce, and Louis Yang 1 1 Department of Physics and Astronomy, University of California,
More informationLeptogenesis via varying Weinberg operator
Silvia Pascoli IPPP, Department of Physics, Durham University, Durham DH1 3LE, United Kingdom E-mail: silvia.pascoli@durham.ac.uk Jessica Turner Theoretical Physics Department, Fermi National Accelerator
More informationSM*A*S*H. Standard Model * Axion * See-saw * Hidden PQ scalar inflation. Andreas Ringwald (DESY)
SM*A*S*H Standard Model * Axion * See-saw * Hidden PQ scalar inflation Andreas Ringwald (DESY) From the Vacuum to the Universe Kitzbühel, Austria 26 June 1 July 2016 [Guillermo Ballesteros, Javier Redondo,
More informationLeptogenesis with Composite Neutrinos
Leptogenesis with Composite Neutrinos Based on arxiv:0811.0871 In collaboration with Yuval Grossman Cornell University Friday Lunch Talk Yuhsin Tsai, Cornell University/CIHEP Leptogenesis with Composite
More informationBaryogenesis. David Morrissey. SLAC Summer Institute, July 26, 2011
Baryogenesis David Morrissey SLAC Summer Institute, July 26, 2011 Why is There More Matter than Antimatter? About 5% of the energy density of the Universe consists of ordinary (i.e. non-dark) matter. By
More informationStatus Report on Electroweak Baryogenesis
Outline Status Report on Electroweak Baryogenesis Thomas Konstandin KTH Stockholm hep-ph/0410135, hep-ph/0505103, hep-ph/0606298 Outline Outline 1 Introduction Electroweak Baryogenesis Approaches to Transport
More informationRecent progress in leptogenesis
XLIII rd Rencontres de Moriond Electroweak Interactions and Unified Theories La Thuile, Italy, March 1-8, 2008 Recent progress in leptogenesis Steve Blanchet Max-Planck-Institut for Physics, Munich March
More informationWill Planck Observe Gravity Waves?
Will Planck Observe Gravity Waves? Qaisar Shafi Bartol Research Institute Department of Physics and Astronomy University of Delaware in collaboration with G. Dvali, R. K. Schaefer, G. Lazarides, N. Okada,
More informationBig Bang Nucleosynthesis
Big Bang Nucleosynthesis George Gamow (1904-1968) 5 t dec ~10 yr T dec 0.26 ev Neutrons-protons inter-converting processes At the equilibrium: Equilibrium holds until 0 t ~14 Gyr Freeze-out temperature
More informationRelating the Baryon Asymmetry to WIMP Miracle Dark Matter
Brussels 20/4/12 Relating the Baryon Asymmetry to WIMP Miracle Dark Matter PRD 84 (2011) 103514 (arxiv:1108.4653) + PRD 83 (2011) 083509 (arxiv:1009.3227) John McDonald, LMS Consortium for Fundamental
More informationFlavor Models with Sterile Neutrinos. NuFact 11 Geneva, Aug, He Zhang
Flavor Models with Sterile Neutrinos NuFact 11 Geneva, Aug, 2011 Contents: Sterile neutrinos in ν-osc. and 0νββ decays Mechanisms for light sterile neutrino masses Flavor symmetry with sterile neutrinos
More informationDark Matter and Gauged Baryon Number
Dark Matter and Gauged Baryon Number Sebastian Ohmer Collaborators: Pavel Fileviez Pérez and Hiren H. Patel P. Fileviez Pérez, SO, H. H. Patel, Phys.Lett.B735(2014)[arXiv:1403.8029] P.Fileviez Pérez, SO,
More informationThe Higgs Boson and Electroweak Symmetry Breaking
The Higgs Boson and Electroweak Symmetry Breaking 1. Minimal Standard Model M. E. Peskin Chiemsee School September 2014 The Higgs boson has an odd position in the Standard Model of particle physics. On
More informationThe first one second of the early universe and physics beyond the Standard Model
The first one second of the early universe and physics beyond the Standard Model Koichi Hamaguchi (University of Tokyo) @ Colloquium at Yonsei University, November 9th, 2016. Credit: X-ray: NASA/CXC/CfA/M.Markevitch
More informationWho is afraid of quadratic divergences? (Hierarchy problem) & Why is the Higgs mass 125 GeV? (Stability of Higgs potential)
Who is afraid of quadratic divergences? (Hierarchy problem) & Why is the Higgs mass 125 GeV? (Stability of Higgs potential) Satoshi Iso (KEK, Sokendai) Based on collaborations with H.Aoki (Saga) arxiv:1201.0857
More informationMinimal Extension of the Standard Model of Particle Physics. Dmitry Gorbunov
Minimal Extension of the Standard Model of Particle Physics Dmitry Gorbunov Institute for Nuclear Research, Moscow, Russia 14th Lomonosov Conference on Elementary Paticle Physics, Moscow, MSU, 21.08.2009
More informationSolar and atmospheric neutrino mass splitting with SMASH model
Solar and atmospheric neutrino mass splitting with SMASH model C.R. Das 1, Katri Huitu, Timo Kärkkäinen 3 1 Bogoliubov Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, Joliot-Curie
More informationDynamics of a two-step Electroweak Phase Transition
Dynamics of a two-step Electroweak Phase Transition May 2, 2014 ACFI Higgs Portal Workshop in Collaboration with Pavel Fileviez Pérez Michael J. Ramsey-Musolf Kai Wang hiren.patel@mpi-hd.mpg.de Electroweak
More informationThe 1-loop effective potential for the Standard Model in curved spacetime
The 1-loop effective potential for the Standard Model in curved spacetime arxiv:1804.02020 (JHEP) The 1-loop effective potential for the SM in curved spacetime arxiv:1809.06923 (Review) Cosmological Aspects
More informationThe Standard Model of particle physics and beyond
The Standard Model of particle physics and beyond - Lecture 3: Beyond the Standard Model Avelino Vicente IFIC CSIC / U. Valencia Physics and astrophysics of cosmic rays in space Milano September 2016 1
More informationAstroparticle Physics at Colliders
Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29 Contents 1) Introduction:
More informationLecture 18 - Beyond the Standard Model
Lecture 18 - Beyond the Standard Model Why is the Standard Model incomplete? Grand Unification Baryon and Lepton Number Violation More Higgs Bosons? Supersymmetry (SUSY) Experimental signatures for SUSY
More informationPHYSICS BEYOND SM AND LHC. (Corfu 2010)
PHYSICS BEYOND SM AND LHC (Corfu 2010) We all expect physics beyond SM Fantastic success of SM (LEP!) But it has its limits reflected by the following questions: What is the origin of electroweak symmetry
More informationNeutrino Mass Seesaw, Baryogenesis and LHC
Neutrino Mass Seesaw, Baryogenesis and LHC R. N. Mohapatra University of Maryland Interplay of Collider and Flavor Physics workshop, CERN Blanchet,Chacko, R. N. M., 2008 arxiv:0812:3837 Why? Seesaw Paradigm
More informationRelaxion with Particle Production
Relaxion with Particle Production Gustavo Marques-Tavares Stanford University with A. Hook: 1607.01786 Why is the Higgs mass small? m 2 h? Symmetry +? µ 2 Symmetry Where are you? +? µ 2 Why is the Higgs
More informationAstroparticle Physics and the LC
Astroparticle Physics and the LC Manuel Drees Bonn University Astroparticle Physics p. 1/32 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/32 Contents 1) Introduction:
More informationINFLATION. - EARLY EXPONENTIAL PHASE OF GROWTH OF SCALE FACTOR (after T ~ TGUT ~ GeV)
INFLATION - EARLY EXPONENTIAL PHASE OF GROWTH OF SCALE FACTOR (after T ~ TGUT ~ 10 15 GeV) -Phenomenologically similar to Universe with a dominant cosmological constant, however inflation needs to end
More informationarxiv: v3 [hep-ph] 11 Aug 2015
HGU-CAP-037 EPHOU-15-0009 arxiv:1505.0194v3 [hep-ph] 11 Aug 015 Dilution of axion dark radiation by thermal inflation Hironori Hattori, Tatsuo Kobayashi, Naoya Omoto Department of Physics, Hokkaido University,
More informationElectroweak and Higgs Physics
Electroweak and Higgs Physics Lecture 2 : Higgs Mechanism in the Standard and Supersymmetric Models Alexei Raspereza DESY Summer Student Program Hamburg August 2017 Standard Model (Summary) Building blocks
More informationElectroweak phase transition in the early universe and Baryogenesis
Electroweak phase transition in the early universe and Baryogenesis Arka Banerjee December 14, 2011 Abstract In the Standard Model, it is generally accepted that elementary particles get their masses via
More informationBaryo- and leptogenesis. Purpose : explain the current excess of matter/antimatter. Is there an excess of matter?
Baryo- and leptogenesis Purpose : explain the current excess of matter/antimatter Is there an excess of matter? Baryons: excess directly observed; Antibaryons seen in cosmic rays are compatible with secondary
More informationZhong-Zhi Xianyu (CMSA Harvard) Tsinghua June 30, 2016
Zhong-Zhi Xianyu (CMSA Harvard) Tsinghua June 30, 2016 We are directly observing the history of the universe as we look deeply into the sky. JUN 30, 2016 ZZXianyu (CMSA) 2 At ~10 4 yrs the universe becomes
More informationHiggs boson, neutral leptons, and cosmology. Mikhail Shaposhnikov. LPTHE, Paris 2 June 2014
Higgs boson, neutral leptons, and cosmology Mikhail Shaposhnikov LPTHE, Paris 2 June 2014 Paris, 2 June, 2014 p. 1 July 4, 2012, Higgs at ATLAS and CMS Events / 2 GeV Events Bkg weights / 2 GeV Σ 3500
More informationNeutrinos. Riazuddin National Centre for Physics Quaid-i-Azam University Campus. Islamabad.
Neutrinos Riazuddin National Centre for Physics Quaid-i-Azam University Campus Islamabad. Neutrino was the first particle postulated by a theoretician: W. Pauli in 1930 to save conservation of energy and
More informationIntroduction to Cosmology
Introduction to Cosmology Subir Sarkar CERN Summer training Programme, 22-28 July 2008 Seeing the edge of the Universe: From speculation to science Constructing the Universe: The history of the Universe:
More informationDynamical CP violation in the Early Universe
Dynamical CP violation in the Early Universe Balaji Katlai (McGill University) In collaboration with T. Biswas, R.H. Brandenberger, David London Phys.Lett. B595, 22 (2004) DESY workshop, 2004. p.1/10 .
More informationDynamics of cosmological relaxation after reheating
Dynamics of cosmological relaxation after reheating Hyungjin Kim KAIST & IBS CTPU The 3rd IBS-MultiDark-IPPP Workshop November 24 2016 [Graham, Kaplan, Rajendran 15] m 2 h( 0 ) (90 GeV) 2 [Graham, Kaplan,
More informationEffects of Reheating on Leptogenesis
Effects of Reheating on Leptogenesis Florian Hahn-Woernle Max-Planck-Institut für Physik München 2. Kosmologietag Florian Hahn-Woernle (MPI-München) Effects of Reheating on Leptogenesis Kosmologietag 2007
More informationScale invariance and the electroweak symmetry breaking
Scale invariance and the electroweak symmetry breaking Archil Kobakhidze School of Physics, University of Melbourne R. Foot, A.K., R.R. Volkas, Phys. Lett. B 655,156-161,2007 R. Foot, A.K., K.L. Mcdonald,
More informationarxiv:astro-ph/ v4 5 Jun 2006
BA-06-12 Coleman-Weinberg Potential In Good Agreement With WMAP Q. Shafi and V. N. Şenoğuz Bartol Research Institute, Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA
More informationTeV-scale type-i+ii seesaw mechanism and its collider signatures at the LHC
TeV-scale type-i+ii seesaw mechanism and its collider signatures at the LHC Wei Chao (IHEP) Outline Brief overview of neutrino mass models. Introduction to a TeV-scale type-i+ii seesaw model. EW precision
More informationKatsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy
11/14/12 Katsushi Arisaka 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Seven Phases of Cosmic Evolution 11/14/12 Katsushi Arisaka
More informationBaryon asymmetry from hypermagnetic helicity in inflationary cosmology
Baryon asymmetry from hypermagnetic helicity in inflationary cosmology Reference: Physical Review D 74, 123504 (2006) [e-print arxiv:hep-ph/0611152] Particle and field seminar at National Tsing Hua University
More informationgeneration Outline Outline Motivation Electroweak constraints Selected flavor constraints in B and D sector Conclusion Nejc Košnik
th Discovery Discovery of of the the 4 4th generation generation Outline Outline Motivation Electroweak constraints Selected flavor constraints in B and D sector Conclusion 1 Introduction Introduction
More informationHiggs Inflation Mikhail Shaposhnikov SEWM, Montreal, 29 June - 2 July 2010
Higgs Inflation Mikhail Shaposhnikov SEWM, Montreal, 29 June - 2 July 2010 SEWM, June 29 - July 2 2010 p. 1 Original part based on: F. Bezrukov, M. S., Phys. Lett. B 659 (2008) 703 F. Bezrukov, D. Gorbunov,
More informationHiggs Vacuum Stability and Physics Beyond the Standard Model Archil Kobakhidze
Higgs Vacuum Stability and Physics Beyond the Standard Model Archil Kobakhidze AK & A. Spencer-Smith, Phys Lett B 722 (2013) 130 [arxiv:1301.2846] AK & A. Spencer-Smith, JHEP 1308 (2013) 036 [arxiv:1305.7283]
More informationPhysics Spring Week 7 INFLATION, BEFORE AND AFTER
Physics 224 - Spring 2010 Week 7 INFLATION, BEFORE AND AFTER Joel Primack University of California, Santa Cruz Motivations for Inflation Joel Primack, in Formation of Structure in the Universe, ed. Dekel
More informationThe Origin of Matter. Koichi Funakubo Dept. Physics Saga University. NASA Hubble Space Telescope NGC 4911
The Origin of Matter Koichi Funakubo Dept. Physics Saga University NASA Hubble Space Telescope NGC 4911 fundamental theory of elementary particles Local Quantum Field Theory causality relativistic quantum
More informationG.F. Giudice. Theoretical Implications of the Higgs Discovery. DaMeSyFla Meeting Padua, 11 April 2013
Theoretical Implications of the Higgs Discovery G.F. Giudice DaMeSyFla Meeting Padua, 11 April 2013 GFG, A. Strumia, arxiv:1108.6077 J. Elias-Miró, J.R. Espinosa, GFG, G. Isidori, A. Riotto, A. Strumia,
More informationA Supersymmetric Two-Field Relaxion Model
A Supersymmetric Two-Field Relaxion Model Natsumi Nagata Univ. of Minnesota Phenomenology 2016 May. 10, 2016 University of Pi
More informationInflation, Gravity Waves, and Dark Matter. Qaisar Shafi
Inflation, Gravity Waves, and Dark Matter Qaisar Shafi Bartol Research Institute Department of Physics and Astronomy University of Delaware Feb 2015 University of Virginia Charlottesville, VA Units ћ =
More informationNatural Nightmares for the LHC
Dirac Neutrinos and a vanishing Higgs at the LHC Athanasios Dedes with T. Underwood and D. Cerdeño, JHEP 09(2006)067, hep-ph/0607157 and in progress with F. Krauss, T. Figy and T. Underwood. Clarification
More informationA model of the basic interactions between elementary particles is defined by the following three ingredients:
I. THE STANDARD MODEL A model of the basic interactions between elementary particles is defined by the following three ingredients:. The symmetries of the Lagrangian; 2. The representations of fermions
More informationRatchet Baryogenesis during Reheating
Ratchet Baryogenesis during Reheating Neil D. Barrie Kavli IPMU (WPI) February 17, 2018 K. Bamba, N. B., A. Sugamoto, T. Takeuchi and K. Yamashita, arxiv:1610.03268, and upcoming work. N. D. Barrie (Kavli
More informationGravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe
Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe Raghavan Rangarajan Physical Research Laboratory Ahmedabad with N. Sahu, A. Sarkar, N. Mahajan OUTLINE THE MATTER-ANTIMATTER ASYMMETRY
More informationNon-Abelian SU(2) H and Two-Higgs Doublets
Non-Abelian SU(2) H and Two-Higgs Doublets Technische Universität Dortmund Wei- Chih Huang 25 Sept 2015 Kavli IPMU arxiv:1510.xxxx(?) with Yue-Lin Sming Tsai, Tzu-Chiang Yuan Plea Please do not take any
More informationHiggs Boson Phenomenology Lecture I
iggs Boson Phenomenology Lecture I Laura Reina TASI 2011, CU-Boulder, June 2011 Outline of Lecture I Understanding the Electroweak Symmetry Breaking as a first step towards a more fundamental theory of
More informationOverview of mass hierarchy, CP violation and leptogenesis.
Overview of mass hierarchy, CP violation and leptogenesis. (Theory and Phenomenology) Walter Winter DESY International Workshop on Next Generation Nucleon Decay and Neutrino Detectors (NNN 2016) 3-5 November
More informationThe mass of the Higgs boson
The mass of the Higgs boson LHC : Higgs particle observation CMS 2011/12 ATLAS 2011/12 a prediction Higgs boson found standard model Higgs boson T.Plehn, M.Rauch Spontaneous symmetry breaking confirmed
More informationSupersymmetry in Cosmology
Supersymmetry in Cosmology Raghavan Rangarajan Ahmedabad University raghavan@ahduni.edu.in OUTLINE THE GRAVITINO PROBLEM SUSY FLAT DIRECTIONS AND THEIR COSMOLOGIAL IMPLICATIONS SUSY DARK MATTER SUMMARY
More informationIntroduction to Particle Physics. HST July 2016 Luis Alvarez Gaume 1
Introduction to Particle Physics HST July 2016 Luis Alvarez Gaume 1 Basics Particle Physics describes the basic constituents of matter and their interactions It has a deep interplay with cosmology Modern
More informationThe Standard model Higgs boson as the inflaton
The Standard model Higgs boson as the inflaton F. Bezrukov M. Shaposhnikov EPFL, Lausanne, Suisse Institute for Nuclear Research, Moscow, Russia PONT d Avignon 08 23 May 2008 Phys. Lett. B 659, 703 (2008)
More informationA String Model for Preons and the Standard Model Particles. Abstract
March 5, 013 A String Model for Preons and the Standard Model Particles Risto Raitio 1 030 Espoo, Finland Abstract A preon model for standard model particles is proposed based on spin 1 fermion and spin
More informationMatter vs Anti-matter
Baryogenesis Matter vs Anti-matter Earth, Solar system made of baryons B Our Galaxy Anti-matter in cosmic rays p/p O(10 4 ) secondary Our Galaxy is made of baryons p galaxy p + p p + p + p + p galaxy γ
More informationBaryogenesis and Particle Antiparticle Oscillations
Baryogenesis and Particle Antiparticle Oscillations Seyda Ipek UC Irvine SI, John March-Russell, arxiv:1604.00009 Sneak peek There is more matter than antimatter - baryogenesis SM cannot explain this There
More informationNaturalizing SUSY with the relaxion and the inflaton
Naturalizing SUSY with the relaxion and the inflaton Tony Gherghetta KEK Theory Meeting on Particle Physics Phenomenology, (KEK-PH 2018) KEK, Japan, February 15, 2018 [Jason Evans, TG, Natsumi Nagata,
More informationHidden Sector Baryogenesis. Jason Kumar (Texas A&M University) w/ Bhaskar Dutta (hep-th/ ) and w/ B.D and Louis Leblond (hepth/ )
Hidden Sector Baryogenesis Jason Kumar (Texas A&M University) w/ Bhaskar Dutta (hep-th/0608188) and w/ B.D and Louis Leblond (hepth/0703278) Basic Issue low-energy interactions seem to preserve baryon
More informationA biased review of Leptogenesis. Lotfi Boubekeur ICTP
A biased review of Leptogenesis Lotfi Boubekeur ICTP Baryogenesis: Basics Observation Our Universe is baryon asymmetric. n B s n b n b s 10 11 BAU is measured in CMB and BBN. Perfect agreement with each
More informationLecture 03. The Standard Model of Particle Physics. Part II The Higgs Boson Properties of the SM
Lecture 03 The Standard Model of Particle Physics Part II The Higgs Boson Properties of the SM The Standard Model So far we talked about all the particles except the Higgs If we know what the particles
More informationTheory of CP Violation
Theory of CP Violation IPPP, Durham CP as Natural Symmetry of Gauge Theories P and C alone are not natural symmetries: consider chiral gauge theory: L = 1 4 F µνf µν + ψ L i σdψ L (+ψ R iσ ψ R) p.1 CP
More informationElectroweak baryogenesis and flavor
Electroweak baryogenesis and flavor Thomas Konstandin Utrecht, May 18, 2017 in collaboration with G. Servant, I. Baldes, S. Bruggisser The serendipity of electroweak baryogenesis Thomas Konstandin Geraldine
More informationCould the Higgs Boson be the Inflaton?
Could the Higgs Boson be the Inflaton? Michael Atkins Phys.Lett. B697 (2011) 37-40 (arxiv:1011.4179) NExT Meeting March 2012, Sussex Outline Why inflation? The Higgs as the inflaton Unitarity and Higgs
More informationDissipative and Stochastic Effects During Inflation 1
Dissipative and Stochastic Effects During Inflation 1 Rudnei O. Ramos Rio de Janeiro State University Department of Theoretical Physics McGill University Montreal, Canada September 8th, 2017 1 Collaborators:
More informationThe Scale-Symmetric Theory as the Origin of the Standard Model
Copyright 2017 by Sylwester Kornowski All rights reserved The Scale-Symmetric Theory as the Origin of the Standard Model Sylwester Kornowski Abstract: Here we showed that the Scale-Symmetric Theory (SST)
More informationElectroweak Baryogenesis in the LHC era
Electroweak Baryogenesis in the LHC era Sean Tulin (Caltech) In collaboration with: Michael Ramsey-Musolf Dan Chung Christopher Lee Vincenzo Cirigliano Bjorn Gabrecht Shin ichiro ichiro Ando Stefano Profumo
More informationModuli Problem, Thermal Inflation and Baryogenesis
Finnish-Japanese Workshop on Particle Physics 2007 Moduli Problem, Thermal Inflation and Baryogenesis Masahiro Kawasaki Institute for Cosmic Ray Research University of Tokyo Cosmological Moduli Problem
More informationParticle Physics Today, Tomorrow and Beyond. John Ellis
Particle Physics Today, Tomorrow and Beyond John Ellis Summary of the Standard Model Particles and SU(3) SU(2) U(1) quantum numbers: Lagrangian: gauge interactions matter fermions Yukawa interactions Higgs
More informationPangenesis in a Baryon-Symmetric Universe: Dark and Visible Matter via the Affleck-Dine Mechanism
Pangenesis in a Baryon-Symmetric Universe: Dark and Visible Matter via the Affleck-Dine Mechanism Kalliopi Petraki University of Melbourne (in collaboration with: R. Volkas, N. Bell, I. Shoemaker) COSMO
More informationPhoton Coupling with Matter, u R
1 / 16 Photon Coupling with Matter, u R Consider the up quark. We know that the u R has electric charge 2 3 e (where e is the proton charge), and that the photon A is a linear combination of the B and
More informationMatter over antimatter: The Sakharov conditions after 50 years
Matter over antimatter: The Sakharov conditions after 50 years Rob Timmermans On behalf of the organizers May 8, 2017 faculty of mathematics and natural sciences van swinderen institute for particle physics
More informationGauge U(1) Dark Symmetry and Radiative Light Fermion Masses
UCRHEP-T565 April 2016 arxiv:1604.01148v1 [hep-ph] 5 Apr 2016 Gauge U(1) Dark Symmetry and Radiative Light Fermion Masses Corey Kownacki 1 and Ernest Ma 1,2,3 1 Department of Physics and Astronomy, University
More informationHiggs field as the main character in the early Universe. Dmitry Gorbunov
Higgs field as the main character in the early Universe Dmitry Gorbunov Institute for Nuclear Research, Moscow, Russia Dual year Russia-Spain, Particle Physics, Nuclear Physics and Astroparticle Physics
More informationNeutrino Oscillation, Leptogenesis and Spontaneous CP Violation
Neutrino Oscillation, Leptogenesis and Spontaneous CP Violation Mu-Chun Chen Fermilab (Jan 1, 27: UC Irvine) M.-C. C & K.T. Mahanthappa, hep-ph/69288, to appear in Phys. Rev. D; Phys. Rev. D71, 351 (25)
More informationYang-Hwan Ahn Based on arxiv:
Yang-Hwan Ahn (CTPU@IBS) Based on arxiv: 1611.08359 1 Introduction Now that the Higgs boson has been discovered at 126 GeV, assuming that it is indeed exactly the one predicted by the SM, there are several
More informationMarch 30, 01 Lecture 5 of 6 @ ORICL Philosophical Society Yuri Kamyshkov/ University of Tennessee email: kamyshkov@utk.edu 1. Concept/misconception of mass in Special Relativity (March,9). and n Oscillations:
More informationStructures in the early Universe. Particle Astrophysics chapter 8 Lecture 4
Structures in the early Universe Particle Astrophysics chapter 8 Lecture 4 overview Part 1: problems in Standard Model of Cosmology: horizon and flatness problems presence of structures Part : Need for
More informationCreating Matter-Antimatter Asymmetry from Dark Matter Annihilations in Scotogenic Scenarios
Creating Matter-Antimatter Asymmetry from Dark Matter Annihilations in Scotogenic Scenarios Based on arxiv:1806.04689 with A Dasgupta, S K Kang (SeoulTech) Debasish Borah Indian Institute of Technology
More informationTo Higgs or not to Higgs
To Higgs or not to Higgs vacuum stability and the origin of mass Wolfgang Gregor Hollik DESY Hamburg Theory Group Dec 12 2016 MU Programmtag Mainz The Higgs mechanism and the origin of mass [CERN bulletin]
More informationLFV Higgs Decay in Extended Mirror Fermion Model
LFV Higgs Decay in Extended Mirror Fermion Model Chrisna Setyo Nugroho (NTNU) In Collaboration with Chia-Feng Chang (NTU), ChiaHung Vincent Chang (NTNU), and Tzu-Chiang Yuan (AS) KIAS-NCTS Joint Workshop
More informationLectures on Standard Model Effective Field Theory
Lectures on Standard Model Effective Field Theory Yi Liao Nankai Univ SYS Univ, July 24-28, 2017 Page 1 Outline 1 Lecture 4: Standard Model EFT: Dimension-six Operators SYS Univ, July 24-28, 2017 Page
More informationWhat can we learn from the 126 GeV Higgs boson for the Planck scale physics? - Hierarchy problem and the stability of the vacuum -
What can we learn from the 126 GeV Higgs boson for the Planck scale physics? - Hierarchy problem and the stability of the vacuum - Satoshi Iso Theory Center, Institute of Particles and Nuclear Studies
More informationImplications of a Heavy Z Gauge Boson
Implications of a Heavy Z Gauge Boson Motivations A (string-motivated) model Non-standard Higgs sector, CDM, g µ 2 Electroweak baryogenesis FCNC and B s B s mixing References T. Han, B. McElrath, PL, hep-ph/0402064
More information