Leptogenesis via Higgs Condensate Relaxation
|
|
- Joleen Jennings
- 6 years ago
- Views:
Transcription
1 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 TASC 2015 November 14th, 2015 Collaborator: Alexander Kusenko and Lauren Pearce Leptogenesis via Higgs Condensate Relaxation (slide 1) TASC 2015
2 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary The Motivation The recent discovery of the Higgs boson with mass M h = ± 0.4 GeV [Particle Data Group 2014] The Higgs potential V (φ) = 1 2 m2 φ λφ4 Very small or negative quartic coupling λ at high scale when consider renormalization group equation (RGE) a meta-stable electroweak vacuum Higgs potential is very shallow at high scale Scalar fields with shallow potentials can obtain large vacuum expectation values (VEVs) during inflation. Post-inflationary Higgs field relaxation possibility to account for the matter-antimatter asymmetry of the Universe. [Dario Buttazzo et al. JHEP 1312 (2013) 089] Leptogenesis via Higgs Condensate Relaxation (slide 2) TASC 2015
3 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Quantum Fluctuations during Inflation During de Sitter expansion, a scalar field can jump quantum mechanically to a nonzero field value due to quantum fluctuation. The field can also roll down classically toward its equilibrium minimum. φ + 3H φ dv (φ) = dφ Classical relaxation time: τ roll 1 [ d 2 ] 1/2 V (φ) = m eff dφ 2 If τ roll H 1 I the Hubble time scale, insufficient time for the field to roll down. Develop a large field value φ 0 during inflation. The VEV is such that V H (φ 0 ) H 4 I For the Higgs field, it obtains a VEV φ 0 λ 1/4 H I V(ϕ) ϕ min Quantum Jump Roll Down Classically ϕ Leptogenesis via Higgs Condensate Relaxation (slide 3) TASC 2015
4 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Relaxation of the Higgs Condensate during Reheating As inflation ends, the Higgs field is no longer frozen. The generated Higgs VEV then rolls down and oscillates around φ = 0 with decreasing amplitude within τ roll H 1. Φ t Φ Φ I GeV I 10 3 GeV T max GeV Λ eff Φ GeV H I GeV T Λ Φ 0 t End of Inflation at t 0 Leptogenesis via Higgs Condensate Relaxation (slide 4) TASC 2015
5 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Leptogenesis The relaxation of the Higgs condensate across the entire Universe after inflation can leads to many interesting physics. One possibility is to explain the matter-antimatter asymmetry (Baryogenesis or Leptogenesis). A. Kusenko, L. Pearce, L. Yang, Phys. Rev. Lett. 114 (2015) 6, L. Pearce, L. Yang, A. Kusenko, M. Peloso, Phys. Rev. D 92 (2015) 2, L. Yang, L. Pearce, A. Kusenko, Phys. Rev. D 92 (2015) Sakharov conditions for Baryogenesis/Leptogenesis: Out of thermal equilibrium: Time-dependent Higgs VEV CP-violation: Higher dimensional operators,... Baryon/Lepton number violation: Right-handed Majorana neutrinos Leptogenesis via Higgs Condensate Relaxation (slide 5) TASC 2015
6 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Effective Chemical Potential In the early Universe, the Higgs field might be sensitive to higher dimensional operator L 6 = 1 ( µφ 2) j µ Λ 2 B+L 1 ( tφ 2) j n Λ 2 B+L 0 n where Λ n could be temperature T or the mass scale of M n. It can be generated from loops of heavy fermions or thermal loops with the electroweak anomaly equation. As the Higgs VEV rolls down, this lowers the energy of particle and raises the energy of antiparticle. Effective chemical potential to leptons µ eff = 1 0φ 2 Λ 2 n V(ϕ) Higgs VEV Rolls Down Reheating Leads to l, q l, q ϕ Leptogenesis via Higgs Condensate Relaxation (slide 6) TASC 2015
7 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Lepton Number Violation Processes Another ingredient: Right-handed neutrino with Majorana mass M R Lepton-number-violating processes: ν Lh 0 ν Lh 0 ν Lν L h 0 h 0 & ν Lν L h 0 h 0 h 0 h 0 h 0 h 0 ν L N R N c R ν c l ν L N R N c R ν c l ν L h 0 ν c L h 0 N R N c R N R N c R ν l h 0 ν c l h 0 Leptogenesis via Higgs Condensate Relaxation (slide 7) TASC 2015
8 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Boltzmann Transport Equation If the system is in equilibrium, the lepton asymmetry will reach a value n L,eq = 2 π 2 µ efft 2. However, the interaction is not fast enough for the system to reach equilibrium asymmetry. One describes this by the Boltzmann transport equation d d n L + 3Hn L 2 = π 2 T 3 σ R (n L + 2π ) 2 µ efft 2 where n L is the lepton asymmetry. Leptogenesis via Higgs Condensate Relaxation (slide 8) TASC 2015
9 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Resulting Lepton Asymmetry log Η T Tmax First Φ crossing Μ eff T 2 Μ eff M n 2 Radiation Domination log t GeV 1 Example: Λ I = GeV, Γ I = 10 8 GeV, and T max = GeV For the blue curve, M n = GeV. The final asymmetry η = 45 2π 2 g n L T is enough to account for the asymmetry we observe today. Leptogenesis via Higgs Condensate Relaxation (slide 9) TASC 2015
10 The Motivation Quantum Fluctuations Higgs Relaxation Leptogenesis Summary Summary During inflation, the Higgs field can obtain a large VEV through quantum fluctuation. The relaxation of the Higgs condensate after inflation could create an effective chemical potential for lepton number. In the present of of lepton-number-violating processes due to right-handed neutrino, this produces sufficient lepton number to explain the asymmetry we observe today. Most importantly, the relaxation of Higgs condensate can lead to interesting phenomena. Thank you for your listening! Leptogenesis via Higgs Condensate Relaxation (slide 10) TASC 2015
11 The Higgs Field φ Mh Mt Mh Mt sign V log V GeV Electroweak Vacuum log Φ GeV Planck scale vacuum In our model, we consider the case that the second minimum is not below our electroweak minimum. Note m GeV 2. So when φ 10 2 GeV, the potential is well approximated by V H (φ) = 1 4 λ effφ 4. The λ eff around Planck scale can be approximated by the form λ eff (φ) λ min + α ln (φ/φ 0) 2. An example of the set of parameters is: λ min = , φ 0 = GeV, and α = Leptogenesis via Higgs Condensate Relaxation (slide 11) TASC 2015
12 Inflation The Universe appears to be almost homogeneous and isotropic today Inflation In the early universe, the energy density was dominated by vacuum energy. Inflation from a real scalar field: Inflaton I (x) L I = 1 2 gµν µi νi V I (I) The equation of motion is Ï+3HI+Γ II+ dv I (I) = 0, with H 2 di ( ) 2 ȧ = 8π (ρ a 3m 2 I + ρ other ) pl where we assume a uniform field configuration and a FRW spacetime ds 2 = dt 2 a (t) 2 ( dr 2 + r 2 dω 2). Leptogenesis via Higgs Condensate Relaxation (slide 12) TASC 2015
13 The Brief History of the Early Universe 1 Slow-roll (inflation) regime: Ï dv di Γ I is not active. and I 2 V. 3HI = dv di, and H2 8π = 3m 2 V I (I) pl V(I) Slow-Roll Inflaton acts like vacuum energy. a(t) e Ht Coherent Oscillations 2 Coherent oscillations regime: a (t) (t t i ) 2/3 Inflaton acts like non-relativistic particle. The Universe is matter-dominated. Inflaton then decays into relativistic particles ρ R. Tmax ΡI Λ I I Radiation- Dominated ρ I + 3Hρ I + Γ I ρ I = 0 ρ I (t) = Λ4 I a (t) 3 e Γ I t TRH Coherent Oscillations (matter like) ΡR log t End of Inflation t ' t 1 I 3 Radiation-dominated regime: a (t) (t t i ) 1/2 At t = 1/Γ I, most of the inflatons decay into ρ R, Leptogenesis via Higgs and Condensate the reheating Relaxation is complete. (slide 13) TASC 2015
14 The Hawking-Moss Tunneling If V (φ f ) V (φ i ) V (φ i ), we have S E (φ i) S E (φ f ) = 3m4 pl 8 The transition rate is then ( Γ V exp 3m4 pl 8 [ 1 V (φ 1 ] i) V (φ f ) 3m4 pl 8 ) V (φ f ) V (φ i) V (φ i) 2 Thus, the transition is not suppressed as long as V (φ f ) V (φ i) < 8 V (φ i) 2 3m 4 pl V (φ f ) V (φ i) V (φ i) 2 Leptogenesis via Higgs Condensate Relaxation (slide 14) TASC 2015
15 Isocurvature perturbations One issue for applying to Leptogenesis φ 0 = φ 2 is the average over several Hubble volumes. Each Hubble volume has different initial φ 0 value. When inflation end, each patch of the observable universe began with different value of φ 0. If L 0 φ 2 Different asymmetry in each Hubble volume Large isocurvature perturbations, which are constrained by current CMB observation. [Figure from Lauren Pearce] Leptogenesis via Higgs Condensate Relaxation (slide 15) TASC 2015
16 Isocurvature perturbations One issue for applying to Leptogenesis φ 0 = φ 2 is the average over several Hubble volumes. Each Hubble volume has different initial φ 0 value. When inflation end, each patch of the observable universe began with different value of φ 0. If L 0 φ 2 Different asymmetry in each Hubble volume Large isocurvature perturbations, which are constrained by current CMB observation. [Figure from Lauren Pearce] Leptogenesis via Higgs Condensate Relaxation (slide 15) TASC 2015
17 Isocurvature perturbations One issue for applying to Leptogenesis φ 0 = φ 2 is the average over several Hubble volumes. Each Hubble volume has different initial φ 0 value. When inflation end, each patch of the observable universe began with different value of φ 0. If L 0 φ 2 Different asymmetry in each Hubble volume Large isocurvature perturbations, which are constrained by current CMB observation. φ 0 φ 0 φ 0 [Figure from Lauren Pearce] Leptogenesis via Higgs Condensate Relaxation (slide 15) TASC 2015
18 Isocurvature perturbations One issue for applying to Leptogenesis φ 0 = φ 2 is the average over several Hubble volumes. Each Hubble volume has different initial φ 0 value. When inflation end, each patch of the observable universe began with different value of φ 0. If L 0 φ 2 Different asymmetry in each Hubble volume Large isocurvature perturbations, which are constrained by current CMB observation. [Figure from Lauren Pearce] Leptogenesis via Higgs Condensate Relaxation (slide 15) TASC 2015
19 Solutions to the isocurvature perturbation issue Solutions: 1 IC-1: Second Minimum at Large VEVs (φ v EW ) E.g. V(ϕ) L lift = φ10 Λ 6 lift Second Min. ϕ 2 IC-2: Inflaton-Higgs coupling E.g. V(ϕ) L ΦI = 1 2 M I 2n 2n 2 φ2 Very Steep Potential due to Inflaton ϕ Leptogenesis via Higgs Condensate Relaxation (slide 16) TASC 2015
20 IC-1: Second minimum at large VEV Motivations: 1 At large VEVs, Higgs potential is sensitive to higher-dimensional operators. L lift = φ10 Λ 6 lift 2 There seems to be a planckian minimum below our electroweak (EW) vacuum. Our EW vacuum is not stable. 3 A higher-dimensional operator can lift the possible planckian minimum and stablize our EW vacuum. The second minimum becomes metastable and higher than the EW vacuum. Leptogenesis via Higgs Condensate Relaxation (slide 17) TASC 2015
21 IC-1: Second minimum at large VEV The scenario: 1 Large VEV at early stage of inflation 2 The initial Higgs VEV is trapped in this second minimum (quasi-stable vacuum) at the end of inflation. 3 Reheating destablize the quasi-stable vacuum. 4 Higgs field rolls down from the second minimum. V(ϕ) H 4 Early stage of inflation Second Min. ϕ Leptogenesis via Higgs Condensate Relaxation (slide 18) TASC 2015
22 IC-1: Second minimum at large VEV The scenario: V(ϕ) 1 Large VEV at early stage of inflation 2 The initial Higgs VEV is trapped in this second minimum (quasi-stable vacuum) at the end of inflation. 3 Reheating destablize the quasi-stable vacuum. 4 Higgs field rolls down from the second minimum. H 4 Trapped Second Min. ϕ Leptogenesis via Higgs Condensate Relaxation (slide 18) TASC 2015
23 IC-1: Second minimum at large VEV The scenario: 1 Large VEV at early stage of inflation 2 The initial Higgs VEV is trapped in this second minimum (quasi-stable vacuum) at the end of inflation. 3 Reheating destablize the quasi-stable vacuum. 4 Higgs field rolls down from the second minimum. V(ϕ) Reheating Thermal correction ϕ Leptogenesis via Higgs Condensate Relaxation (slide 18) TASC 2015
24 IC-1: Second minimum at large VEV The scenario: 1 Large VEV at early stage of inflation 2 The initial Higgs VEV is trapped in this second minimum (quasi-stable vacuum) at the end of inflation. 3 Reheating destablize the quasi-stable vacuum. 4 Higgs field rolls down from the second minimum. V(ϕ) Higgs VEV Rolls Down Reheating ϕ Leptogenesis via Higgs Condensate Relaxation (slide 18) TASC 2015
25 IC-1: Second minimum at large VEV < IC1 > Λ I = GeV Γ I = 10 9 GeV ϕ 0 = GeV ϕ/ϕ T(t) ϕ 0 t Leptogenesis via Higgs Condensate Relaxation (slide 19) TASC 2015
26 IC-2: Inflaton-Higgs coupling Introduce coupling between the Higgs and inflaton field. E.g. I 2n L ΦI = 1 2 M 2n 2 φ2. Motivations: This could be obtained by integrating out heavy states in loops. Induces an large effective mass m eff,φ ( I ) = I n /M n 1 for the Higgs field when I is large. If m eff,φ ( I ) H in the early stage of inflation, the slow roll condition is not satisfied. Leptogenesis via Higgs Condensate Relaxation (slide 20) TASC 2015
27 IC-2: Inflaton-Higgs coupling 1 In the early stage of inflation, I is large. Higgs potential is steep. Slow-roll condition is not satisfied. The Higgs VEV stay at φ = 0. 2 At the last N last e-folds of inflation, I, m eff,φ ( I ) < H I, Higgs VEV starts to develop. 3 At the end of inflation, the Higgs field has obtained a VEV φ 0 = φ 2 = H I Nlast. 2π V(ϕ) φ 2 ~0 Quantum jumps Rolls down classically Early stage of inflation H 4 ϕ 4 The Higgs VEV then rolls down from φ 0. Leptogenesis via Higgs Condensate Relaxation (slide 21) TASC 2015
28 IC-2: Inflaton-Higgs coupling 1 In the early stage of inflation, I is large. Higgs potential is steep. Slow-roll condition is not satisfied. The Higgs VEV stay at φ = 0. 2 At the last N last e-folds of inflation, I, m eff,φ ( I ) < H I, Higgs VEV starts to develop. 3 At the end of inflation, the Higgs field has obtained a VEV φ 0 = φ 2 = H I Nlast. 2π V(ϕ) Last N e-folds of inflation H 4 ϕ φ 2 starts to grow 4 The Higgs VEV then rolls down from φ 0. Leptogenesis via Higgs Condensate Relaxation (slide 21) TASC 2015
29 IC-2: Inflaton-Higgs coupling 1 In the early stage of inflation, I is large. Higgs potential is steep. Slow-roll condition is not satisfied. The Higgs VEV stay at φ = 0. 2 At the last N last e-folds of inflation, I, m eff,φ ( I ) < H I, Higgs VEV starts to develop. 3 At the end of inflation, the Higgs field has obtained a VEV φ 0 = φ 2 = H I Nlast. 2π 4 The Higgs VEV then rolls down from φ 0. V(ϕ) φ 2 = H I 2 N/4π 2 End of inflation ϕ Leptogenesis via Higgs Condensate Relaxation (slide 21) TASC 2015
30 IC-2: Inflaton-Higgs coupling 1 In the early stage of inflation, I is large. Higgs potential is steep. Slow-roll condition is not satisfied. The Higgs VEV stay at φ = 0. 2 At the last N last e-folds of inflation, I, m eff,φ ( I ) < H I, Higgs VEV starts to develop. 3 At the end of inflation, the Higgs field has obtained a VEV φ 0 = φ 2 = H I Nlast. 2π 4 The Higgs VEV then rolls down from φ 0. V(ϕ) After inflation Rolls down classically ϕ Leptogenesis via Higgs Condensate Relaxation (slide 21) TASC 2015
31 IC-2: Inflaton-Higgs coupling For N last = 5 8, the isocurvature perturbation only develops on the small angular scales which are not yet constrained. ϕ/ϕ < IC2 > Λ I = GeV Γ I = 10 8 GeV N last = 8 ϕ 0 = GeV ϕ 0 t Leptogenesis via Higgs Condensate Relaxation (slide 22) TASC 2015
32 Relaxation of the Higgs field after inflation During the oscillation of the Higgs field, the Higgs condensate can decay into several product particles: Non-perturbative decay: W and Z bonsons Φ0 WT k 0,Τ log n k Λ I = GeV and Γ I = 10 9 GeV for IC-1 Perturbative decay (thermalization): top quark. Those decay channels do affect the oscillation of the Higgs field but they becomes important only after several oscillations. Leptogenesis via Higgs Condensate Relaxation (slide 23) TASC 2015
33 Perturbative decay (thermalization) to top quark Thermalization rate is comparable to the Hubble parameter only after the maximum reheating has been reached H(t) H(t) GeV t GeV 1 H(t) vs Γ H(t) through top quark for IC-1, with the parameters Λ I = GeV and Γ I = 10 9 GeV. The vertical lines: the first time the Higgs VEV crosses zero, and the time of maximum reheating, from left to right. Leptogenesis via Higgs Condensate Relaxation (slide 24) TASC 2015
Evolution 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 informationPOST-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 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 30, 2016 4TH INTERNATIONAL WORKSHOP ON DARK MATTER,
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 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 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 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 informationAstro 507 Lecture 28 April 2, 2014
Astro 507 Lecture 28 April 2, 2014 Announcements: PS 5 due now Preflight 6 posted today last PF! 1 Last time: slow-roll inflation scalar field dynamics in an expanding universe slow roll conditions constrain
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 informationScalar field dark matter and the Higgs field
Scalar field dark matter and the Higgs field Catarina M. Cosme in collaboration with João Rosa and Orfeu Bertolami Phys. Lett., B759:1-8, 2016 COSMO-17, Paris Diderot University, 29 August 2017 Outline
More informationInflation. By The amazing sleeping man, Dan the Man and the Alices
Inflation By The amazing sleeping man, Dan the Man and the Alices AIMS Introduction to basic inflationary cosmology. Solving the rate of expansion equation both analytically and numerically using different
More informationCosmology and particle physics
Cosmology and particle physics Lecture notes Timm Wrase Lecture 9 Inflation - part I Having discussed the thermal history of our universe and in particular its evolution at times larger than 10 14 seconds
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 informationCOSMIC INFLATION AND THE REHEATING OF THE UNIVERSE
COSMIC INFLATION AND THE REHEATING OF THE UNIVERSE Francisco Torrentí - IFT/UAM Valencia Students Seminars - December 2014 Contents 1. The Friedmann equations 2. Inflation 2.1. The problems of hot Big
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 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 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 informationCHAPTER 4 INFLATIONARY MODEL BUILDING. 4.1 Canonical scalar field dynamics. Non-minimal coupling and f(r) theories
CHAPTER 4 INFLATIONARY MODEL BUILDING Essentially, all models are wrong, but some are useful. George E. P. Box, 1987 As we learnt in the previous chapter, inflation is not a model, but rather a paradigm
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 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 informationHIGGS-CURVATURE COUPLING AND POST-INFLATIONARY VACUUM STABILITY
HIGGS-CURVATURE COUPLING AND POST-INFLATIONARY VACUUM STABILITY Francisco Torrentí, IFT UAM/CSIC with Daniel G. Figueroa and Arttu Rajantie (arxiv:1612.xxxxx) V Postgraduate Meeting on Theoretical Physics,
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 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 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 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 informationDark inflation. Micha l Artymowski. Jagiellonian University. December 12, 2017 COSPA arxiv:
Dark inflation Micha l Artymowski Jagiellonian University December 12, 2017 COSPA 2017 arxiv:1711.08473 (with Olga Czerwińska, M. Lewicki and Z. Lalak) Cosmic microwave background Cosmic microwave background
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 informationDark inflation. Micha l Artymowski. Jagiellonian University. January 29, Osaka University. arxiv:
Dark inflation Micha l Artymowski Jagiellonian University January 29, 2018 Osaka University arxiv:1711.08473 (with Olga Czerwińska, M. Lewicki and Z. Lalak) Cosmic microwave background Cosmic microwave
More informationPAPER 71 COSMOLOGY. Attempt THREE questions There are seven questions in total The questions carry equal weight
MATHEMATICAL TRIPOS Part III Friday 31 May 00 9 to 1 PAPER 71 COSMOLOGY Attempt THREE questions There are seven questions in total The questions carry equal weight You may make free use of the information
More informationEntropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays.
Entropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays. Kai Schmitz Deutsches Elektronen-Synchrotron DESY, Hamburg, Germany Based on arxiv:1008.2355 [hep-ph] and arxiv:1104.2750 [hep-ph].
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 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 informationarxiv: v1 [hep-ph] 25 Jan 2008
Effects of reheating on leptogenesis arxiv:0801.3972v1 [hep-ph] 25 Jan 2008 F. Hahn-Woernle and M. Plümacher Max Planck Institute for Physics, Föhringer Ring 6, 80805 Munich, Germany Abstract We study
More informationElectroweak baryogenesis in the two Higgs doublet model
Michael Seniuch Bielefeld University 1 Electroweak baryogenesis in the two Higgs doublet model M. Seniuch, Bielefeld University COSMO 05 Bonn August 2005 Work is done in collaboration with Lars Fromme
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 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 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 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 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 informationInflation and the origin of structure in the Universe
Phi in the Sky, Porto 0 th July 004 Inflation and the origin of structure in the Universe David Wands Institute of Cosmology and Gravitation University of Portsmouth outline! motivation! the Primordial
More informationGuido D Amico Center for Cosmology and Particle Physics New York University. Unwinding Inflation
Guido D Amico Center for Cosmology and Particle Physics New York University Unwinding Inflation New Lights in Cosmology from the CMB ICTP Trieste, Summer 2013 with Roberto Gobbetti, Matthew Kleban, Marjorie
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 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 informationPREHEATING THE UNIVERSE IN HYBRID INFLATION
PREHEATING THE UNIVERSE IN HYBRID INFLATION JUAN GARCÍA-BELLIDO Theory Division, C.E.R.N., CH-1211 Genève 23, Switzerland One of the fundamental problems of modern cosmology is to explain the origin of
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 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 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 informationWe can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years
² ² ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter:
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 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 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 informationGravitational waves from the early Universe
Gravitational waves from the early Universe Part 2 Sachiko Kuroyanagi (Nagoya University) 26 Aug 2017 Summer Institute 2017 GWs from inflation Inflation Accelerated expansion in the early Universe Solves
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 informationInflationary cosmology from higher-derivative gravity
Inflationary cosmology from higher-derivative gravity Sergey D. Odintsov ICREA and IEEC/ICE, Barcelona April 2015 REFERENCES R. Myrzakulov, S. Odintsov and L. Sebastiani, Inflationary universe from higher-derivative
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 informationExact Inflationary Solution. Sergio del Campo
Exact Inflationary Solution Sergio del Campo Instituto de Física Pontificia Universidad Católica de Valparaíso Chile I CosmoSul Rio de Janeiro, 1 al 5 de Agosto, 2011 Inflation as a paradigm. Models Slow-roll
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 informationGravitation et Cosmologie: le Modèle Standard Cours 8: 6 fevrier 2009
Particules Élémentaires, Gravitation et Cosmologie Année 2008-09 Gravitation et Cosmologie: le Modèle Standard Cours 8: 6 fevrier 2009 Le paradigme inflationnaire Homogeneity and flatness problems in HBB
More informationCosmic Bubble Collisions
Outline Background Expanding Universe: Einstein s Eqn with FRW metric Inflationary Cosmology: model with scalar field QFTà Bubble nucleationà Bubble collisions Bubble Collisions in Single Field Theory
More informationCosmological Relaxation of the Electroweak Scale
the Relaxion Cosmological Relaxation of the Electroweak Scale with P. Graham and D. E. Kaplan arxiv: 1504.07551 The Hierarchy Problem The Higgs mass in the standard model is sensitive to the ultraviolet.
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 informationMIAMI 2012 December 13-20, 2012, Fort Lauderdale, Florida, USA
NEWS FROM LHC: ARE WE LIVING IN A METASTABLE VACUUM? Vincenzo Branchina and Emanuele Messina Department of Physics, University of Catania, Italy and INFN, Sezione di Catania, Italy MIAMI 01 December 13-0,
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 informationPriming the BICEP. Wayne Hu Chicago, March BB
Priming the BICEP 0.05 0.04 0.03 0.02 0.01 0 0.01 BB 0 50 100 150 200 250 300 Wayne Hu Chicago, March 2014 A BICEP Primer How do gravitational waves affect the CMB temperature and polarization spectrum?
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 informationHolographic Model of Cosmic (P)reheating
Holographic Model of Cosmic (P)reheating Yi-Fu Cai 蔡一夫 University of Science & Technology of China New perspectives on Cosmology, APCTP, Feb 13 th 2017 In collaboration with S. Lin, J. Liu & J. Sun, Based
More informationSpacetime curvature and Higgs stability during and after inflation
Spacetime curvature and Higgs stability during and after inflation arxiv:1407.3141 (PRL 113, 211102) arxiv:1506.04065 Tommi Markkanen 12 Matti Herranen 3 Sami Nurmi 4 Arttu Rajantie 2 1 King s College
More informationPhysics 133: Extragalactic Astronomy and Cosmology. Week 8
Physics 133: Extragalactic Astronomy and Cosmology Week 8 Outline for Week 8 Primordial Nucleosynthesis Successes of the standard Big Bang model Olbers paradox/age of the Universe Hubble s law CMB Chemical/Physical
More informationFalsifying High-Scale Leptogenesis at the LHC
Falsifying High-Scale Leptogenesis at the LHC based on Frank F. Deppisch, JH, Martin Hirsch Phys. Rev. Lett. 112, 221601 (2014), arxiv: 1312.4447 [hep-ph] University College London 21/07/2104 SUSY 2014,
More informationClassical Dynamics of Inflation
Preprint typeset in JHEP style - HYPER VERSION Classical Dynamics of Inflation Daniel Baumann School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540 http://www.sns.ias.edu/ dbaumann/
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 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 informationIntroduction to Inflation
Introduction to Inflation Miguel Campos MPI für Kernphysik & Heidelberg Universität September 23, 2014 Index (Brief) historic background The Cosmological Principle Big-bang puzzles Flatness Horizons Monopoles
More informationExtending classical big bang theory
Chapter 21 Extending classical big bang theory The big bang is our standard model for the origin of the Universe and has been for almost half a century. This place in well earned. At a broader conceptual
More informationMATHEMATICAL TRIPOS Part III PAPER 53 COSMOLOGY
MATHEMATICAL TRIPOS Part III Wednesday, 8 June, 2011 9:00 am to 12:00 pm PAPER 53 COSMOLOGY Attempt no more than THREE questions. There are FOUR questions in total. The questions carry equal weight. STATIONERY
More informationHot Big Bang model: early Universe and history of matter
Hot Big Bang model: early Universe and history of matter nitial soup with elementary particles and radiation in thermal equilibrium. adiation dominated era (recall energy density grows faster than matter
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 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 informationIntroduction to Quantum fields in Curved Spaces
Introduction to Quantum fields in Curved Spaces Tommi Markkanen Imperial College London t.markkanen@imperial.ac.uk April/June-2018 Solvalla QFT in curved spacetime 1 / 35 Outline 1 Introduction 2 Cosmological
More informationThe early and late time acceleration of the Universe
The early and late time acceleration of the Universe Tomo Takahashi (Saga University) March 7, 2016 New Generation Quantum Theory -Particle Physics, Cosmology, and Chemistry- @Kyoto University The early
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 informationElectroweak-scale Right-handed Neutrino Model And 126 GeV Higgs-like Particle
Electroweak-scale Right-handed Neutrino Model And 126 GeV Higgs-like Particle Ajinkya S. Kamat ask4db@virginia.edu http://people.virginia.edu/ ask4db With Prof. P. Q. Hung and Vinh Van Hoang (paper in
More informationInflationary density perturbations
Cosener s House 7 th June 003 Inflationary density perturbations David Wands Institute of Cosmology and Gravitation University of Portsmouth outline! some motivation! Primordial Density Perturbation (and
More informationHIGGS INFLATION & VACUUM STABILITY
HIGGS INFLATION & VACUUM STABILITY Javier Rubio based on Phys. Rev. D 92, 083512 F. Bezrukov, J.R., M.Shaposhnikov Outline Could the Higgs field itself be responsible for inflation? 1. Reminder of inflation/
More informationDark Radiation and Inflationary Freedom
Dark Radiation and Inflationary Freedom Based on [SG et al., JCAP 1504 (2015) 023] [Di Valentino et al., PRD 91 (2015) 123505] Stefano Gariazzo University of Torino, INFN of Torino http://personalpages.to.infn.it/~gariazzo/
More informationCP Violation, Baryon violation, RPV in SUSY, Mesino Oscillations, and Baryogenesis
CP Violation, Baryon violation, RPV in SUSY, Mesino Oscillations, and Baryogenesis David McKeen and AEN, arxiv:1512.05359 Akshay Ghalsasi, David McKeen, AEN., arxiv:1508.05392 (Thursday: Kyle Aitken, David
More informationNeutrinos and Fundamental Symmetries: L, CP, and CP T
Neutrinos and Fundamental Symmetries: L, CP, and CP T Outstanding issues Lepton number (L) CP violation CP T violation Outstanding issues in neutrino intrinsic properties Scale of underlying physics? (string,
More informationAstronomy, Astrophysics, and Cosmology
Astronomy, Astrophysics, and Cosmology Luis A. Anchordoqui Department of Physics and Astronomy Lehman College, City University of New York Lesson X April 19, 2016 arxiv:0706.1988 L. A. Anchordoqui (CUNY)
More informationSterile Neutrinos in Cosmology and Astrophysics
Kalliopi Petraki (UCLA) October 27, 2008 Particle Physics Neutrino Oscillation experiments: neutrinos have mass Cosmology and Astrophysics Plenty of unexplained phenomena Dark Matter Pulsar Kicks Supernova
More informationCalculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter
Calculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter, March 8, 2017. arxiv:1612.02793, with Anirban Biswas. Aritra Gupta Why Non-Thermal? 1 / 31 The most widely studied
More informationPreheating in the Higgs as Inflaton Model
Preheating in the Higgs as Inflaton Model Why is preheating interesting? Higgs as inflaton model Relevant physics: nonadiabatic particle production particle decay, thermalization of decay daughters medium
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 informationOddities of the Universe
Oddities of the Universe Koushik Dutta Theory Division, Saha Institute Physics Department, IISER, Kolkata 4th November, 2016 1 Outline - Basics of General Relativity - Expanding FRW Universe - Problems
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 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 informationLeptogenesis from a First-Order Lepton- Number Breaking Phase Transition
Leptogenesis from a First-Order Lepton- umber Breaking Phase Transition Andrew Long TeVPA 2017 at Ohio State University Aug 10, 2017 based on work with Andrea Tesi & Lian-Tao Wang (1703.04902 & JHEP) Bubbles!
More informationTriple unification of inflation, dark matter and dark energy
Triple unification of inflation, dark matter and dark energy May 9, 2008 Leonard Susskind, The Anthropic Landscape of String Theory (2003) A. Liddle, A. Ureña-López, Inflation, dark matter and dark energy
More informationHiggs Physics and Cosmology
Higgs Physics and Cosmology Koichi Funakubo Department of Physics, Saga University 1 This year will be the year of Higgs particle. The discovery of Higgs-like boson will be reported with higher statistics
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 14 Dec. 2, 2015 Today The Inflationary Universe Origin of Density Perturbations Gravitational Waves Origin and Evolution of
More information