Post-Inflationary Higgs Relaxation and Leptogenesis. Louis Yang Kavli IPMU PACIFIC 2018 February 17, 2018
|
|
- Victor Short
- 5 years ago
- Views:
Transcription
1 Post-Inflationary Higgs Relaxation and Leptogenesis Louis Yang Kavli IPMU PACIFIC 2018 February 17, 2018
2 Outline Motivation: the Higgs potential Quantum fluctuation during inflation Post-inflationary Higgs relaxation Leptogenesis via Higgs field relaxation Cosmic Infrared Background (CIB) excess Isocurvature perturbation Based on: [1] A. Kusenko, L. Pearce, LY, Phys. Rev. Lett. 114, (2015). [2] L. Pearce, LY, A. Kusenko, M. Peloso, Phys. Rev. D 92, (2015). [3] LY, L. Pearce, A. Kusenko, Phys. Rev. D 92, (2015). [4] H. Gertov, L. Pearce, F. Sannino, LY, Phys. Rev. D 93, (2016). [5] A. Kusenko, L. Pearce, LY, Phys. Rev. D 93, (2016). [6] M. Kawasaki, A. Kusenko, L. Pearce, LY, Phys. Rev. D 95, (2017). 2
3 Motivation The Higgs Potential 3
4 The Higgs Boson In 2012, ATLAS and CMS found the Higgs boson. V Φ = m 2 Φ + Φ + λ Φ + Φ 2, 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 I Quantum Fluctuation during Inflation 9
10 Quantum Fluctuation during Inflation During inflation, quantum fluctuations of scalar field get amplified and pulled to over the horizon size. 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 Stochastic Approach 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 = GGG, the Hubble rate Λ I 2 H I = ~10 11 GGG, and λ~0. 00, the Higgs VEV after 3M pp inflation is φ H I /λ 1/4 ~ GGG. For such a large VEV, the Higgs field can be sensitive to higher scale physics. 13
14 Post-Inflationary Higgs Field Relaxation 14
15 Post-inflationary Higgs Relaxation As the inflation end, the H drops. When H < m φ,eee, the Higgs field can relax classically φ t + 33 t φ t + V eff φ, T t = 0 φ V eee (φ, T) is the finite temperature effective potential. Higgs field oscillates with decreasing amplitude due to the Hubble friction 3Hφ t. Relaxation time (depending on T RR and Λ I ) 2.5 4/3 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. 9/ λφ 0 if the zero T dominates V λφ 4 /4 Typically during reheating or right after reheating. 15
16 Post-inflationary Higgs Relaxation M. Kawasaki, A. Kusenko, L. Pearce, LY, Phys. Rev. D 95, (2017). 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 (assuming MD) A solution: φ t + 2 t φ t + α T 2 T RR t t RR φ t = 0 3 φ t = φ 0 Γ J 4α T β 2 3 x α T β 2 3 x where β = T RR t RR, x = t/t RR, and J n (z) is the Bessel function of the first kind. 16
17 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! 17
18 Initial Conditions for the Higgs field Initial Condition 1 (IC-1): A metastable Planckian vacuum due to higher dimensional operators O~ M 2 φ6, M 4 φ8, φ11 M6 Higgs field trapped in a metastable vacuum during inflation Reheating destabilize the metastable vacuum via δδ~t 2 φ 2 and the Higgs VEV relaxes V(ϕ) H 4 Trapped Reheating Second Min. Thermal correction ϕ 18
19 Initial Conditions for the Higgs field Initial Condition 2 (IC-2): Inflaton VEV induced mass term to the Higgs via O = I n φ m /Λ n+m 4 Large I during early stage of inflation Large Higgs mass and suppressing quantum fluctuation In the last N llll e-fold of inflation, I decreases and Higgs becomes massless with φ 0 = H N llll 22 V(ϕ) Last Early N e-folds stage End of of inflation Quantum jumps Rolls down classically φ 2 φ~0 2 starts φ 2 to = grow H 2 I N/4π 2 H 4 H 4 ϕ 19
20 II Leptogenesis via the Relaxation of the Higgs Field 20
21 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 21
22 Effective Operator M. E. Shaposhnikov (1987), M. E. Shaposhnikov (1988) CP violation: 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: Also used by baryogenesis But suppressed by small Yukawa and small CC phase 22
23 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 23
24 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 s conditions doesn t have to be satisfied explicitly in this form. 24
25 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 Produce more lepton than antilepton in the present of L violating process. 25
26 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 LY, L. Pearce, A. Kusenko, Phys. Rev. D 92, (2015). 26
27 Evolution of Lepton Asymmetry Boltzman equation: n L + 33n L 2 π 2 T3 σ R n L 2 π 2 μ eeet 2 Final lepton asymmetry: Y = n L s 99σ R π 6 g S φ 0 Λ n 2 3z0 T RR eee 4α T t RR π 2 Λ I = GeV, Γ I = 10 8 GeV, T RR = GeV, φ 0 = GeV. For μ eff M n 2 case, M n = GeV. σ R T 3 RR t RR Could be one origin of the matter-antimatter asymmetry! 27
28 III Cosmic Infrared Background Radiation Excess 30
29 Cosmic Infrared Background (CIB) Radiation CIB: IR part of extragalactic background light from galaxies at all redshifts Difficult to determine absolute intensity (isotropic flux) due to foreground signal, galactic components, and zodiacal light. More focus on the anisotropies (spatial fluctuation) of CIB CIB (spatial) fluctuations observed by Spitzer space telescope 31
30 Excess in the CIB fluctuations Helgason et al., MNRAS 455, 282 (2015) Kashlinsky et al. ApJ 804, 99 (2015) Spitzer AKARI Excess found in near-ir (1 11 μμ) at θ = 3 33 arcmins scale. Not from known galaxy populations at z < 6 Most possible: First stars (population III stars, metal-free) at z 11 in 10 6 M minihalos But: Needs too large star formation efficiency and/or radiation efficiency due to insufficient stars forming at z =
31 CIB fluctuation from population III stars CIB fluctuation: δf CCC nwm 2 sr 1 (2 55m at 5 ) Matter density fluctuation at 5 arcmins scale: Δ Inferred isotropic flux: F CCC δf CCC Δ 5 = 1 nwm 2 sr 1 CIB flux from first stars (population III) F FF = c 44 ε ρ B c 2 1 f hhhh f z eee f hhhh : mass fraction of the universe inside collapsed halos f : the star formation efficiency ε : radiation efficiency To explain the CIB fluctuation by first stars forming: f hhhh ε 10 3 f F FF F CCC Difficult to reach with only adiabatic density perturbation from usual inflation. Solution: isocurvature perturbation in the small spatial scale 33
32 Large vs Small scale density perturbation Δ 5 10% ~10 6 M minihalos Add isocurvature perturbation from relaxation leptogenesis θ ~ 5 Large scale fluctuation in CIB due to the adiabatic perturbation from inflaton Increasing the density contrast δ B in small scale increase the number of collapse halos f hhhh 34
33 Isocurvature Perturbation from Relaxation Leptogenesis 35
34 Isocurvature Perturbation Fluctuation of φ in each patch of the universe during inflation Variation in baryon asymmetry δ(b B ) through leptogenesis (Y B φ 0 2 ) Spatial fluctuation of baryon asymmetry after patches reenter V(φ) φ Baryon asymmetry δy B Baryon density δρ B Produce isocurvature perturbation of baryon φφφ φ φφ No contribution to the initial curvature perturbation. 36
35 Higgs Fluctuation during Inflation In IC-2, the Higgs φ becomes massless in the last N llll e-fold of inflation due to the inflaton couplings. Quantum fluctuation δφ k H I is produced at the scale 22 smaller than the horizon scale l~h 1 at that time When Higgs becomes massless t = 0 Outside the horizon H I Inside the horizon No difference from Minkowski space After N llll e-fold of inflation t = N llll H H I eee N llll H I δφ k H I 22 Inflationary region p = k/a Physical momentum 37
36 Higgs Fluctuation during Inflation The horizon at N llll before the end of inflation has a scale k S at present k S 22e N llllh I T RR Λ I g S 1 3 g S T nnn T RR T nnn T RR Power spectrum of φ P φ k H I for k k S otherwise Baryonic isocurvature perturbation for k > k S δ B k δρ B = δy B = δ φ2 k ρ B Y k B φ 2 2 ln1 2 k k S N k llll θ k k S 38
37 Constraints on Isocurvature Perturbation CMB: MMc 1 k 0. 1 MMc 1 (Limited by Silk damping) Lyman-α: 0. 1 MMc 1 k 11 MMc 1 Allowed N of e-folds of inflation for the Higgs field: N llll < ll k 11 MMc ll Λ I GGG ll T RR GGG 39
38 Growth of density perturbation Baryon isocurvature perturbation only growth after decoupling But the induced potential allows dark matter to grows faster. δ M becomes nonlinear earlier δ B,0 = 0.025, k S = 65 Mpc 1, N last = 46.5 Matter power Spectrum Contribution from relaxation leptogenesis model only appear in the small scale Silk damping does not affect baryonic isocurvature perturbation. 40
39 Variance of the density contrast Solid lines: Isocurvature perturbations from k S = 65 Mpc 1 Dashed lines: with only adiabatic perturbation Dash-dot line: δ c = Halos with 10 6 M collapsed by z = 10. Mass fraction in collapsed halos Solid lines: 10 6 M halos Reach f halo = 0.16 by z = 10 for k S = 65 Mpc 1 Dashed lines: 10 8 M halos unchanged Can explain the CIB fluctuation excess! 10 8 M 10 6 M 41
40 Summary Our universe seems to be right at the meta-stable vacuum. A small quartic coupling of the Higgs potential at high energy scale gives a shallow potential. Higgs can obtain a 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. Isocurvature perturbation generated by the relaxation leptogenesis might explain the CIB fluctuation excess. Higgs relaxation is an interesting epoch in the early universe. Thanks for your listening! 42
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 30, 2016 4TH INTERNATIONAL WORKSHOP ON DARK MATTER,
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 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 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 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 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 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 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 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 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 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 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 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 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 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 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 informationWhat could we learn about high energy particle physics from cosmological observations at largest spatial scales?
What could we learn about high energy particle physics from cosmological observations at largest spatial scales? Dmitry Gorbunov 1,a 1 Institute for Nuclear Research of Russian Academy of Sciences, 117312
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 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 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 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 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 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 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 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 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 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 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 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 informationInflationary cosmology. Andrei Linde
Inflationary cosmology Andrei Linde Problems of the Big Bang theory: What was before the Big Bang? Why is our universe so homogeneous? Why is it isotropic? Why its parts started expanding simultaneously?
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 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 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 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 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 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 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 informationScale symmetry a link from quantum gravity to cosmology
Scale symmetry a link from quantum gravity to cosmology scale symmetry fluctuations induce running couplings violation of scale symmetry well known in QCD or standard model Fixed Points Quantum scale symmetry
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 informationStructures in the early Universe. Particle Astrophysics chapter 8 Lecture 4
Structures in the early Universe Particle Astrophysics chapter 8 Lecture 4 overview problems in Standard Model of Cosmology: horizon and flatness problems presence of structures Need for an exponential
More informationScalar fields and vacuum fluctuations II
Scalar fields and vacuum fluctuations II Julian Merten ITA July 12, 2007 Julian Merten (ITA) Scalar fields and vacuum fluctuations II July 12, 2007 1 / 22 Outline 1 What we did so far 2 Primordial curvature
More informationFormation of Primordial Black Holes in Double Inflation
Formation of Primordial Black Holes in Double Inflation Masahiro Kawasaki (ICRR and Kavli-IPMU, University of Tokyo) Based on MK Mukaida Yanagida, arxiv:1605.04974 MK Kusenko Tada Yanagida arxiv:1606.07631
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 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 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 informationCaldwell, MK, Wadley (open) (flat) CMB determination of the geometry (MK, Spergel, and Sugiyama, 1994) Where did large scale structure (e.g., galaxies, clusters, larger-scale explosions clustering)
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 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 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 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 informationGerman physicist stops Universe
Big bang or freeze? NATURE NEWS Cosmologist claims Universe may not be expanding Particles' changing masses could explain why distant galaxies appear to be rushing away. Jon Cartwright 16 July 2013 German
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 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 informationA873: Cosmology Course Notes. VII. Inflation
Readings VII. Inflation Alan Guth s Inflationary Universe paper (Phys Rev D, Vol. 23, p. 347, 1981) is a classic, well worth reading. The basics are well covered by Ryden, Chapter 11. For more physics
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 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 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 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 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 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 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 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 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 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 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 Massive Gravity
New perspectives on cosmology APCTP, 15 Feb., 017 Inflationary Massive Gravity Misao Sasaki Yukawa Institute for Theoretical Physics, Kyoto University C. Lin & MS, PLB 75, 84 (016) [arxiv:1504.01373 ]
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 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 informationThe cosmological constant puzzle
The cosmological constant puzzle Steven Bass Cosmological constant puzzle: Accelerating Universe: believed to be driven by energy of nothing (vacuum) Vacuum energy density (cosmological constant or dark
More informationHiggs field in cosmology
Higgs field in cosmology Christian Friedrich Steinwachs Albert-Ludwigs-Universität Freiburg 678th Wilhelm and Else Heraeus Seminar: Hundred Years of Gauge Theory, Bad Honnef, 02.08.2018 Cosmic history
More informationDilaton and IR-Driven Inflation
Dilaton and IR-Driven Inflation Chong-Sun Chu National Center for Theoretical Science NCTS and National Tsing-Hua University, Taiwan Third KIAS-NCTS Joint Workshop High 1 Feb 1, 2016 1506.02848 in collaboration
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 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 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 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 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 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 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 informationCosmological Signatures of a Mirror Twin Higgs
Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness
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 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 informationWeek 10 Cosmic Inflation: Before & After. Joel Primack
Astro/Phys 224 Spring 2014 Origin and Evolution of the Universe Week 10 Cosmic Inflation: Before & After Joel Primack University of California, Santa Cruz Physics 224 - Spring 2014 Tentative Term Project
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 informationTesting the string theory landscape in cosmology
別府 01..1 1 Testing the string theory landscape in cosmology 佐々木節 1. Cosmology Today Big Bang theory has been firmly established wavelength[mm] COBE/FIRAS CMB spectrum at T=.75K 00 sigma error-bars frequency[ghz]
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 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 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 informationTesting leptogenesis at the LHC
Santa Fe Summer Neutrino Workshop Implications of Neutrino Flavor Oscillations Santa Fe, New Mexico, July 6-10, 2009 Testing leptogenesis at the LHC ArXiv:0904.2174 ; with Z. Chacko, S. Granor and R. Mohapatra
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 informationUnifying inflation with the axion, dark matter, baryogenesis and the seesaw mechanism
Unifying inflation with the axion, dark matter, baryogenesis and the seesaw mechanism Carlos Tamarit, Durham IP3 arxiv:1608.05414 arxiv:1610.01639 In collaboration with... Guillermo Ballesteros SACLAY
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 informationDe Sitter Space Without Quantum Fluctuations
De Sitter Space Without Quantum Fluctuations arxiv:1405.0298 (with Kim Boddy and Sean Carroll) Jason Pollack Quantum Foundations of a Classical Universe IBM Watson Research Center August 12, 2014 8/12/2014
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 informationFrom Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology
From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology Yi-Fu Cai June 18, 2013 in Hefei CYF, Chang, Chen, Easson & Qiu, 1304.6938 Two Standard Models Cosmology CMB: Cobe (1989), WMAP (2001),
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 informationState of the Universe Address
State of the Universe Address Prof. Scott Watson ( Syracuse University ) This talk is available online at: https://gswatson.expressions.syr.edu This research was supported in part by: Theoretical Cosmology
More informationBig Bang Planck Era. This theory: cosmological model of the universe that is best supported by several aspects of scientific evidence and observation
Big Bang Planck Era Source: http://www.crystalinks.com/bigbang.html Source: http://www.odec.ca/index.htm This theory: cosmological model of the universe that is best supported by several aspects of scientific
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 information