Inflationary density perturbations
|
|
- Joella Curtis
- 5 years ago
- Views:
Transcription
1 Cosener s House 7 th June 003 Inflationary density perturbations David Wands Institute of Cosmology and Gravitation University of Portsmouth
2 outline! some motivation! Primordial Density Perturbation (and conserved quantities on large scales)! constraints on single-field models! predictions from multi-field models! conclusions
3 Cosmological inflation: Starobinsky (1980) Guth (1981) period of accelerated expansion in the very early universe requires negative pressure e.g. self-interacting scalar field V(φ) speculative and uncertain physics φ just the kind of peculiar cosmological behaviour we observe today
4 Motivation: inflation in very early universe testable through primordial perturbation spectra! radiation/matter density perturbations! + gravitational waves (we hope) gravitational instability new observational data offers precision tests of cosmological parameters and the Primordial Density Perturbation
5 Primordial Density Perturbation e.g., epoch of primordial nucleosynthesis cosmic fluid consists of photons, γ, neutrinos, ν, baryons, B, cold dark matter, CDM, (+quintessence?)! total density perturbation, or curvature perturbation R δρ δρ/ρ! relative density perturbations, or isocurvature pertbns S i =δ(n i /n γ )/(n i /n γ )! large-angle CMB: ( T/T) lss [ R - S m ] / 5
6 Conserved cosmological perturbations Lyth & Wands in preparation time t t 1 A B For every quantity, x, that obeys a local conservation equation dx dn space = y( x), e. g. & ρ = 3Hρ where dn = Hdt is the locally-defined expansion along comoving worldlines there is a conserved perturbation where perturbation δ x = x A -x B is a evaluated on hypersurfaces separated by uniform expansion N= lna m ζ δn = x m δ x y(x)
7 examples: (i) total energy conservation: dρ = dn H 1 & ρ = 3( ρ + for perfect fluid / adiabatic perturbations, P=P(ρ) δρ R ζ ρ = conserved 3( ρ + P) (ii) energy conservation for non-interacting perfect fluids: 1 δρi H ρ& i = 3( ρi + Pi ) where Pi = Pi ( ρi ) ζ i = 3( ρ + P ) (iii) conserved particle/quantum numbers (e.g., B, B-L, ) ni H 1 δ n& i = 3ni ζ i = 3n P) i i i
8 Primordial Density Perturbation (II) epoch of primordial nucleosynthesis perturbed cosmic fluid consists of photons, ζ γ, neutrinos, ζ ν, baryons, ζ B, cold dark matter, ζ CDM, (+quintessence, ζ Q ) total density perturbation, or curvature perturbation relative density perturbations, or isocurvature perturbtns R = i & ρi ζ i & ρ ( ) S = ζ ζ i 3 i γ
9 where do these perturbations come from?
10 perturbations in an FRW universe: wave equation δ & φ + 3Hδφ& δφ = Characteristic timescales for comoving wavemode k oscillation period/wavelength a / k Hubble damping time-scale H -1 small-scales k > ah under-damped oscillator large-scales k < ah over-damped oscillator ( frozen-in ) 0 vacuum comoving Hubble length H -1 / a frozen-in oscillates comoving wavelength, k -1 conformal time inflation accelerated expansion (or contraction) radiation or matter era decelerated expansion
11 Wilkinson Microwave Anisotropy Probe February 003 coherent oscillations in photon-baryon plasma from primordial density perturbations on super-horizon scales
12 Vacuum fluctuations V(φ) Hawking 8, Starobinsky 8, Guth & Pi 8 small-scale/underdamped zero-point fluctuations large-scale/overdamped perturbations in growing mode linear evolution Gaussian random field δφ 4π k 3 δφ k k = ah 3 (π ) π fluctuations of any light fields (m<3h/) `frozen-in on large scales = H δφ k φ e ik η k *** assumes Bunch-Davies vacuum on small scales *** all modes start sub-planck length for k/a > M Pl Niemeyer; Brandenberger & Martin (000) effect likely to be small for H << M Pl Starobinsky; Niemeyer; Easther et al ; Kaloper et al (00)
13 Inflaton -> matter perturbations R = for adiabatic perturbations on super-horizon scales R & = 0 during inflation scalar field fluctuation, δφ scalar curvature on uniform-field hypersurfaces Hδσ & σ during matter+radiation era density perturbation, δρ time scalar curvature on uniform-density hypersurfaces R = Hδρ & ρ ζ ζ = ζ = ζ = ζ = cdm ( ) necessarily adiabatic primordial perturbations γ B ν σ
14 Inflaton scenario: high energy / not-so-slow roll 1. large field ( ϕ < M Pl ) e.g. chaotic inflation see, e.g., Lyth & Riotto Kinney, Melchiorri & Riotto (001) 0 <η < ε not-so-high energy / very slow roll. small field e.g. new or natural inflation η < 0 3. hybrid inflation e.g., susy or sugra models 0 < ε <η slow-roll solution for potential-dominated, over-damped evolution gives useful approximation to growing mode for { ε, η } << 1 & 16π V H V 8π V H M P Vφ H ε M m P φφ η =
15 can be distinguished by observations slow time-dependence during inflation -> weak scale-dependence of spectra n = 1 6ε + η tensor/scalar ratio suppressed at low energies/slow-roll T R = 16ε
16 WMAP constraints (I) Microwave background only (WMAPext) Peiris et al (003) r < 1.8 Harrison-Zel dovich spectral index n R 1 6ε + η n 1, r 0
17 WMAP constraints (II) Microwave background + df + Ly-alpha Peiris et al (003) r < 1.8 spectral index n R 1 6ε + η
18 WMAP constraints (III) Microwave background + df + Ly-alpha Peiris et al (003) dn R / d ln k = n R =1.13± 0.08 r < 1.8
19 scale-dependent tilt? dn R d ln k ( 3ε η) ξ 8ε third slow-roll parameter ξ V V 4 M Pl, φ 64π V, φφφ involving four derivatives of the potential, not two the beginning of the end for slow-roll? inflaton effective mass is not constant dη ξ + εη dn slow-roll inflation could be just a passing phase!
20 digging deeper: additional fields may play an important role initial state ending inflation enhancing inflation new inflation hybrid inflation assisted inflation warm inflation brane-world inflation producing density perturbations may yield additional information non-gaussianity isocurvature (non-adiabatic) modes
21
22 Inflation -> primordial perturbations (II) scalar field fluctuations two fields (σ,χ) curvature of uniform-field slices R = * isocurvature S = * Hδσ & σ Hδχ & σ R S 1 = primordial 0 k<< ah density perturbations matter and radiation (m,γ) curvature of uniform-density slices R& = αhs, S& = βhs T T RS SS R S * * S = R = δn n inflation k = ah Hδρ & ρ δn model-dependent transfer functions m m Amendola, Gordon, Wands & Sasaki (00) Wands, Bartolo, Matarrese & Riotto (00) n γ γ
23 examples: field dynamics during inflation Polarski & Starobinsky; Sasaki & Stewart; Garcia-Bellido & Wands; Steinhardt & Mukhanov; Adams, Ross & Sarkar; Langlois (1996+) variable couplings during/after reheating Dvali, Gruzinov & Zaldariaga; Kofman (003) late-decaying scalar : the curvaton scenario Enqvist & Sloth; Lyth & Wands; Moroi & Takahashi (001+)
24 curvaton scenario: Lyth & Wands, Moroi & Takahashi, Enqvist & Sloth (00) assume negligible curvature perturbation during inflation R * = 0 light during inflation, hence acquires isocurvature spectrum late-decay, hence energy density non-negligible at decay large-scale density perturbation generated entirely by non-adiabatic modes after inflation R = T RS S * Ω T RS Ω χ, decay χ, decay S * δρ ρ χ χ ( δρ χ χ / ρ ) negligible gravitational waves 100%correlated residual isocurvature modes detectable non-gaussianity if Ω χ,decay <<1
25 primordial isocurvature perturbations from curvaton? Moroi & Takahashi; Lyth, Ungarelli & Wands 03 cdm, neutrinos, baryon asymmetry all created after curvaton decays ζ ( ζ γ = ζν = ζ = ζ ) Ωχ, decay ζ χ = cdm B S = 0 i cdm/baryon asymmetry created at high energies before curvaton decay ζ = ζ γ Ωχ, decayζ χ, ζ m = 0 S m = 3ζ 100% correlation between curvature and residual isocurvature mode naturally of same magnitude neutrino asymmetry (ξ<0.1) created at high energies before curvaton decay S υ 135 ξ = 7 π ζ
26 Observational constraints Gordon & Lewis, astro-ph/0148v using CMB + df + HST + BBN isocurvature / curvature ratio B = S B / ζ pre-wmap 95% c.f. Peiris et al f iso = S cdm /ζ 0.1 B and marginalised over correlation angle -> f iso < 0.33 post-wmap
27 isocurvature perturbations from curvaton (II) cdm/baryon asymmetry created by curvaton decay ζ = ζ = ζ γ Ωχ,decayζ χ, ζ m χ Lyth, Ungarelli & Wands 0 Gupta, Malik & Wands in preparation S m = ( ) χ, decay Ω ζ = 3 ζ 3 1 χ, decay χ 1 Ω Ω χ, decay curvature and isocuravture perturbations naturally of same magnitude relative magnitude related to non-gaussianity
28 non-gaussianity simplest kind of non-gaussianity: Komatsu & Spergel (001) Wang & Kamiokowski (000) recall that for curvaton corresponds to δρ ρ δ ρ Ω χ,decay δρ ρ δρ ρ significant constraints on f NL from WMAP f NL < 134 χ χ Ω δ1ρ + ρ χ,decay f NL δ1ρ ρ δχ δχ + χ χ 1ρ δχ 1 Ωχ,decay, f NL χ Ωχ,decay Lyth, Ungarelli & Wands 0 hence Ω χ,decay > 0.01 and 10-5 < δχ/χ < 10-3
29 observable parameters inflaton regime curvature & tensor perturbations n s & tensor/scalar ratio = n t curvaton regime curvature + isocurvature perturbations n s = n iso & isocurvature/curvature ratio intermediate regime n s, n iso, n corr, n t, tensor/scalar, iso/curvature, correlation Wands, Bartolo, Matarrese & Riotto, 0
30 Conclusions: 1. Observations of tilt of density perturbations (n 1) and gravitational waves (ε>0) can distinguish between slow-roll models. Isocurvature perturbations and/or non- Gaussianity may provide valuable info 3. Non-adiabatic perturbations in multi-field models are an additional source of curvature perturbations on large scales 4. Consistency relations remain an important test in multi-field models - can falsify slow-roll inflation 5. More precise data allows/requires us to study more detailed models!
Inflation 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 informationThe multi-field facets of inflation. David Langlois (APC, Paris)
The multi-field facets of inflation David Langlois (APC, Paris) Introduction After 25 years of existence, inflation has been so far very successful to account for observational data. The nature of the
More informationCurvaton model for origin of structure! after Planck
Implications of Planck for Fundamental Physics Manchester, 8 th May 013 Curvaton model for origin of structure! after Planck David Wands Institute of Cosmology and Gravitation, University of Portsmouth
More informationMisao Sasaki YITP, Kyoto University. 29 June, 2009 ICG, Portsmouth
Misao Sasaki YITP, Kyoto University 9 June, 009 ICG, Portsmouth contents 1. Inflation and curvature perturbations δn formalism. Origin of non-gaussianity subhorizon or superhorizon scales 3. Non-Gaussianity
More informationCompleting the curvaton model Rose Lerner (Helsinki University) with K. Enqvist and O. Taanila [arxiv: ]
Completing the curvaton model Rose Lerner (Helsinki University) with K. Enqvist and O. Taanila [arxiv:1105.0498] Origin of? super-horizon Origin of (almost) scale-invariant? perturbations Outline What
More informationLarge Primordial Non- Gaussianity from early Universe. Kazuya Koyama University of Portsmouth
Large Primordial Non- Gaussianity from early Universe Kazuya Koyama University of Portsmouth Primordial curvature perturbations Proved by CMB anisotropies nearly scale invariant n s = 0.960 ± 0.013 nearly
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 informationFrom inflation to the CMB to today s universe. I - How it all begins
From inflation to the CMB to today s universe I - How it all begins Raul Abramo Physics Institute - University of São Paulo abramo@fma.if.usp.br redshift Very brief cosmic history 10 9 200 s BBN 1 MeV
More informationPrimordial perturbations from inflation. David Langlois (APC, Paris)
Primordial perturbations from inflation David Langlois (APC, Paris) Cosmological evolution Homogeneous and isotropic Universe Einstein s equations Friedmann equations The Universe in the Past The energy
More informationSingle versus multi field inflation post Planck Christian Byrnes University of Sussex, Brighton, UK. Kosmologietag, Bielefeld.
Single versus multi field inflation post Planck Christian Byrnes University of Sussex, Brighton, UK Kosmologietag, Bielefeld. 7th May 15+5 min What have we learnt from the precision era? Planck completes
More informationCosmology and the origin of structure
1 Cosmology and the origin of structure ocy I: The universe observed ocy II: Perturbations ocy III: Inflation Primordial perturbations CB: a snapshot of the universe 38, AB correlations on scales 38, light
More informationprimordial avec les perturbations cosmologiques *
Tests de l Univers primordial avec les perturbations cosmologiques * Filippo Vernizzi Batz-sur-Mer, 16 octobre, 2008 * Soustitré en anglais What is the initial condition? Standard single field inflation
More informationInflation : sources of primordial perturbations
DESY Workshop, Particle Cosmology 30 th September 004 Iflatio : sources of primordial perturbatios David Wads Istitute of Cosmology ad Gravitatio Uiversity of Portsmouth Cosmological iflatio: Starobisky
More informationPrimordial non Gaussianity from modulated trapping. David Langlois (APC)
Primordial non Gaussianity from modulated trapping David Langlois (APC) Outline 1. Par&cle produc&on during infla&on 2. Consequences for the power spectrum 3. Modulaton and primordial perturba&ons 4. Non
More informationThe Theory of Inflationary Perturbations
The Theory of Inflationary Perturbations Jérôme Martin Institut d Astrophysique de Paris (IAP) Indian Institute of Technology, Chennai 03/02/2012 1 Introduction Outline A brief description of inflation
More informationCurrent status of inflationary cosmology. Gunma National college of Technology,Japan
Current status of inflationary cosmology Shinji Tsujikawa Gunma National college of Technology,Japan Bright side of the world Recent observations have determined basic cosmological parameters in high precisions.
More informationArchaeology of Our Universe YIFU CAI ( 蔡一夫 )
Archaeology of Our Universe YIFU CAI ( 蔡一夫 ) 2013-11-05 Thermal History Primordial era 13.8 billion years by WMAP/NASA Large Scale Structure (LSS) by 2MASS Cosmic Microwave Background (CMB) by ESA/Planck
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 informationIsocurvature cosmological perturbations and the CMB
C. R. Physique 4 (2003) 953 959 The Cosmic Microwave Background/Le rayonnement fossile à 3K Isocurvature cosmological perturbations and the CMB David Langlois Institut d astrophysique de Paris, 98bis,
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 informationNon-linear perturbations from cosmological inflation
JGRG0, YITP, Kyoto 5 th September 00 Non-linear perturbations from cosmological inflation David Wands Institute of Cosmology and Gravitation University of Portsmouth summary: non-linear perturbations offer
More informationOrigins and observations of primordial non-gaussianity. Kazuya Koyama
Origins and observations of primordial non-gaussianity Kazuya Koyama University of Portsmouth Primordial curvature perturbations Komatsu et.al. 008 Proved by CMB anisotropies nearly scale invariant ns
More informationInflation and the Primordial Perturbation Spectrum
PORTILLO 1 Inflation and the Primordial Perturbation Spectrum Stephen K N PORTILLO Introduction The theory of cosmic inflation is the leading hypothesis for the origin of structure in the universe. It
More informationCosmology: An Introduction. Eung Jin Chun
Cosmology: An Introduction Eung Jin Chun Cosmology Hot Big Bang + Inflation. Theory of the evolution of the Universe described by General relativity (spacetime) Thermodynamics, Particle/nuclear physics
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 informationHemispherical CMB power asymmetry: observation vs. models
Helsinki May 2014 Hemispherical CMB power asymmetry: observation vs. models EnqFest May 2014 Helsinki John McDonald, Dept. of Physics, University of Lancaster Outline 1. Observed Hemispherical Asymmetry
More informationInflationary Cosmology and Alternatives
Inflationary Cosmology and Alternatives V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Department of paricle Physics abd Cosmology Physics Faculty Moscow State
More informationSchool Observational Cosmology Angra Terceira Açores 3 rd June Juan García-Bellido Física Teórica UAM Madrid, Spain
School Observational Cosmology Angra Terceira Açores 3 rd June 2014 Juan García-Bellido Física Teórica UAM Madrid, Spain Outline Lecture 1 Shortcomings of the Hot Big Bang The Inflationary Paradigm Homogeneous
More informationConservation and evolution of the curvature perturbation
Conservation and evolution of the curvature perturbation University of Wisconsin-Madison 1150 University Avenue, Madison WI 53706-1390 USA Cosmo 08 University of Wisconsin-Madison, USA 28th August, 2008
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 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 informationLooking Beyond the Cosmological Horizon
Looking Beyond the Cosmological Horizon 175 µk 175 µk Observable Universe Adrienne Erickcek in collaboration with Sean Carroll and Marc Kamionkowski A Hemispherical Power Asymmetry from Inflation Phys.
More informationCosmological Imprints of Dark Matter Produced During Inflation
Cosmological Imprints of Dark Matter Produced During Inflation Daniel J. H. Chung 10/15/2014 Isocurvature Sample High-energy theory motivated: Multi-field inflation: Axenides, Brandenberger, Turner 83;
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 informationEl Universo en Expansion. Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004
El Universo en Expansion Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004 5 billion years (you are here) Space is Homogeneous and Isotropic General Relativity An Expanding Universe
More informationTowards Multi-field Inflation with a Random Potential
Towards Multi-field Inflation with a Random Potential Jiajun Xu LEPP, Cornell Univeristy Based on H. Tye, JX, Y. Zhang, arxiv:0812.1944 and work in progress 1 Outline Motivation from string theory A scenario
More informationarxiv: v3 [astro-ph.co] 23 Apr 2014
ICRR-Report-674-2013-23 IPMU14-0066 arxiv:1403.5823v3 [astro-ph.co] 23 Apr 2014 Compensation for large tensor modes with iso-curvature perturbations in CMB anisotropies Masahiro Kawasaki a,b and Shuichiro
More informationObserving Primordial Fluctuations From the Early Universe: Gaussian, or non- Gaussian?
Observing Primordial Fluctuations From the Early Universe: Gaussian, or non- Gaussian? Eiichiro Komatsu The University of Texas at Austin Colloquium at the University of Oklahoma, February 21, 2008 1 Messages
More informationarxiv:astro-ph/ v2 22 Aug 2001
RESCEU-17/01 TU-628 astro-ph/0108081 August, 2001 arxiv:astro-ph/0108081v2 22 Aug 2001 Isocurvature Fluctuations in Tracker Quintessence Models Masahiro Kawasaki (a), Takeo Moroi (b) and Tomo Takahashi
More informationPhysics 463, Spring 07. Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum
Physics 463, Spring 07 Lecture 3 Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum last time: how fluctuations are generated and how the smooth Universe grows
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 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 informationASPECTS OF D-BRANE INFLATION IN STRING COSMOLOGY
Summer Institute 2011 @ Fujiyoshida August 5, 2011 ASPECTS OF D-BRANE INFLATION IN STRING COSMOLOGY Takeshi Kobayashi (RESCEU, Tokyo U.) TODAY S PLAN Cosmic Inflation and String Theory D-Brane Inflation
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 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 informationWeek 6: Inflation and the Cosmic Microwave Background
Week 6: Inflation and the Cosmic Microwave Background January 9, 2012 1 Motivation The standard hot big-bang model with an (flat) FRW spacetime accounts correctly for the observed expansion, the CMB, BBN,
More informationNew Ekpyrotic Cosmology and Non-Gaussianity
New Ekpyrotic Cosmology and Non-Gaussianity Justin Khoury (Perimeter) with Evgeny Buchbinder (PI) Burt Ovrut (UPenn) hep-th/0702154, hep-th/0706.3903, hep-th/0710.5172 Related work: Lehners, McFadden,
More informationThe Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004
The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The history of modern cosmology 1917 Static via cosmological constant? (Einstein) 1917 Expansion (Slipher) 1952 Big Bang criticism (Hoyle)
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 informationarxiv:hep-ph/ v1 28 Apr 2004
TU-717 hep-ph/0404253 April, 2004 arxiv:hep-ph/0404253v1 28 Apr 2004 Curvaton Scenario with Affleck-Dine Baryogenesis Maki Ikegami and Takeo Moroi Department of Physics, Tohoku University, Sendai 980-8578,
More informationInflation in a general reionization scenario
Cosmology on the beach, Puerto Vallarta,, Mexico 13/01/2011 Inflation in a general reionization scenario Stefania Pandolfi, University of Rome La Sapienza Harrison-Zel dovich primordial spectrum is consistent
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 informationParticle Astrophysics, Inflation, and Beyond
Particle Astrophysics, Inflation, and Beyond - A Historical Perspective - KIAS, December, 017 Yukawa Institute for Theoretical Physics, Kyoto University Misao Sasaki 1 Progress in Particle Cosmology (1)
More informationNon-Gaussianity from Curvatons Revisited
RESCEU/DENET Summer School @ Kumamoto July 28, 2011 Non-Gaussianity from Curvatons Revisited Takeshi Kobayashi (RESCEU, Tokyo U.) based on: arxiv:1107.6011 with Masahiro Kawasaki, Fuminobu Takahashi The
More informationLecture 09. The Cosmic Microwave Background. Part II Features of the Angular Power Spectrum
The Cosmic Microwave Background Part II Features of the Angular Power Spectrum Angular Power Spectrum Recall the angular power spectrum Peak at l=200 corresponds to 1o structure Exactly the horizon distance
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 information4 Evolution of density perturbations
Spring term 2014: Dark Matter lecture 3/9 Torsten Bringmann (torsten.bringmann@fys.uio.no) reading: Weinberg, chapters 5-8 4 Evolution of density perturbations 4.1 Statistical description The cosmological
More informationisocurvature modes Since there are two degrees of freedom in
isocurvature modes Since there are two degrees of freedom in the matter-radiation perturbation, there must be a second independent perturbation mode to complement the adiabatic solution. This clearly must
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 informationWarm intermediate inflationary universe models with a generalized dissipative coefficient / 34
Warm intermediate inflationary universe models with a generalized dissipative coefficient Departamento de Física Universidad de Chile In collaboration with: Ramón Herrera and Marco Olivares CosmoSur III
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 informationPPP11 Tamkang University 13,14 May, Misao Sasaki. Yukawa Institute for Theoretical Physics Kyoto University
PPP11 Tamkang University 13,14 May, 015 Misao Sasaki Yukawa Institute for Theoretical Physics Kyoto University General Relativity 1 8 G G R g R T ; T 0 4 c Einstein (1915) GR applied to homogeneous & isotropic
More informationKey: cosmological perturbations. With the LHC, we hope to be able to go up to temperatures T 100 GeV, age t second
Lecture 3 With Big Bang nucleosynthesis theory and observations we are confident of the theory of the early Universe at temperatures up to T 1 MeV, age t 1 second With the LHC, we hope to be able to go
More informationMASAHIDE YAMAGUCHI. Quantum generation of density perturbations in the early Universe. (Tokyo Institute of Technology)
Quantum generation of density perturbations in the early Universe MASAHIDE YAMAGUCHI (Tokyo Institute of Technology) 03/07/16@Symposium: New Generation Quantum Theory -Particle Physics, Cosmology, and
More informationPrimordial Black Holes as (part of the) dark matter
Primordial Black Holes as (part of the) dark matter Anne Green University of Nottingham Lecture 1: Motivation Formation: collapse of large (inflationary) density perturbations other mechanisms Mass function
More informationConnecting Quarks to the Cosmos
Connecting Quarks to the Cosmos Institute for Nuclear Theory 29 June to 10 July 2009 Inflationary Cosmology II Michael S. Turner Kavli Institute for Cosmological Physics The University of Chicago Michael
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 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 informationCOSMIC MICROWAVE BACKGROUND ANISOTROPIES
COSMIC MICROWAVE BACKGROUND ANISOTROPIES Anthony Challinor Institute of Astronomy & Department of Applied Mathematics and Theoretical Physics University of Cambridge, U.K. a.d.challinor@ast.cam.ac.uk 26
More informationGravitational waves from inflation
RIVISTA DEL NUOVO CIMENTO Vol. 39, N. 9 2016 DOI 10.1393/ncr/i2016-10127-1 Gravitational waves from inflation M. C. Guzzetti( 1 )( 2 )( ),N.Bartolo( 1 )( 2 )( 3 ),M.Liguori( 1 )( 2 )( 3 ) and S. Matarrese(
More informationNew Insights in Hybrid Inflation
Dr. Sébastien Clesse TU Munich, T70 group: Theoretical Physics of the Early Universe Excellence Cluster Universe Based on S.C., B. Garbrecht, Y. Zhu, Non-gaussianities and curvature perturbations in hybrid
More informationCurvature perturbations and non-gaussianity from waterfall phase transition. Hassan Firouzjahi. In collaborations with
Curvature perturbations and non-gaussianity from waterfall phase transition Hassan Firouzjahi IPM, Tehran In collaborations with Ali Akbar Abolhasani, Misao Sasaki Mohammad Hossein Namjoo, Shahram Khosravi
More informationThe self-interacting (subdominant) curvaton
Corfu.9.010 The self-interacting (subdominant) curvaton Kari Enqvist Helsinki University and Helsinki Institute of Physics in collaboration with C. Byrnes (Bielefeld), S. Nurmi (Heidelberg), A. Mazumdar
More informationObservational signatures of holographic models of inflation
Observational signatures of holographic models of inflation Paul McFadden Universiteit van Amsterdam First String Meeting 5/11/10 This talk I. Cosmological observables & non-gaussianity II. Holographic
More informationρ r + 4Hρ r = Γ φ 2.
Physics Letters B 526 (2002 1 8 wwwelseviercom/locate/npe Density perturbations in warm inflation and COBE normalization HP de Oliveira ab a NASA Fermilab Astrophysics Center Fermi National Accelerator
More informationGalaxies 626. Lecture 3: From the CMBR to the first star
Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic
More informationInflation and the origin of structure David Wands Institute of Cosmology and Gravitation University of Portsmouth
Cody Astronomical Society 7 th December 2011 Inflation and the origin of structure David Wands Institute of Cosmology and Gravitation University of Portsmouth outline of my talk: large-structure in the
More informationCosmology with CMB & LSS:
Cosmology with CMB & LSS: the Early universe VSP08 lecture 4 (May 12-16, 2008) Tarun Souradeep I.U.C.A.A, Pune, India Ω +Ω +Ω +Ω + Ω +... = 1 0 0 0 0... 1 m DE K r r The Cosmic Triangle (Ostriker & Steinhardt)
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 informationThe Effects of Inhomogeneities on the Universe Today. Antonio Riotto INFN, Padova
The Effects of Inhomogeneities on the Universe Today Antonio Riotto INFN, Padova Frascati, November the 19th 2004 Plan of the talk Short introduction to Inflation Short introduction to cosmological perturbations
More informationMisao Sasaki. KIAS-YITP joint workshop 22 September, 2017
Misao Sasaki KIAS-YITP joint workshop September, 017 Introduction Inflation: the origin of Big Bang Brout, Englert & Gunzig 77, Starobinsky 79, Guth 81, Sato 81, Linde 8, Inflation is a quasi-exponential
More informationThe scalar bispectrum during inflation and preheating in single field inflationary models
The scalar bispectrum during inflation and preheating in single field inflationary models L. Sriramkumar Department of Physics, Indian Institute of Technology Madras, Chennai Raman Research Institute,
More informationWhat have we learnt about the early universe?
What have we learnt about the early universe? V(φ) φ Hiranya Peiris STFC Advanced Fellow University of Cambridge Roadmap Lecture 1: The physics of the cosmic microwave background. Lecture 2: What have
More informationThe (p, q) inflation model
. Article. SCIENCE CHINA Physics Mechanics & Astronomy November 205 Vol. 58 No. : 040 doi: 07/s4-05-572- The (p q) inflation model HUANG QingGuo * State Key Laboratory of Theoretical Physics Institute
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 informationAspects of Inflationary Theory. Andrei Linde
Aspects of Inflationary Theory Andrei Linde New Inflation 1981-1982 V Chaotic Inflation 1983 Eternal Inflation Hybrid Inflation 1991, 1994 Predictions of Inflation: 1) The universe should be homogeneous,
More informationWhat was the Universe before the hot Big Bang?
What was the Universe before the hot Big Bang? V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences Department of Particle Physics and Cosmology Physics Faculty Moscow State University
More informationWMAP 9-Year Results and Cosmological Implications: The Final Results
WMAP 9-Year Results and Cosmological Implications: The Final Results Eiichiro Komatsu (Max-Planck-Institut für Astrophysik) 17th Paris Cosmology Colloquium 2013 Observatoire de Paris, July 24, 2013 1 used
More informationEffects of the field-space metric on Spiral Inflation
Effects of the field-space metric on Spiral Inflation Josh Erlich College of William & Mary digitaldante.columbia.edu Miami 2015 December 20, 2015 The Cosmic Microwave Background Planck collaboration Composition
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 informationLecture 3. The inflation-building toolkit
Lecture 3 The inflation-building toolkit Types of inflationary research Fundamental physics modelling of inflation. Building inflation models within the context of M-theory/braneworld/ supergravity/etc
More informationBouncing Cosmologies with Dark Matter and Dark Energy
Article Bouncing Cosmologies with Dark Matter and Dark Energy Yi-Fu Cai 1, *, Antonino Marcianò 2, Dong-Gang Wang 1,3,4 and Edward Wilson-Ewing 5 1 CAS Key Laboratory for Research in Galaxies and Cosmology,
More informationSymmetries! of the! primordial perturbations!
Paolo Creminelli, ICTP Trieste! Symmetries! of the! primordial perturbations! PC, 1108.0874 (PRD)! with J. Noreña and M. Simonović, 1203.4595! ( with G. D'Amico, M. Musso and J. Noreña, 1106.1462 (JCAP)!
More informationInflation from High Energy Physics and non-gaussianities. Hassan Firouzjahi. IPM, Tehran. Celebrating DBI in the Sky.
Inflation from High Energy Physics and non-gaussianities Hassan Firouzjahi IPM, Tehran Celebrating DBI in the Sky 31 Farvardin 1391 Outline Motivation for Inflation from High Energy Physics Review of String
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 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 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 informationRealistic Inflation Models and Primordial Gravity Waves
Journal of Physics: Conference Series Realistic Inflation Models and Primordial Gravity Waves To cite this article: Qaisar Shafi 2010 J. Phys.: Conf. Ser. 259 012008 Related content - Low-scale supersymmetry
More informationCosmological perturbations in mimetic gravity models
Università degli Studi di Padova DIPARTIMENTO DI FISICA E ASTRONOMIA GALILEO GALILEI Corso di Laurea in Fisica Tesi di laurea magistrale Cosmological perturbations in mimetic gravity models Candidato:
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 information