Cosmological Constraints on high energy neutrino injection. KEKPH07 March 1-3, 2007
|
|
- Archibald Lucas
- 5 years ago
- Views:
Transcription
1 Cosmological Constraints on high energy neutrino injection KEKPH07 March 1-3, 2007 Toru Kanzaki, Masahiro Kawasaki, Kazunori Kohri and Takeo Moroi Institute for Cosmic Ray Research
2 Introduction physics beyond the Standard model To solve { hierarchy problem dark matter. Supersymmetry (SUSY) is a prominent candidate. the existence of exotic long-lived particle X, e.g. gravitino ( In the framework of string theories, moduli ) We derive general and model-independent constraints on the relic abundance of X.
3 The decay of X have significant effects on cosmology, especially, the Big-Bang Nucleosynthesis (BBN) the Cosmic Microwave Background (CMB) diffuse photon flux diffuse neutrino flux decay product ( sec) ( sec) (10 12 sec ) What observation gives the most stringent constraints depends on the lifetime and decay products of X. X Y + γ an invisible particle X Y + ν { X Y + ν + Z(Z ) X Y + l + W (W ) main decay mode 3,4-body decay mode ( Branching ratio B X ) 3 free parameters: m X, τ X, B X B X Γ(X 3, 4body)/Γ(X all)
4 BBN constraints : ( Reno and Seckel 1988 ) ( Dimopoulos et.al ) ( Kawasaki and Moroi 1995 ) ( Kawasaki, Kohri and Moroi 2005 ) If the decay of X occur during or after BBN, the standard particles emitted in the decay can affect the abundance of primordial light elements. Resultant abundances of light elements may significantly conflict with observations. As a result, the relic abundance of X is severely constrained. ν + ν BG 2-body decay : X Y + ν { l+ + l π + + π electromagnetic shower p-n conversion 3,4-body decay : X Y + ν + Z(Z ), Y + l + W (W ) l, W, Z electromagnetic shower W, Z hadronic shower
5 B X = 10 3 m X = 300GeV lifetime Here we define yield value : Y X [ nx s 4 p-n conversion : He overproduction ] t τ X lifetime short 6 hadronic shower : D and Li overproduction 3 electromagnetic shower : He overproduction long
6 CMB constraints : y and µ distortions ( Silk and Stebbins 1983 ) ( Kawasaki and Sato 1986 ) ( Hu and Silk 1993 ) COBE observations show that the CMB spectrum is almost perfect blackbody. Therefore, any photon energy injection that cause distortions in the spectum of CMB are severely constrained. { µ ρ γ ρ γ µ distortion : (10 5 z 10 7 ) y distortion : y body decay ρ γ ρ γ (10 3 z 10 5 ) ν + ν BG l + + l exotic photon energy 3,4-body decay X Y + ν + Z(Z ), Y + l + W (W ) µ y ( COBE 1996, Smoot and Scott 1997 ) Some of the energy of these particles convert to photon energy.
7 B X = 10 6 m X = 10 2 GeV B X = 10 3 m X = 10 2 GeV lifetime lifetime When lifetime is short, the constraints are determined by 2-body decay. The constraints become severe with larger m X When lifetime is long, the constraints are determined by 3,4-body decay. The constraints become severe with smaller m X E X γ /E X = (m X = 100GeV) E X γ /E X = (m X = 10 5 GeV)
8 diffuse neutrino constraints : ( Ellis et. al ) ( Gondolo, Gelmini and Sarkar 1993 ) ( Beacom, Bell and Mack 2006 ) 2-body decay : X Y + ν (E ν = m X /2) When neutrino injection takes place at late time, the emitted neutrinos may produce an observable peak in the diffuse neutrino ν µ + ν µ spectrum. The atmospheric neutrino { Super-Kamiokande AMANDA (ν µ + ν µ ) has been observed by ( GeV) ( GeV) ( Ashie et. al ) ( Gonzalez-Garcia et. al ) ( Geenen et. al ) To obtain the constraints on the neutrino flux, we require that the signal from injected neutrino should not exceed the atmospheric neutrino.
9 No appreciable signal of ν e was detected at SK. through ( ν e + p n + e + ) This experiment set the upper bound of above a threshold energy. ν e background flux The upper bound of the diffuse signal ν e is given by Super-Kamiokande Φ ν < 1.2cm 2 s 1 for E ν > 19.3MeV ( Malek et. al )
10 SK m X = 10 3 GeV m X = 10 5 GeV τ X = sec AMANDA m X = 10 2 GeV present neutrino energy lifetime When lifetime is short, the constraints are determined by diffuse ν e. The constraints are in proportion to m X When lifetime is long, the constraints are determined by atmospheric neutrino. The constraints are roughly in inverse proportion to m X
11 diffuse photon constraints : There are two points different from atmospheric neutrino case : Injected photon spectrum is not monoenergetic. { photons from 3,4-body decay of X X γ photons produced by inverse Compton process and e + γ BG e + γ High energy photons scatter through various processes. { γ + γ CMB γ + γ, e + + e γ + γ IBL e + + e The diffuse photon flux has been observed by { COMPTEL EGRET (0.8 30MeV) X e (0 < z < 5) (30MeV 100GeV) ( Zdziarski and Svensson 1989 ) ( Kribs and Rothstein 1997 ) ( Salamon and Stecker 1998 ) ( Primack et. al ) ( Stecker, Malkan and Scully 2006 ) ( Kappadath et. al ) ( Sreekumarand et. al )
12 τ X = sec COMPTEL m X = 10 3 GeV m X = 10 5 GeV EGRET m X = 10 2 GeV present photon energy lifetime The constraints are almost independent of m X at early time. High energy photons are effectively absorbed by IBL photons.
13 Results : B X = 10 3 m X = 300GeV lifetime m X B X BBN CMB early time late time diffuse neutrino diffuse photon severe severe loose severe loose severe irrelevant severe irrelevant severe
14 Conclusions : We have considered the long-lived particle X which mainly decay into neutrino and investigated the effect of decay of X on cosmology. We derive general and model-independent constraints on the abundance of X from the BBN, CMB, diffuse neutrino and diffuse photon flux. We show that the BBN and diffuse neutrino flux provide stringent constraints on the abundance of X with larger mass.
15
16 Hadronic energy injection At early epoch (t < 10 2 sec) The emitted hadrons do not directly destroy the light elements due to the quick energy loss through EM interaction. The mesons with relatively long lifetimes such as can cause the p n conversion. π ± and K 0,± At later epoch (t > 10 2 sec) The high energy p and n interact with background hadrons before they lose energy, and produce secondary hadrons. Such hadronic interactions occur successively and evolve into hadronic shower ( hadro-dissociation )
17 p n conversion The Hadron-Nucleon interaction rate should be greater than the decay rate. Hadron-Nucleon interaction rate : Γ N N ( sec) 1 ( σv 40mb pion π + + n p + π 0, p + γ { π + p n + π 0, n + γ ) ( T ) 3 1MeV kaon { K + n Σ + π 0, K L + N N + Lifetime : τ π ± = sec τ K ± = sec = sec τ KL
18 Freeze-out of weak interaction (T 0.84MeV) n + ν p + e, n/p 1/6 n + e + p + ν The formation of the light elements n/p 1/7 n/p 1/7 + neutron decay + p n conversion (T 0.08MeV) ( This determines completely. ) Y p More 4 He n/p ratio increases
19 hadro-dissociation High energy p and n scatter off the background baryons before stopping. background p BG n(p) + p BG n(p) + p n(p) + p BG n(p) + p + π, background α BG n(p) + α BG n(p) + α n(p) + α BG D + T ( 3 He) n(p) + α BG n + n(p) + 3 He n(p) + α BG p + n(p) + T, D, T and 3 He are produced from the 4 He dissociation.
20 non-thermal production of 6 Li is not thought to be of primordial origin due to the cross section D(α, γ) 6 Li being small. 6 Li ( Nollett, Lemoine, Schramm 1997 ) non-thermal production of T and n(p) + α BG D + T ( 3 He) n(p) + α BG n + n(p) + 3 He n(p) + α BG p + n(p) + T, 3 He non-thermal production of 6 Li T + 4 He 6 Li + n [4.03MeV] 3 He + 4 He 6 Li + p [4.8MeV]
21 Electromagnetic energy injection electromagnetic cascade processes Photon-photon pair creation γ + γ BG e + + e (ɛ γ m e 2 /22T ) Photon-photon scattering γ + γ BG γ + γ (ɛ γ m e 2 /80T ) Inverse Compton e + γ BG e + γ Compton scattering γ + e BG γ + e
22 High-energy photon is quickly thermalized by photon-photon process. ɛ γ 2.2MeV ɛ γ 20MeV (T < 10keV or t > 10 4 sec) (T < 1keV or t > 10 6 sec) The destruction of light elements takes place only if binding energy is under this threshold energy. t > 10 4 sec : D overdestruction D + γ n + p [2.22MeV] T + γ D + n [6.2MeV] 3 He + γ D + p [5.5MeV] 4 He + γ T + p [19.8MeV] t > 10 6 sec : D overproduction 4 He + γ 3 He + n [20.5MeV] 4 He + γ D + n + p [26.1MeV]
23 non-thermal production of 6 Li is not thought to be of primordial origin due to the cross section D(α, γ) 6 Li being small. 6 Li ( Nollett, Lemoine, Schramm 1997 ) non-thermal production of T and 3 He 4 He + γ T + p [19.8MeV] 4 He + γ 3 He + n [20.5MeV] non-thermal production of 6 Li T + 4 He 6 Li + n [4.03MeV] 3 He + 4 He 6 Li + p [4.8MeV]
24 m X = 10 5 GeV τ X = 10 9 sec m X = 10 2 GeV time r = E lep /(n X /τ X )/(m X /2) r is the dimensionless parameter which represents the ratio of energy transferring to photon energy per time. High energy neutrino has larger cross section for lepton pair creations. High energy neutrino is easy to exceed the threshold energy for lepton pair creations.
25 Constraints on relativistic energy A late injection of relativistic energy could be spotted in the CMB or in large scale structure (LSS) regardless of the emitted species. For decays before recombination, the effective number of neutrino species : N eff ν 4.6 (WMAP 3rd-year and SDSS LRGs) ( Ichikawa, Kawasaki and Takahashi 2006 ) B X = 10 3 B X = 10 6 m X = 10 3 GeV Constraints from N eff ν
26 m X = 10 2 GeV m X = 10 2 GeV lifetime The number of photon from decay of X is m 1 X with fixed m X Y X. { The observed neutrino flux is roughly E0 3. The observed photon flux is roughly E 2. 0 lifetime { [m X Y X ] upper bound m X m 3 X [m X Y X ] upper bound m X m 2 X m X m 1 X m X const. ( neutrino ) ( photon )
Big Bang Nucleosynthesis and Particle Physics
New Generation Quantum Theory -Particle Physics, Cosmology and Chemistry- Kyoto University Mar.7-9 2016 Big Bang Nucleosynthesis and Particle Physics Masahiro Kawasaki (ICRR & Kavli IPMU, University of
More informationarxiv: v1 [hep-ph] 5 Sep 2017
IPMU17-0117 UT-17-29 September, 2017 arxiv:1709.01211v1 [hep-ph] 5 Sep 2017 Revisiting Big-Bang Nucleosynthesis Constraints on Long-Lived Decaying Particles Masahiro Kawasaki (a,b), Kazunori Kohri (c,d,e),
More informationarxiv: v3 [hep-ph] 3 Dec 2018
IPMU17-0117 UT-17-29 September, 2017 arxiv:1709.01211v3 [hep-ph] 3 Dec 2018 Revisiting Big-Bang Nucleosynthesis Constraints on Long-Lived Decaying Particles Masahiro Kawasaki (a,b), Kazunori Kohri (c,d),
More informationastro-ph/ Dec 1994
TU-474 ICRR-Report-333-94-8 astro-phxxxx Electromagnetic Cascade in the Early Universe and its Application to the Big-Bang Nucleosynthesis M. Kawasaki 1 and T. Moroi y 1 Institute for Cosmic Ray Research,
More informationPrimordial (Big Bang) Nucleosynthesis
Primordial (Big Bang) Nucleosynthesis H Li Be Which elements? He METALS - 1942: Gamow suggests a Big Bang origin of the elements. - 1948: Alpher, Bethe & Gamow: all elements are synthesized minutes after
More informationDark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis
Dark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis Institute for Cosmic Ray Research, University of Tokyo Kazunori Nakayama J.Hisano, M.Kawasaki, K.Kohri and KN, arxiv:0810.1892 J.Hisano,
More informationLecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741
Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals
More informationDark Matter from Decays
Dark Matter from Decays Manoj Kaplinghat Center for Cosmology University of California, Irvine Collaborators James Bullock, Arvind Rajaraman, Louie Strigari Cold Dark Matter: Theory Most favored candidate
More informationarxiv:astro-ph/ v2 2 Mar 2005
ICRR-Report-508-2004-6 OU-TAP-234 TU-727 astro-ph/0408426 August, 2004 arxiv:astro-ph/0408426v2 2 Mar 2005 Big-Bang Nucleosynthesis and Hadronic Decay of Long-Lived Massive Particles Masahiro Kawasaki
More informationTheory Group. Masahiro Kawasaki
Theory Group Masahiro Kawasaki Current members of theory group Staffs Masahiro Kawasaki (2004~) cosmology Masahiro Ibe (2011~) particle physics Postdoctoral Fellows Shuichiro Yokoyama Shohei Sugiyama Daisuke
More informationGravitino LSP as Dark Matter in the Constrained MSSM
Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, 20-24 June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration
More informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
More informationCosmological Constraints! on! Very Dark Photons
Cosmological Constraints on Very Dark Photons Anthony Fradette work presented in AF, Maxim Pospelov, Josef Pradler, Adam Ritz : PRD Aug 204 (arxiv:407.0993) Cosmo 204 - Chicago, IL Plan Dark Photon review
More information12 Big Bang Nucleosynthesis. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
12 Big Bang Nucleosynthesis introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 12.1 The Early Universe According to the accepted cosmological theories: The Universe has cooled during its expansion
More informationPossible sources of very energetic neutrinos. Active Galactic Nuclei
Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical
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 informationDark Radiation from Particle Decay
Dark Radiation from Particle Decay Jörn Kersten University of Hamburg Based on Jasper Hasenkamp, JK, JCAP 08 (2013), 024 [arxiv:1212.4160] Jörn Kersten (Uni Hamburg) Dark Radiation from Particle Decay
More informationarxiv:hep-ph/ v1 20 Jul 2005
hep-ph/0507245 OU-TAP-26 TU-749 July, 2005 arxiv:hep-ph/0507245v 20 Jul 2005 Big-Bang Nucleosynthesis with Unstable Gravitino and Upper Bound on the Reheating Temperature Kazunori Kohri a,b, Takeo Moroi
More informationNuclear Astrophysics - I
Nuclear Astrophysics - I Carl Brune Ohio University, Athens Ohio Exotic Beam Summer School 2016 July 20, 2016 Astrophysics and Cosmology Observations Underlying Physics Electromagnetic Spectrum: radio,
More informationVery Dark Photons! (in Cosmology) Anthony Fradette. work presented in AF, Maxim Pospelov, Josef Pradler, Adam Ritz : PRD Aug 2014 (arxiv:1407.
Very Dark Photons (in Cosmology) Anthony Fradette work presented in AF, Maxim Pospelov, Josef Pradler, Adam Ritz : PRD Aug 204 (arxiv:407.0993) Theoretical Perspective on New Physics at the Intensity Frontier
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 informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
More informationMatter vs. Antimatter in the Big Bang. E = mc 2
Matter vs. Antimatter in the Big Bang Threshold temperatures If a particle encounters its corresponding antiparticle, the two will annihilate: particle + antiparticle ---> radiation * Correspondingly,
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 informationThe first 400,000 years
The first 400,000 years All about the Big Bang Temperature Chronology of the Big Bang The Cosmic Microwave Background (CMB) The VERY early universe Our Evolving Universe 1 Temperature and the Big Bang
More informationCosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation
Cosmology Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Energy density versus scale factor z=1/a-1 Early times,
More informationTau Neutrino Physics Introduction. Barry Barish 18 September 2000
Tau Neutrino Physics Introduction Barry Barish 18 September 2000 ν τ the third neutrino The Number of Neutrinos big-bang nucleosynthesis D, 3 He, 4 He and 7 Li primordial abundances abundances range over
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,
More informationBig-Bang Nucleosynthesis (BBN) & Supersymmetric Model with Heavy Sfermions
Big-Bang Nucleosynthesis (BBN) & Supersymmetric Model with Heavy Sfermions Takeo Moroi (Tokyo) Helsinki (2017.09.28) 1. Introduction & Outline Today, I discuss: BBN constraints on the decaying gravitino
More informationNeutrinos and Big-Bang Nucleosynthesis
1 Neutrinos and Big-Bang Nucleosynthesis T. KAJINO a b c and M. ORITO a a National Astronomical Observatory, Division of Theoretical Astrophysics b The Graduate University for Advanced Studies, Department
More informationBig Bang Nucleosynthesis
Big Bang Nucleosynthesis Grazia Luparello PhD Course Physics of the early Universe Grazia Luparello 1 / 24 Summary 1 Introduction 2 Neutron - proton ratio (at T1MeV) 3 Reactions for the
More informationarxiv: v1 [hep-ph] 23 Apr 2008
TU-812 April, 2008 arxiv:0804.3745v1 [hep-ph] 23 Apr 2008 Big-Bang Nucleosynthesis and Gravitino (a)(b) Masahiro Kawasaki, (c) Kazunori Kohri, (d) Takeo Moroi, (d) Akira Yotsuyanagi (a) Institute for Cosmic
More informationLecture 19 Big Bang Nucleosynthesis
Lecture 19 Big Bang Nucleosynthesis As with all course material (including homework, exams), these lecture notes are not be reproduced, redistributed, or sold in any form. The CMB as seen by the WMAP satellite.!2
More informationCMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
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 informationPlasma Universe. The origin of CMB
Plasma Universe As we go back in time, temperature goes up. T=2.73(1+z) K At z~1100, T~3000 K About the same temperature as M-dwarfs Ionization of hydrogen atoms H + photon! p + e - Inverse process: recombination
More informationLearning from WIMPs. Manuel Drees. Bonn University. Learning from WIMPs p. 1/29
Learning from WIMPs Manuel Drees Bonn University Learning from WIMPs p. 1/29 Contents 1 Introduction Learning from WIMPs p. 2/29 Contents 1 Introduction 2 Learning about the early Universe Learning from
More information4 The Big Bang, the genesis of the Universe, the origin of the microwave background
4 The Big Bang, the genesis of the Universe, the origin of the microwave background a(t) = 0 The origin of the universe: a(t) = 0 Big Bang coined by Fred Hoyle he calculated the ratio of elements created
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 informationCMB & Light Degrees of Freedom
CMB & Light Degrees of Freedom Joel Meyers Canadian Institute for Theoretical Astrophysics SLAC Summer Institute 2017 Cosmic Opportunities August 21, 2017 Image Credits: Planck, ANL Light Relics What and
More informationPhysics Quarknet/Service Learning
Physics 29000 Quarknet/Service Learning Lecture 3: Ionizing Radiation Purdue University Department of Physics February 1, 2013 1 Resources Particle Data Group: http://pdg.lbl.gov Summary tables of particle
More informationstringent constraint on galactic positron production
stringent constraint on galactic positron production the ohio state university Phys. Rev. Lett. 97, 071102 (2006) [astro-ph/0512411] in collaboration with john beacom Workshop on TeV Particle Astrophysics
More informationSupersymmetric dark matter with low reheating temperature of the Universe
Supersymmetric dark matter with low reheating temperature of the Universe Sebastian Trojanowski National Center for Nuclear Research, Warsaw COSMO 204 Chicago, August 29, 204 L. Roszkowski, ST, K. Turzyński
More informationThe Cosmic Lithium Problems and Supersymmetric Dark Matter
The Cosmic Lithium Problems and Supersymmetric Dark Matter Karsten JEDAMZIK LPTA, Montpellier Karsten Jedamzik, Chicago, a cold December day in 05 p.1/21 The Li Problem 7e-10 6e-10 "observed" "predicted"
More informationPhys/Astro 689: Lecture 1. Evidence for Dark Matter
Phys/Astro 689: Lecture 1 Evidence for Dark Matter Why? This class is primarily a consideration of whether Cold Dark Matter theory can be reconciled with galaxy observations. Spoiler: CDM has a small scale
More informationInteractions. Laws. Evolution
Lecture Origin of the Elements MODEL: Origin of the Elements or Nucleosynthesis Fundamental Particles quarks, gluons, leptons, photons, neutrinos + Basic Forces gravity, electromagnetic, nuclear Interactions
More information. Thus his equation would have to be of the form. 2 t. but must also satisfy the relativistic energy-momentum relation. H 2 φ = ( p 2 + m 2 )φ (3)
1 Antiparticles The Klein-Gordon equation 2 φ t 2 + 2 φ = m 2 φ 1 that we derived in the previous lecture is not satisfactory for dealing with massive particles that have spin. Such an equation must take
More informationPropagation in the Galaxy 2: electrons, positrons, antiprotons
Propagation in the Galaxy 2: electrons, positrons, antiprotons As we mentioned in the previous lecture the results of the propagation in the Galaxy depend on the particle interaction cross section. If
More informationVisit for more fantastic resources. AQA. A Level. A Level Physics. Particles (Answers) Name: Total Marks: /30
Visit http://www.mathsmadeeasy.co.uk/ for more fantastic resources. AQA A Level A Level Physics Particles (Answers) Name: Total Marks: /30 Maths Made Easy Complete Tuition Ltd 2017 1. This question explores
More informationLecture 2: The First Second origin of neutrons and protons
Lecture 2: The First Second origin of neutrons and protons Hot Big Bang Expanding and cooling Soup of free particles + anti-particles Symmetry breaking Soup of free quarks Quarks confined into neutrons
More informationWIMPs and superwimps. Jonathan Feng UC Irvine. MIT Particle Theory Seminar 17 March 2003
WIMPs and superwimps Jonathan Feng UC Irvine MIT Particle Theory Seminar 17 March 2003 Dark Matter The dawn (mid-morning?) of precision cosmology: Ω DM = 0.23 ± 0.04 Ω total = 1.02 ± 0.02 Ω baryon = 0.044
More informationXI. Beyond the Standard Model
XI. Beyond the Standard Model While the Standard Model appears to be confirmed in all ways, there are some unclear points and possible extensions: Why do the observed quarks and leptons have the masses
More informationNeutrino Mass Limits from Cosmology
Neutrino Physics and Beyond 2012 Shenzhen, September 24th, 2012 This review contains limits obtained in collaboration with: Emilio Ciuffoli, Hong Li and Xinmin Zhang Goal of the talk Cosmology provides
More information1920s 1990s (from Friedmann to Freedman)
20 th century cosmology 1920s 1990s (from Friedmann to Freedman) theoretical technology available, but no data 20 th century: birth of observational cosmology Hubble s law ~1930 Development of astrophysics
More informationLecture 17: the CMB and BBN
Lecture 17: the CMB and BBN As with all course material (including homework, exams), these lecture notes are not be reproduced, redistributed, or sold in any form. Peering out/back into the Universe As
More informationSplit SUSY and the LHC
Split SUSY and the LHC Pietro Slavich LAPTH Annecy IFAE 2006, Pavia, April 19-21 Why Split Supersymmetry SUSY with light (scalar and fermionic) superpartners provides a technical solution to the electroweak
More informationThe Linear Collider and the Preposterous Universe
The Linear Collider and the Preposterous Universe Sean Carroll, University of Chicago 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Why do these components dominate our universe? Would an Apollonian
More information14 Lecture 14: Early Universe
PHYS 652: Astrophysics 70 14 Lecture 14: Early Universe True science teaches us to doubt and, in ignorance, to refrain. Claude Bernard The Big Picture: Today we introduce the Boltzmann equation for annihilation
More informationAstr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic
Astr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic Inflation Galaxy Formation 1 Chapter 24: #3 Chapter
More informationDark Matter in the Universe
Dark Matter in the Universe NTNU Trondheim [] Experimental anomalies: WMAP haze: synchrotron radiation from the GC Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron
More informationNeutrinos and Astrophysics
Neutrinos and Astrophysics Astrophysical neutrinos Solar and stellar neutrinos Supernovae High energy neutrinos Cosmology Leptogenesis Big bang nucleosynthesis Large-scale structure and CMB Relic neutrinos
More informationMatter-antimatter asymmetry in the Universe
Matter-antimatter asymmetry in the Universe Wan-il Park (KIAS) APCTP-TRP, Nov. 30 - Dec. 01 (2012), APCTP, Seoul 1 Plan Lecture 1 - Our universe - Birth of antimatter - Matter vs. antimatter - Baryon asymmetry
More informationMICROPHYSICS AND THE DARK UNIVERSE
MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances
More informationCosmology II: The thermal history of the Universe
.. Cosmology II: The thermal history of the Universe Ruth Durrer Département de Physique Théorique et CAP Université de Genève Suisse August 6, 2014 Ruth Durrer (Université de Genève) Cosmology II August
More informationSubir Sarkar
Trinity 2016 Oxford 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
More informationThe Big Bang Theory, General Timeline. The Planck Era. (Big Bang To 10^-35 Seconds) Inflationary Model Added. (10^-35 to 10^-33 Of A Second)
The Big Bang Theory, General Timeline The Planck Era. (Big Bang To 10^-35 Seconds) The time from the exact moment of the Big Bang until 10^-35 of a second later is referred to as the Planck Era. While
More informationthe astrophysical formation of the elements
the astrophysical formation of the elements Rebecca Surman Union College Second Uio-MSU-ORNL-UT School on Topics in Nuclear Physics 3-7 January 2011 the astrophysical formation of the elements lecture
More informationThe Dark Matter Problem
The Dark Matter Problem matter : anything with equation of state w=0 more obvious contribution to matter: baryons (stars, planets, us!) and both Big Bang Nucleosynthesis and WMAP tell us that Ω baryons
More informationComputational Applications in Nuclear Astrophysics using JAVA
Computational Applications in Nuclear Astrophysics using JAVA Lecture: Friday 10:15-11:45 Room NB 7/67 Jim Ritman and Elisabetta Prencipe j.ritman@fz-juelich.de e.prencipe@fz-juelich.de Computer Lab: Friday
More informationBeyond standard model physics signatures in small scale structure
Beyond standard model physics signatures in small scale structure Manoj Kaplinghat Center for Cosmology UC Irvine photo by Art Rosch Outline Dark matter model space and link to Beyond Standard Model physics
More information20. BIG-BANG NUCLEOSYNTHESIS
20. Big-Bang nucleosynthesis 1 20. BIG-BANG NUCLEOSYNTHESIS Revised October 2003 by B.D. Fields (Univ. of Illinois) and S. Sarkar (Univ. of Oxford). Big-bang nucleosynthesis (BBN) offers the deepest reliable
More informationElectromagnetic and hadronic showers development. G. Gaudio, M. Livan The Art of Calorimetry Lecture II
Electromagnetic and hadronic showers development 1 G. Gaudio, M. Livan The Art of Calorimetry Lecture II Summary (Z dependence) Z Z 4 5 Z(Z + 1) Z Z(Z + 1) 2 A simple shower 3 Electromagnetic Showers Differences
More informationPHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
More informationPhysics of the hot universe!
Cosmology Winter School 5/12/2011! Lecture 2:! Physics of the hot universe! Jean-Philippe UZAN! The standard cosmological models! a 0!! Eq. state! Scaling Scale factor! radiation! w=1/3! a -4! t 1/2! Matter
More informationParticle Physics (concise summary) QuarkNet summer workshop June 24-28, 2013
Particle Physics (concise summary) QuarkNet summer workshop June 24-28, 2013 1 Matter Particles Quarks: Leptons: Anti-matter Particles Anti-quarks: Anti-leptons: Hadrons Stable bound states of quarks Baryons:
More informationOrigin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean?
Origin of the Universe - 2 ASTR 2120 Sarazin What does it all mean? Fundamental Questions in Cosmology 1. Why did the Big Bang occur? 2. Why is the Universe old? 3. Why is the Universe made of matter?
More informationLimits on Cosmic Matter Antimatter Domains from Big Bang Nucleosynthesis
Limits on Cosmic Matter Antimatter Domains from Big Bang Nucleosynthesis Jan B. Rehm and Karsten Jedamzik Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany (June 29,
More informationCosmology: Building the Universe.
Cosmology: Building the Universe. The term has several different meanings. We are interested in physical cosmology - the study of the origin and development of the physical universe, and all the structure
More informationIndirect Dark Matter Detection
Indirect Dark Matter Detection Martin Stüer 11.06.2010 Contents 1. Theoretical Considerations 2. PAMELA 3. Fermi Large Area Telescope 4. IceCube 5. Summary Indirect Dark Matter Detection 1 1. Theoretical
More informationGravitino Dark Matter p.1/42. with broken R-parity
Gravitino Dark Matter with broken R-parity In collaboration with Alejandro Ibarra DESY W. Buchmüller, L. Covi, K. Hamaguchi and T. Yanagida (JHEP 0703:037, 2007) G. Bertone, W. Buchmüller, L. Covi (JCAP11(2007)003)
More informationDoctopic: Phenomenology ARTICLE IN PRESS PLB:26744 JID:PLB AID:26744 /SCO Doctopic: Phenomenology [m5gv1.3; v 1.38; Prn:6/05/2010; 11:50] P.
Doctopic: Phenomenology ATICLE IN PESS PLB:26744 JID:PLB AID:26744 /SCO Doctopic: Phenomenology [m5gv1.3; v 1.38; Prn:6/05/2010; 11:50] P.1 (1-6) Physics Letters B ( ) Contents lists available at ScienceDirect
More informationThe Early Universe. Overview: The Early Universe. Accelerators recreate the early universe. Simple Friedmann equation for the radiation era:
The Early Universe Notes based on Teaching Company lectures, and associated undergraduate text with some additional material added. ) From µs to s: quark confinement; particle freezout. 2) From s to 3
More informationConcordance Cosmology and Particle Physics. Richard Easther (Yale University)
Concordance Cosmology and Particle Physics Richard Easther (Yale University) Concordance Cosmology The standard model for cosmology Simplest model that fits the data Smallest number of free parameters
More informationDARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium
DARK MATTERS Jonathan Feng University of California, Irvine 2 June 2005 UCSC Colloquium 2 June 05 Graphic: Feng N. Graf 1 WHAT IS THE UNIVERSE MADE OF? An age old question, but Recently there have been
More informationarxiv:hep-ph/ v2 12 Sep 2006
Preprint typeset in JHEP style - PAPER VERSION hep-ph/0605306 MPP-2006-66 arxiv:hep-ph/0605306v2 12 Sep 2006 Gravitino Dark Matter and Cosmological Constraints Frank Daniel Steffen Max-Planck-Institut
More informationObservational Prospects for Quark Nugget Dark Matter
Observational Prospects for Quark Nugget Dark Matter Kyle Lawson University of British Columbia Partially based on material reviewed in http://arxiv.org/abs/1305.6318 Outline Baryogenesis (matter/antimatter
More informationLecture 3: Big Bang Nucleosynthesis The First Three Minutes
Lecture 3: Big Bang Nucleosynthesis The First Three Minutes Last time: particle anti-particle soup --> quark soup --> neutron-proton soup p / n ratio at onset of 2 D formation Today: Form 2 D and 4 He
More informationASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER
16 December 2011 ASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER Paolo Ciarcelluti Motivation of this research We are now in the ERA OF PRECISION COSMOLOGY and... Motivation of this research We are now
More informationEpisode 535: Particle reactions
Episode 535: Particle reactions This episode considers both hadrons and leptons in particle reactions. Students must take account of both conservation of lepton number and conservation of baryon number.
More informationCOSMOLOGY AT COLLIDERS
COSMOLOGY AT COLLIDERS Jonathan Feng University of California, Irvine 23 September 2005 SoCal Strings Seminar 23 September 05 Graphic: Feng N. Graf 1 COSMOLOGY NOW We are living through a revolution in
More informationSignatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:
Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in
More informationWeek 3: Thermal History of the Universe
Week 3: Thermal History of the Universe Cosmology, Ay127, Spring 2008 April 21, 2008 1 Brief Overview Before moving on, let s review some of the high points in the history of the Universe: T 10 4 ev, t
More informationParticle Cosmology. V.A. Rubakov. Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University
Particle Cosmology V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University Topics Basics of Hot Big Bang cosmology Dark matter: WIMPs Axions Warm
More informationRECENT PROGRESS IN SUSY DARK MATTER
RECENT PROGRESS IN SUSY DARK MATTER Jonathan Feng University of California, Irvine 12 April 2006 Texas A&M Mitchell Symposium 12 Apr 06 Graphic: Feng N. Graf 1 Supersymmetric dark matter has been around
More informationStochastic Backgrounds
Stochastic Backgrounds For our last lecture, we will focus on stochastic backgrounds, with an emphasis on primordial gravitational waves. To get a handle on these issues, we need to think in terms of broad
More informationDecaying Dark Matter and the PAMELA anomaly
Decaying Dark Matter and the PAMELA anomaly Alejandro Ibarra Technische Universität München In collaboration with Wilfried Buchmüller, Gianfranco Bertone, Laura Covi, Michael Grefe, Koichi Hamaguchi, Tetsuo
More informationTopics in Nuclear Astrophysics. John Beacom, Theoretical Astrophysics Group, Fermilab
Topics in Nuclear Astrophysics John Beacom Theoretical Astrophysics Group, Fermilab Classical Nuclear Astrophysics How do stars shine? How old is the Universe? How do supernovae work? How do neutron stars
More informationOption 212: UNIT 2 Elementary Particles
Department of Physics and Astronomy Option 212: UNIT 2 Elementary Particles SCHEDULE 26-Jan-15 13.pm LRB Intro lecture 28-Jan-15 12.pm LRB Problem solving (2-Feb-15 1.am E Problem Workshop) 4-Feb-15 12.pm
More informationMeasurementof 7 Be(n,α) and 7 Be(n,p) cross sections for the Cosmological Li problem in
Measurementof Be(n,α) and Be(n,p) cross sections for the Cosmological Li problem in EAR2@n_TOF M. Barbagallo, A. Musumarra, L. Cosentino, N. Colonna, P. Finocchiaro, A. Pappalardo and the n_tof Collaboration
More informationPERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
More information