Cosmic ray physics and AUGER latest results

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Cosmic rays, year zero! 104 ■ Historical opening of a non-photonic astronomy! ◆ ◆ Eventually: identification and study of individual sources Necessary to increase collecting power at the highest energies Auger Nord (Lamar, Colorado) (sources are there: letʼs go and get them!) Shower detection from space (JEM-EUSO, S-EUSO…) ■ Many questions ◆ ◆ sources, CR origin, acceleration mechanisms, behaviour of energetic sources in the universe, link with low-energy CRs and galactic ecology study of high-energy physics (LHC results are awaited!) Paris, 9 th June 2008 — IDAPPʼs two days 2008 — E. Parizot (APC / Univ. Paris 7)
Galactic/Extragalactic transition 105 ■ Fixed by flux rather than confinement? low-energy CRs are confined in galaxies ⇒ enhanced flux high-energy CRs fill the intergalactic medium ■ Transition occurs when EGCR flux ≥ GCR flux extragalactic Galactic Paris, 9 th June 2008 — IDAPPʼs two days 2008 — E. Parizot (APC / Univ. Paris 7)
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1 Cosmic-ray physics and Auger late
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3 Cosmic rays: “CRs” ■ Key su
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Cosmic ray physics started one cent
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7 Viktor Hess: August, 7 th 1912 12
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9 Then a long story began… ■
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11 CR-induced atmospheric showers P
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Schism… and ecumenism! 13 study o
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A remarkably coherent, though myste
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[CR flux] x E 3 17 ■ Essentially
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19 The way out of the mist ■ Anal
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21 Propagation: a “3-space” pro
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23 Angular distribution ■ Isotrop
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Interaction with B inhomogeneities
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Reaching the diffusive regime 27 <
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Diffusive transport and GCR confine
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GCR large angular scale anisotropy
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larger energy 33 Paris, 9 th June 2
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still larger energy 35 “Ballistic
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37 Propagation: a “3-space” pro
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Energy losses and nuclear interacti
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Pion production in interstellar med
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Nuclear interactions in ISM 43 Pari
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Composition: CR vs solar system 45
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Secondary/primary ratios 47 Strong
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49 Some results ■ ■ ■ ■ Sec
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51 Cosmic-ray clocks 54 Mn/Mn 36 Cl
Page 53 and 54: 53 Antiprotons Strong & Moskalenko
Page 55 and 56: Search for dark matter: positron fr
Page 57 and 58: 57 High energy CR propagation ■
Page 59 and 60: 59 [cross section] x [inelasticity]
Page 61 and 62: 61 "Propagated" spectrum z = 0.01,
Page 63 and 64: 63 10 Spectre propagé (source uniq
Page 65 and 66: UHE Nuclei propagation 65 2D nuclea
Page 67 and 68: Fe interaction and energy loss leng
Page 69 and 70: Fit of the spectrum with a “pure
Page 71 and 72: Are there nuclei among EGCRs? 71 Pu
Page 73 and 74: 73 The Pierre Auger Observatory Nor
Page 75 and 76: High-energy CR detection 75 • com
Page 77 and 78: Hexagonal array (1.5 km spacing, 30
Page 79 and 80: Aerial view of Los Leones fluoresce
Page 81 and 82: One of the fluorescence eyes 81 440
Page 83 and 84: 83 Independent analyses of stereo e
Page 85 and 86: Atmospheric depth of shower maximum
Page 87 and 88: Energy reconstruction with surface
Page 89 and 90: Cross-calibration of the detectors
Page 91 and 92: Energy spectrum from SD showers wit
Page 93 and 94: Energy spectrum 93 Paris, 9 th June
Page 95 and 96: Auger main anisotropy result 95 ■
Page 97 and 98: Auger main anisotropy result 97 3 f
Page 99 and 100: Significance of the anisotropy resu
Page 101 and 102: 101 Auger main anisotropy result Th
Page 103: Summary of Auger results 103 compos
Page 107 and 108: Toy model: holistic scenario 107
Page 109 and 110: What is at stake 109 ■ Major disc
Page 111 and 112: 111 Extra slides Paris, 9 th June 2
Page 113 and 114: Photon flux limit 113 astro-ph/0712
Page 115 and 116: Neutrino detection with Auger "GZK
Page 117 and 118: Selection criteria 117 young shower
Page 119 and 120: Horizontal showers 119 Example of a
Page 121 and 122: LiBeB nucleosynthesis 121 ■ Li, B
Page 123: HE photon emission from GCR interac
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Cosmic ray physics and AUGER latest results

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