Cosmic ray physics and AUGER latest results

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48 Cosmic-ray clocks ■ 12 C + H → 9 Be (stable secondary nucleus) 12 C + H → 10 Be (unstable secondary nucleus: ~ 4 Myr) AMS: 1 yr ■ ■ The 10 Be/ 9 Be ratio depends on the history of secondary nuclei production (on cross sections) Link between time and the quantity of matter gone through Paris, 9 th June 2008 — IDAPPʼs two days 2008 — E. Parizot (APC / Univ. Paris 7)
49 Some results ■ ■ ■ ■ Secondary/primary ratios ⇒ CRs have gone through a grammage of X RC = 6–10 g/cm 2 on average, from their sources to the Earth Cosmic-ray clocks ⇒ CRs have spent typically t RC ~ 2 10 7 years on their way Thus, they propagated in a medium of average density n = X RC /ct RC ~ 0.2 part. cm -3 Thus, they must have spent most of their time in the halo! Paris, 9 th June 2008 — IDAPPʼs two days 2008 — E. Parizot (APC / Univ. Paris 7)
Page 1 and 2: 1 Cosmic-ray physics and Auger late
Page 3 and 4: 3 Cosmic rays: “CRs” ■ Key su
Page 5 and 6: Cosmic ray physics started one cent
Page 7 and 8: 7 Viktor Hess: August, 7 th 1912 12
Page 9 and 10: 9 Then a long story began… ■
Page 11 and 12: 11 CR-induced atmospheric showers P
Page 13 and 14: Schism… and ecumenism! 13 study o
Page 15 and 16: A remarkably coherent, though myste
Page 17 and 18: [CR flux] x E 3 17 ■ Essentially
Page 19 and 20: 19 The way out of the mist ■ Anal
Page 21 and 22: 21 Propagation: a “3-space” pro
Page 23 and 24: 23 Angular distribution ■ Isotrop
Page 25 and 26: Interaction with B inhomogeneities
Page 27 and 28: Reaching the diffusive regime 27 <
Page 29 and 30: Diffusive transport and GCR confine
Page 31 and 32: GCR large angular scale anisotropy
Page 33 and 34: larger energy 33 Paris, 9 th June 2
Page 35 and 36: still larger energy 35 “Ballistic
Page 37 and 38: 37 Propagation: a “3-space” pro
Page 39 and 40: Energy losses and nuclear interacti
Page 41 and 42: Pion production in interstellar med
Page 43 and 44: Nuclear interactions in ISM 43 Pari
Page 45 and 46: Composition: CR vs solar system 45
Page 47: Secondary/primary ratios 47 Strong
Page 51 and 52: 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 and 104:
Summary of Auger results 103 compos
Page 105 and 106:
Galactic/Extragalactic transition 1
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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