Extensive air shower muons: the key of the UHECR puzzle
Transcrição
Extensive air shower muons: the key of the UHECR puzzle
Extensive Air Shower Muons The key of the UHECR puzzle L. Cazon L Cazon NWPAC 29-31 Jan, 2014 Braga 1 Ultra High Energy Cosmic Rays Detection of Primaries Satellites, Balloons Detection of Secondaries (Shower) Ground Arrays GZK-cutoff 2 UHE Particle Physics & UHE Astrophysics Window of oportunity UHECR: exciting and puzzeling. • A few nearby sources shooting iron, with high B deflections? • Many sources shooting protons? • Combinations of both? Intermediate compositions He, C, N, O? If we could separate UHECRs by composition • Beam for UHE particle physics • Dawn of UHE Charged Particle Astronomy But changes in hadronic physics and changes in CR composition often mock each other 3 Electrons Photons Muons Neutrons protons Electrons Photons Muons Neutrons protons Primary: Hadron Hadronic shower (mainly pions) Muonic component Electromagnetic shower (electrons and photons) Muons are the smoking gun of the hadronic cascade which is the real backbone of the whole shower. L Cazon Primary: Photon Hadronic skeletons L Cazon Hadronic reaction NWPAC 29-31 Jan, 2014 Braga 6 L Cazon A A A A A A Generation ordered NWPAC 29-31 Jan, 2014 Braga 7 J. Matthews Astropart.Phys. 22 (2005) 387-397 Hadronic cascade E0 1 N ch 0 N ch2 E0 2 N tot E0 3 N tot N ch3 c 20 GeV L Cazon E0 N tot E ln 0 c E0 nc 0.85 log10 3 c ln N ch 2 N tot 1 N ch N ch 2 The hadronic cascade loses energy that goes into the EM cascade 8 J. Matthews Astropart.Phys. 22 (2005) 387-397 EM cascade 1 E0 2 E0 / 2 22 E0 / 22 23 E0 / 23 24 E0 / 24 L Cazon ce 85MeV E0 ln e c nc ln 2 9 Composition scaling X max X E0 nc r ln( 2) r ln e c max E0 i nc i 0.85 log10 c E0 N c E0 N ln(1 N ch ) c 1 0.14 1 N ch ln 1 3 / 2 A= UHECR mass number E0 X max ( A) r ln ln ce X max ln A A L Cazon E / A ln N ( A) ln A 0 ln N (1 ) ln A c NWPAC 29-31 Jan, 2014 Braga 10 Energy balance dE Ne( X )dX dX dX Ecal h( X )dX N EM channel ends up carrying all the shower energy except a small remaining fraction fraction called “Invisible energy” E0 Ecal bN 1 N ch p (1 k ) E 1 N ch 0 2 c 20 GeV X max h(X) L Cazon X EM max Ne(X) 0.2 1 1 2 kE 3 1 kE 3 k=inelasticity EM n 1 E 1 3 E0 1 n EM E 1 1 3 0.5 Hadronic 11 Full MC simulations & Auger data L Cazon Full MC simulations & Auger data LHC-EPOS makes a better treatement of diffraction rapidity gaps. QGSJetII.04 could be missing additional and relevant effects that compensates Xµmax Deficit of Nµ in all models L Cazon σ(Xµmax) Events Xµmax L Cazon Events σ(Nµ) E [eV] NWPAC 29-31 Jan, 2014 Braga 14 E [eV] Nµ Event by event Mass Separation Xmax - Nµ plane L Cazon NWPAC 29-31 Jan, 2014 Braga 15 Mass / Hadronic models Disentanglement Mock data point p < Nµ > - σ (Nµ ) He N Fe <Xmax> - < Nµ > L Cazon 16 R. Conceição Conclusions • EM component is the most exploited sector of the air shower to study UHECR • Muons carry information from the hadronic skeleton of the shower. They are experimentally underexploited. • The momenta of Nµ , Xmax and Xµmax distributions are very sensitive tools to high energy interaction models and average masses • The combined use of Nµ with Xmax event by event could separate primaries regardless of high energy interaction models. • Clean(er) beam for UHE particle physics and UHE astrophysics 17 L Cazon NWPAC 29-31 Jan, 2014 Braga 18 X max X E0 N c ln(1 N ch ) 1 0.14 1 N ch ln 1 3 / 2 E0 nc r ln( 2) r ln e c max E0 i nc i 0.85 log10 c E0 e X max ( A) r ln ln c X max ln A A E0 / A N ( A) A A1 N c ln N ( A) ln N (1 ) ln A L Cazon NWPAC 29-31 Jan, 2014 Braga 19 mair X 1 ( E ) i ( E ) p air ( E ) Aair ( E ) A p air ( E / A) L Cazon NWPAC 29-31 Jan, 2014 Braga 20 Multivariant analysis Larger discrimination power K.H. Kampert & M.Unger 2011 L Cazon NWPAC 29-31 Jan, 2014 Braga 21
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