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Neutrino Shower Simulation: Status and Prospects

Neutrino Shower Simulation: Status and Prospects. Ofelia Pisanti. Status Open issues Future work. ICRC 2003 – Tsukuba – August 5 th 2003 1/11. Neutrinos as universe messengers. Monte Carlo Simulation of Neutrino Induced EAS.

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Neutrino Shower Simulation: Status and Prospects

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  1. Neutrino Shower Simulation: Status and Prospects Ofelia Pisanti • Status • Open issues • Future work

  2. ICRC 2003 – Tsukuba – August 5th 2003 1/11 Neutrinos as universe messengers Monte Carlo Simulation of Neutrino Induced EAS • observation of EHE n induced showers is very important for getting information on cosmic ray sources in the universe and interactions of n with the matter in presently not accessible energy ranges; • neutrino initiated showers have in principle different signatures from the hadronic ones. But, for extracting physical information from data (Auger) on a more quantitative basis, we need simulations. X. Bertou, P. Billoir, and S. Coutu Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  3. ICRC 2003 – Tsukuba – August 5th 2003 3/11 Flow diagram Monte Carlo Simulation of Neutrino Induced EAS Calculate the first interaction point (chi is the interaction length) chi D. Heck, J. Knapp, J.N. Capdevielle, G. Shatz, and T. Thouw CORSIKA 6.014 main program BOX2 CORSIKA intermediate stack  type, energy P. Marchesini, B. Webber, G. Abbiendi, G. Corcella, I. Knowles, S.Moretti, K. Odagiri, P. Richardson, M. Seymour, and L. Stanco FI particles Link routine between CORSIKA and HERWIG NUINT HERWIG 6.4 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  4. Low energy showers ICRC 2003 – Tsukuba – August 5th 2003 4/11 Monte Carlo Simulation of Neutrino Induced EAS Auger GAP-Note-2003-013 astro-ph/0302602 • Main information: • the fraction of CC events with respect to NC ones is ~ .73 • the lepton carries away an average energy fraction of ~ .70 E = 1015 eV  = 70°  = 0° HDPM Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  5. ICRC 2003 – Tsukuba – August 5th 2003 5/11 Outgoing lepton in FI Monte Carlo Simulation of Neutrino Induced EAS The more the energy of the neutrino the larger the fraction of neutrino energy carried by the outgoing lepton. MRST 98 Leading Order PDF’s: x ≥ 10-6; 1.25 GeV2 ≤ Q2 ≤ 107 GeV2 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  6. Low energy showers ICRC 2003 – Tsukuba – August 5th 2003 4/11 Monte Carlo Simulation of Neutrino Induced EAS Auger GAP-Note-2003-013 astro-ph/0302602 • Main information: • the fraction of CC events with respect to NC ones is ~ .73 • the lepton carries away an average energy fraction of ~ .70 in e showers, with a “good” probability (~ 73%), ~70% of the energy of the primary  goes to the e.m. component E = 1015 eV  = 70°  = 0° HDPM in m showers ~70% of the energy of the primary  is hidden Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  7. Hadronic models ICRC 2003 – Tsukuba – August 5th 2003 7/11 Monte Carlo Simulation of Neutrino Induced EAS good agreement between different hadronic models HDPM HDPM QGSJET QGSJET E = 1015 eV  = 70°  = 0° Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  8. High energy showers ICRC 2003 – Tsukuba – August 5th 2003 10/11 Monte Carlo Simulation of Neutrino Induced EAS • eCC showers very similar to e- ones and more penetrating than p showers • NC first interaction responsible for the suppression of the e profile with respect to the eCC one • extreme suppression of µ profile due to the large fraction of  energy to the outgoing lepton E = 1019 eV  = 70°  = 0° QGSJET Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  9. FI with HERWIG ICRC 2003 – Tsukuba – August 5th 2003 9/11 Monte Carlo Simulation of Neutrino Induced EAS Q2  - q2 = -(k-k’)2 x = Q2/(2 mN) y = / E = (E-El)/ E Q2 = 2 mN E x y 5000 events GRV 98 Leading Order PDF’s: x ≥ 10-9; 0.8 GeV2 ≤ Q2 ≤ 109 GeV2 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  10. ICRC 2003 – Tsukuba – August 5th 2003 9/11 Open issues Monte Carlo Simulation of Neutrino Induced EAS • first interaction with HERWIG: • is HERWIG reliable at 1019 eV? • how much do the results depend on the input parameters (CC and NC  cross • section, PDF’s, …) or on the MC strategy (HERWIG,LEPTO?) Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  11. Impact of PDF’s Auger Meeting – Valencia – October 20th 2003 Neutrino Shower Simulation: Status and Prospect CTEQ6 PDF’s: 38% change with respect to CTEQ4. Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  12. ICRC 2003 – Tsukuba – August 5th 2003 9/11 Open issues Monte Carlo Simulation of Neutrino Induced EAS • first interaction with HERWIG: • is HERWIG reliable at 1019 eV? • how much do the results depend on the input parameters (CC and NC  cross • section, PDF’s, …) or on the MC strategy (HERWIG,LEPTO?) • non recognized particles: • do charmed particles have a main role in changing shower features? • do  induced showers look similar to e or µ ones? Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  13. Charmedparticles Auger Meeting – Valencia – October 20th 2003 Neutrino Shower Simulation: Status and Prospect Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  14. ICRC 2003 – Tsukuba – August 5th 2003 9/11 Open issues Monte Carlo Simulation of Neutrino Induced EAS • first interaction with HERWIG: • is HERWIG reliable at 1019 eV? • how much do the results depend on the input parameters (CC and NC  cross • section, PDF’s, …) or on the MC strategy (HERWIG,LEPTO?) • non recognized particles: • do charmed particles have a main role in changing shower features? • do  induced showers look similar to e or µ ones? • µ interaction with matter: • do the changes make some difference? Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  15. ICRC 2003 – Tsukuba – August 5th 2003 9/11 Open issues Monte Carlo Simulation of Neutrino Induced EAS • first interaction with HERWIG: • is HERWIG reliable at 1019 eV? • how much do the results depend on the input parameters (CC and NC  cross • section, PDF’s, …) or on the MC strategy (HERWIG,LEPTO?) • non recognized particles: • do charmed particles have a main role in changing shower features? • do  induced showers look similar to e or µ ones? • µ interaction with matter: • do the changes make some difference? • LPM effect • which is its impact? Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  16. LPM effect Auger Meeting – Valencia – October 20th 2003 Neutrino Shower Simulation: Status and Prospect deep energetic eCC showers have a very distintive feature due to the separation of the hadronic and electromagnetic component under the LPM effect E = 1020 eV  = 80°  = 0° QGSJET Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  17. Possible Research Lines… Auger Meeting – Valencia – October 20th 2003 Neutrino Shower Simulation: Status and Prospect • statistics on deep showers in the atmosphere (paper): • study of FI with HERWIG/LEPTO • impact of new µ interaction on µ high energy shower features • zero step in simulation (from earth at Auger) • second step in simulation (NUSIM+FDSIM) with Carla • e - µprimaries • 1019 – 1020 – 3 1021 eV • 80° inclination • with/without LPM effect (EUSO type approach) 2 3 1 20+20 240 with Rino, Sergio, Lorenzo, and Marco with Lorenzo, Carla, and Luigi with Rino, Antonio and Nino with Fausto, Rossella, … Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  18. …and Last but not Least Auger Meeting – Valencia – October 20th 2003 Neutrino Shower Simulation: Status and Prospect An official invitation to Villaplana tapas place! Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

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