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Title: Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation

Abstract

We have studied the hadronic interaction for the calculation of the atmospheric neutrino flux by summarizing the accurately measured atmospheric muon flux data and comparing with simulations. We find the atmospheric muon and neutrino fluxes respond to errors in the {pi}-production of the hadronic interaction similarly, and compare the atmospheric muon flux calculated using the HKKM04 [M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 70, 043008 (2004).] code with experimental measurements. The {mu}{sup +}+{mu}{sup -} data show good agreement in the 1{approx}30 GeV/c range, but a large disagreement above 30 GeV/c. The {mu}{sup +}/{mu}{sup -} ratio shows sizable differences at lower and higher momenta for opposite directions. As the disagreements are considered to be due to assumptions in the hadronic interaction model, we try to improve it phenomenologically based on the quark parton model. The improved interaction model reproduces the observed muon flux data well. The calculation of the atmospheric neutrino flux will be reported in the following paper [M. Honda et al., Phys. Rev. D 75, 043006 (2007).].

Authors:
; ; ; ;  [1];  [2];  [2];  [2]
  1. International Center for Elementary Particle Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)
  2. (Japan)
Publication Date:
OSTI Identifier:
21011037
Resource Type:
Journal Article
Resource Relation:
Journal Name: Physical Review. D, Particles Fields; Journal Volume: 75; Journal Issue: 4; Other Information: DOI: 10.1103/PhysRevD.75.043005; (c) 2007 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; COMPARATIVE EVALUATIONS; COMPUTERIZED SIMULATION; COSMIC RADIATION; ERRORS; GEV RANGE; H CODES; HADRONS; MUONS MINUS; MUONS PLUS; NEUTRINOS; PARTICLE INTERACTIONS; QUARK MODEL; QUARKS

Citation Formats

Sanuki, T., Honda, M., Kajita, T., Kasahara, K., Midorikawa, S., Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Shibaura Institute of Technology, 307 Fukasaku, Minuma-ku, Saitama 337-8570, and Faculty of Software and Information Technology, Aomori University, 2-3-1 Kobata, Aomori, Aomori 030-0943. Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation. United States: N. p., 2007. Web. doi:10.1103/PHYSREVD.75.043005.
Sanuki, T., Honda, M., Kajita, T., Kasahara, K., Midorikawa, S., Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Shibaura Institute of Technology, 307 Fukasaku, Minuma-ku, Saitama 337-8570, & Faculty of Software and Information Technology, Aomori University, 2-3-1 Kobata, Aomori, Aomori 030-0943. Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation. United States. doi:10.1103/PHYSREVD.75.043005.
Sanuki, T., Honda, M., Kajita, T., Kasahara, K., Midorikawa, S., Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Shibaura Institute of Technology, 307 Fukasaku, Minuma-ku, Saitama 337-8570, and Faculty of Software and Information Technology, Aomori University, 2-3-1 Kobata, Aomori, Aomori 030-0943. Thu . "Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation". United States. doi:10.1103/PHYSREVD.75.043005.
@article{osti_21011037,
title = {Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation},
author = {Sanuki, T. and Honda, M. and Kajita, T. and Kasahara, K. and Midorikawa, S. and Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582 and Shibaura Institute of Technology, 307 Fukasaku, Minuma-ku, Saitama 337-8570 and Faculty of Software and Information Technology, Aomori University, 2-3-1 Kobata, Aomori, Aomori 030-0943},
abstractNote = {We have studied the hadronic interaction for the calculation of the atmospheric neutrino flux by summarizing the accurately measured atmospheric muon flux data and comparing with simulations. We find the atmospheric muon and neutrino fluxes respond to errors in the {pi}-production of the hadronic interaction similarly, and compare the atmospheric muon flux calculated using the HKKM04 [M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 70, 043008 (2004).] code with experimental measurements. The {mu}{sup +}+{mu}{sup -} data show good agreement in the 1{approx}30 GeV/c range, but a large disagreement above 30 GeV/c. The {mu}{sup +}/{mu}{sup -} ratio shows sizable differences at lower and higher momenta for opposite directions. As the disagreements are considered to be due to assumptions in the hadronic interaction model, we try to improve it phenomenologically based on the quark parton model. The improved interaction model reproduces the observed muon flux data well. The calculation of the atmospheric neutrino flux will be reported in the following paper [M. Honda et al., Phys. Rev. D 75, 043006 (2007).].},
doi = {10.1103/PHYSREVD.75.043005},
journal = {Physical Review. D, Particles Fields},
number = 4,
volume = 75,
place = {United States},
year = {Thu Feb 15 00:00:00 EST 2007},
month = {Thu Feb 15 00:00:00 EST 2007}
}
  • Using the 'modified DPMJET-III' model explained in the previous paper [T. Sanuki et al., preceding Article, Phys. Rev. D 75, 043005 (2007).], we calculate the atmospheric neutrino flux. The calculation scheme is almost the same as HKKM04 [M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 70, 043008 (2004).], but the usage of the 'virtual detector' is improved to reduce the error due to it. Then we study the uncertainty of the calculated atmospheric neutrino flux summarizing the uncertainties of individual components of the simulation. The uncertainty of K-production in the interaction model is estimated using othermore » interaction models: FLUKA'97 and FRITIOF 7.02, and modifying them so that they also reproduce the atmospheric muon flux data correctly. The uncertainties of the flux ratio and zenith angle dependence of the atmospheric neutrino flux are also studied.« less
  • We present the calculation of the atmospheric neutrino fluxes with an interaction model named JAM, which is used in PHITS (Particle and Heavy-Ion Transport code System) [K. Niita et al., Radiation Measurements 41, 1080 (2006).]. The JAM interaction model agrees with the HARP experiment [H. Collaboration, Astropart. Phys. 30, 124 (2008).] a little better than DPMJET-III[S. Roesler, R. Engel, and J. Ranft, arXiv:hep-ph/0012252.]. After some modifications, it reproduces the muon flux below 1 GeV/c at balloon altitudes better than the modified DPMJET-III, which we used for the calculation of atmospheric neutrino flux in previous works [T. Sanuki, M. Honda, T.more » Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 75, 043005 (2007).][M. Honda, T. Kajita, K. Kasahara, S. Midorikawa, and T. Sanuki, Phys. Rev. D 75, 043006 (2007).]. Some improvements in the calculation of atmospheric neutrino flux are also reported.« less
  • The background of cosmic ray muons in the chlorine solar neutrino detector is calculated directly for depths of 25 to 10,000 m.w.e. The charge exchange channel (..pi../sup +/,..pi../sup 0/) is taken into account for the first time and it is shown that inclusion of the increase of the multiplicity of the pions produced in the target fragmentation region leads to an additional increase of the background per muon with increasing depth. The results of the analysis are compared with the experimental points. It is shown that the background from muons at a depth of 4400 m.w.e. is 0.40 SNU, whichmore » corresponds to 0.075 /sup 37/Ar atoms per day in 610 tons of perchloroethylene.« less