Precise Measurement of Cosmic‐Ray Proton and Helium Spectra with the BESS Spectrometer

Sanuki, T.; Motoki, M.; Matsumoto, Hiroshi; Seo, E. S.; Wang, J. Z.; Abe, K.; Anraku, K.; Asaoka, Y.; Fujikawa, M.; Imori, M.; Maeno, T.; Makida, Y.; Matsui, N.; Matsunaga, H.; Mitchell, J. W.; Mitsui, T.; Моисеев, А. А.; Nishimura, Jun; Nozaki, M.; Orito, S.; Ormes, J. F.; Saeki, T.; Sasaki, M.; Shikaze, Y.; Sonoda, T.; Streitmatter, R. E.; Suzuki, Jun–ichi; Tanaka, Kenichi; Ueda, I.; Yajima, N.; Yamagami, T.; Yamamoto, A.; Yoshida, Tetsuya; Yoshimura, K.

doi:10.1086/317873

Cited by 312 publications

(232 citation statements)

References 28 publications

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“…1 are well determined below 100 GeV, since the observed data by AMS-01 [7] and BESS [8,9] show a very good agreement. We used the atmospheric muon spectra observed mainly by BESS [9,20,21].…”

Section: Hadronic Interaction Model and Muon Calibrationmentioning

confidence: 71%

“…We used the primary flux model based on AMS [7] and BESS [8,9] data shown in Fig. 1 For the 3-dimensional calculation, we assumed the surface of the earth is a sphere with radius of R e =63781.80 km.…”

Section: Calculation Schemementioning

confidence: 99%

“…Small triangles show the AMS-01 [7] data, small circles BESS [8], small squares BESS-TeV [9], Large triangles JACEE [12], and large squares RUNJOB [13].…”

Section: Calculation Schemementioning

confidence: 99%

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Theory Predictions for Inclusive atmospheric Neutrino flux

Honda

2013

EPJ Web of Conferences

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Abstract. We describe the history of theory prediction of inclusive atmospheric neutrino flux shortly, then the 3-dimensional calculation of atmospheric neutrino flux in some detail. With the calculated atmospheric neutrino flux for INO and South Pole, we discuss on the relation of atmospheric neutrino flux and geomagnetic field. We find the full 3-dimensional scheme calculation is necessary for the theory prediction of the atmospheric neutrino flux. Short history as the introductionThe atmospheric neutrino flux is calculated in the 1-dimensional scheme for long time [1,2]. It is believed that the 1-dimensional scheme calculation is good enough because of the nature of the hadronic interaction and the small muon bending angle in the geomagnetic field ( ∼5 degree) before the decay. Also the 3-dimensional scheme calculation is very inefficient computation compared to the 1dimensional scheme calculation. We had considered it is impossible to complete within a reasonable computation time.These situation continued until Fluka group [3] reported the calculation in a 3-dimensional scheme, limiting the effect of geomagnetic field only to the rigidity cutoff. In this scheme of the calculation, they could reduce the computation time largely, but find a large horizontal enhancement of neutrino flux, which is not seen in the 1-dimensional scheme calculation.The importance of the geomagnetic field in the atmosphere is discussed by Lipari [4] qualitatively, and a 3-dimensional scheme calculation with the geomagnetic field in the atmosphere was carried out by Barr et al. [5], supporting the discussion of Lipari quantitatively. However, they introduced many acceleration technique in their calculation. It is not a full 3-dimensional calculation yet.A calculation a little more close to the full 3-dimensional scheme was carried out by Honda et al. [6], with fast interaction code and virtual detector correction. We illustrate this work and the following developments in this paper. Calculation SchemeFor the calculation of atmospheric neutrino flux, we need the primary cosmic ray spectra model, the atmosphere model, and the geomagnetic field model, other than the a e-mail: mhonda@icrr.u-tokyo.ac.jp hadronic interaction model. We used the primary flux model based on AMS [7] and BESS [8,9] data shown in Fig. 1 For the 3-dimensional calculation, we assumed the surface of the earth is a sphere with radius of R e =63781.80 km. In addition to the surface of the earth we assumed three more spheres, the injection sphere, the simulation sphere, and the escape sphere. We have taken the radius of the injection sphere as R in j = R e + 100km, and the radius of simulation sphere as R esc = R sim = 3 × R e , and that of escape sphere as R esc = R sim = 10 × R e =63781.80 km EPJ Web of Conferences

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Section: Hadronic Interaction Model and Muon Calibrationmentioning

confidence: 71%

Section: Calculation Schemementioning

confidence: 99%

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Theory Predictions for Inclusive atmospheric Neutrino flux

Honda

2013

EPJ Web of Conferences

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“…In order to allow a direct comparison with previously published computations, we used the fit of all-nucleon flux proposed by the Bartol group [3]. This flux has also the merit that, at least up to about hundred GeV it is quite close to the recent measurements of proton primaries performed by BESS [8] and AMS [9]. A comparison with these data sets is shown in Fig.…”

Section: Monte Carlo Setupmentioning

confidence: 99%

Comparison of the FLUKA calculations with CAPRICE94 data on muons in atmosphere

Battistoni¹,

Ferrari²,

Montaruli³

et al. 2002

Astroparticle Physics

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In order to benchmark the 3-dimensional calculation of the atmospheric neutrino flux based on the FLUKA Monte Carlo code, muon fluxes in the atmosphere have been computed and compared with data taken by the CAPRICE94 experiment at ground level and at different altitudes in the atmosphere. For this purpose only two additions have been introduced with respect to the neutrino flux calculation: the specific solar modulation corresponding to the period of data taking and the bending of charged particles in the atmosphere. Results are in good agreement with experimental data, although improvements in the model are possible. At this level, however, it is not possible to disentangle the interplay between the primary flux and the interaction model.

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“…Figure 1. Left: Calculated proton interstellar spectrum (LIS) and modulated spectrum (Φ = 750 MV) with data [8][9][10][11]. Right: Calculatedp interstellar spectrum (LIS) and modulated spectrum (Φ = 400 MV) with data [12,13].…”

Section: Introductionmentioning

confidence: 99%

Antiprotons below 200MeV in the interstellar medium: perspectives for observing exotic matter signatures

Moskalenko

Christian

Моисеев

et al. 2001

The Outer Heliosphere: The Next Frontiers, Proceedings of the COSPAR Colloquium

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Most cosmic ray antiprotons observed near the Earth are secondaries produced in collisions of energetic cosmic ray (CR) particles with interstellar gas. The spectrum of secondary antiprotons is expected to peak at ∼ 2 GeV and decrease sharply at lower energies. This leaves a low energy window in which to look for signatures of exotic processes such as evaporation of primordial black holes or dark matter annihilation. In the inner heliosphere, however, modulation of CRs by the solar wind makes analysis difficult. Detecting these antiprotons outside the heliosphere on an interstellar probe removes most of the complications of modulation. We present a new calculation of the expected secondary antiproton flux (the background) as well as a preliminary design of a light-weight, low-power instrument for the interstellar probe to make such measurements.

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Precise Measurement of Cosmic‐Ray Proton and Helium Spectra with the BESS Spectrometer

Cited by 312 publications

References 28 publications

Theory Predictions for Inclusive atmospheric Neutrino flux

Theory Predictions for Inclusive atmospheric Neutrino flux

Comparison of the FLUKA calculations with CAPRICE94 data on muons in atmosphere

Antiprotons below 200MeV in the interstellar medium: perspectives for observing exotic matter signatures

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