Cosmic protons

Alcaraz, J.; Alpat, B.; Ambrosi, G.; Anderhub, H.; Ao, L.; Arefiev, A.; Azzarello, P.; Babucci, E.; Baldini, Luca; Basile, M.; Barancourt, D.; Barão, F.; Barbier, G.; Barreira, G.; Battiston, R.; Becker, R. H.; Becker, U.; Bellagamba, L.; Béné, P.; Berdugo, J.; Berges, P.; Bertucci, B.; Biland, A.; Bizzaglia, S.; Blasko, S.; Boella, G.; Boschini, M.; Bourquin, M.; Brocco, L.; Bruni, G.; Buénerd, M.; Burger, J. D.; Burger, W. J.; Cai, Xudong; Camps, C.; Cannarsa, Piermarco; Capell, M.; Casadei, D.; Casaus, J.; Castellini, G.; Cecchi, C.; Chang, Y. H.; Chen, H.F.; Chen, H.S.; Chen, Z.G.; Chernoplekov, N. A.; Chiueh, Tzihong; Chuang, Yao-Li; Cindolo, F.; Commichau, V.; Contin, A.; Crespo, Paulo; Cristinziani, M.; Cunha, J. Pinto da; Dai, T.; Deus, J. Dias de; Dinu, N.; Djambazov, L.; D’Antone, I.; Dong, Zhiwen; Emonet, P.; Engelberg, J.; Eppling, F. J.; Eronen, T.; Esposito, G.; Extermann, P.; Favier, Jean; Fiandrini, E.; Fisher, P. H.; Fluegge, G.; Fouque, N.; Galaktionov, Yu.; Gervasi, M.; Giusti, P.; Grandi, D.; Grimm, O.; Gu, W.; Hangarter, K.; Hasan, A.; Hermel, V.; Hofer, H.; Huang, M. A.; Hungerford, W.; Ionica, M.; Ionica, R.; Jongmanns, M.; Karlamaa, K.; Karpiński, W.; Kenney, G.; Kenny, J. M.; Kim, W.; Klimentov, A.; Kossakowski, R.; Koutsenko, V.; Kraeber, M.; Laborie, G.; Laitinen, Timo; Lamanna, G.; Laurenti, G.; Lebedev, A.; Lee, S.C.; Levi, G.; Levtchenko, P.; Liu, C.L.; Liu, H.T.; Lopes, I.; Lu, Gangcheng; Lu, Y.; Lübelsmeyer, K.; Luckey, D.; Lustermann, W.; Mañá, C.; Margotti, A.; Mayet, F.; McNeil, R. R.; Meillon, Brigitte; Menichelli, M.; Mihul, A.; Mourão, A.; Mujunen, Ari; Palmonari, F.; Papi, Alberto; Park, I.H.; Pauluzzi, M.; Pauß, F.; Perrin, E.; Pesci, A.; Pevsner, A.; Pimenta, M.; Plyaskin, V.; Pojidaev, V.; Pohl, M.; Postolache, V.; Produit, N.; Rancoita, P.G.; Rapin, D.; Raupach, F.; Ren, D.; Ren, Zhiyuan; Ribordy, M.; Richeux, J.P.; Riihonen, E.; Ritakari, Jouko; Roeser, U.; Roissin, C.; Sagdeev, R. Z.; Sartorelli, G.; Dratzig, A. Schultz von; Schwering, G.; Scolieri, G.; Seo, E. S.; Shoutko, V.; Shoumilov, E.; Siedling, R.; Son, D. C.; Song, Tao; Steuer, M.; Sun, G.S.; Suter, H.; Tang, X.; Ting, Samuel C.C.; Ting, S. M.; Tornikoski, M.; Torsti, J.; Trümper, J.; Ulbricht, J.; Urpo, S.; Usoskin, Ilya; Валтонен, Э.; Vandenhirtz, J.; Velcea, F.; Velikhov, E. P.; Verlaat, B.; Vetlitsky, I.; Vezzu, F.; Vialle, J. P.; Viertel, G.; Vitè, Davide; Gunten, H. von; Wicki, S. Waldmeier; Wallraff, W.; Wang, B.C.; Wang, J.Z.; Wang, Y.H.; Wiik, K.; Williams, C.; Wu, S. X.; Xia, Pan; Yan, J.L.; Yan, L.G.; Yang, Changgen; Yang, Min; Ye, S.W.; Yeh, P.; Xu, Zun-Lei; Zhang, H.Y.; Zhang, Z.P.; Zhao, D.X.; Zhu, G.Y.; Zhu, Wei; Zhuang, H. L.; Zichichi, A.; Zimmermann, B.

doi:10.1016/s0370-2693(00)00970-9

Cited by 273 publications

(154 citation statements)

References 11 publications

Supporting

Mentioning

142

Contrasting

Order By: Relevance

“…One sees that the BESS+JACEE fit is in excellent agreement with the recent AMS data on the proton flux [31]. On the other hand it slightly exceeds the AMS helium flux [32] (with average discrepancy of about 15%).…”

Section: Primary Cosmic Ray Spectrum and Compositionsupporting

confidence: 77%

“…Figure 1 shows a comparison between the BESS+JACEE fit, the data from [19,20], the fit from [21] (shaded areas) and several other experiments [22][23][24][25][26][27][28][29][30][31][32], performed in different periods of solar activity. The filled/shaded areas in fig.…”

Section: Primary Cosmic Ray Spectrum and Compositionmentioning

confidence: 99%

“…The filled/shaded areas in fig. 1 represent the power-type parametrizations derived in [20,22,24,28,31,32] from the original data. The legend indicates the publication dates and (when relevant) the years of measurements.…”

Section: Primary Cosmic Ray Spectrum and Compositionmentioning

confidence: 99%

See 2 more Smart Citations

Atmospheric neutrino flux supported by recent muon experiments

2001

View full text Add to dashboard Cite

We present a new one-dimensional calculation of low and intermediate energy atmospheric muon and neutrino fluxes, using up-to-date data on primary cosmic rays and hadronic interactions. We study several sources of uncertainties relevant to our calculations. A comparison with the muon fluxes and charge ratios measured in several modern balloon-borne experiments suggests that the atmospheric neutrino flux is essentially lower than one used for the standard analyses of the sub-GeV and multi-GeV neutrino induced events in underground detectors.

show abstract

Section: Primary Cosmic Ray Spectrum and Compositionsupporting

confidence: 77%

Section: Primary Cosmic Ray Spectrum and Compositionmentioning

confidence: 99%

See 1 more Smart Citation

Atmospheric neutrino flux supported by recent muon experiments

2001

View full text Add to dashboard Cite

show abstract

“…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: 65%

Theory Predictions for Inclusive atmospheric Neutrino flux

Honda

2013

EPJ Web of Conferences

View full text Add to dashboard Cite

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

show abstract

“…2. Data from the magnetic spectrometers BESS98 (Sanuki, et al, 2000) and AMS (Alcarez et al, 2000a) are indistinguishable on the plot for protons, although they differ somewhat for helium ( Alcarez et al, 2000b). Data from the CAPRICE spectrometer (Boezio et al, 1999) are 15-20% lower than BESS98 above 10 GeV/nucleon.…”

Section: Atmospheric Secondariesmentioning

confidence: 86%

Outstanding Problems in Particle Astrophysics

Gaisser

NATO Science Series

View full text Add to dashboard Cite

The general features of the cosmic-ray spectrum have been known for a long time. Although the basic approaches to understanding cosmic-ray propagation and acceleration have also been well understood for many years, there are several questions of great interest that motivate the current intense experimental activity in the field. If the energy-dependence of the secondary to primary ratio of galactic cosmic rays is as steep as observed, why is the flux of PeV particles so nearly isotropic? Can all antiprotons and positrons be explained as secondaries or is there some contribution from exotic sources? What is the maximum energy of cosmic accelerators? Is the "knee" of the cosmic-ray spectrum an effect of propagation or does it perhaps reflect the upper limit of galactic acceleration processes? Are gamma-ray burst sources (GRBs) and/or active galactic nuclei (AGN) accelerators of ultra-high-energy cosmic rays (UHECR) as well as sources of high-energy photons? Are GRBs and/or AGNs also sources of high-energy neutrinos? If there are indeed particles with energies greater than the cutoff expected from propagation through the microwave background radiation, what are their sources? The purpose of this lecture is to introduce the main topics of the School and to relate the theoretical questions to the experiments that can answer them.

show abstract

Cosmic protons

Cited by 273 publications

References 11 publications

Atmospheric neutrino flux supported by recent muon experiments

Atmospheric neutrino flux supported by recent muon experiments

Theory Predictions for Inclusive atmospheric Neutrino flux

Outstanding Problems in Particle Astrophysics

Contact Info

Product

Resources

About