Protons in near earth orbit

Alcaraz, J.; Alvisi, D.; 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.; Bruni, G.; Buénerd, M.; Burger, J. D.; Burger, W. J.; Cai, Xudong; Cavalletti, R.; Camps, C.; Cannarsa, Piermarco; Capell, M.; Casadei, D.; Casaus, J.; Castellini, G.; Chang, Y. H.; Chen, H.F.; Chen, H.S.; Chen, Z.G.; Chernoplekov, N. A.; Chiarini, A.; Chiueh, Tzihong; Chuang, Yao-Li; Cindolo, F.; Commichau, V.; Contin, A.; Ramusino, A. Cotta; 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; Feng, CF; Fiandrini, E.; Finelli, Francesco; Fisher, P. H.; Flaminio, R.; Fluegge, G.; Fouque, N.; Galaktionov, Yu.; Gervasi, M.; Giusti, P.; Grandi, D.; 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.; Laborie, G.; Laitinen, Timo; Lamanna, G.; Laurenti, G.; Lebedev, A.; Lee, S.C.; Levi, G.; Levtchenko, P.; Liu, C.L.; Liu, H.T.; Lolli, M.; Lopes, I.; Lu, Gangcheng; Lu, Yao; Lübelsmeyer, K.; Luckey, D.; Lustermann, W.; Mañá, C.; Margotti, A.; Massera, F.; Mayet, F.; McNeil, R. R.; Meillon, Brigitte; Menichelli, M.; Mezzanotte, F.; Mezzenga, R.; Mihul, A.; Molinari, G.; Mourão, A.; Mujunen, Ari; Palmonari, F.; Pancaldi, Giuliano; Papi, Alberto; Park, I.H.; Pauluzzi, M.; Pauß, F.; Perrin, E.; Pesci, A.; Pevsner, A.; Pilastrini, R.; Pimenta, M.; Plyaskin, V.; Pojidaev, V.; Postema, H.; Postolache, V.; Prati, E.; Produit, N.; Rancoita, P. G.; Rapin, D.; Raupach, F.; Recupero, Santi Maria; Ren, D.; Ren, Zhiyuan; Ribordy, M.; Richeux, J.P.; Riihonen, E.; Ritakari, Jouko; Roeser, U.; Roissin, C.; Sagdeev, R. Z.; Santos, D.; Sartorelli, G.; Dratzig, A. Schultz von; Schwering, 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.; Torromeo, G.; 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.

doi:10.1016/s0370-2693(99)01427-6

Cited by 196 publications

(107 citation statements)

References 6 publications

Supporting

Mentioning

104

Contrasting

Order By: Relevance

“…At low energy, the subGC secondary spectral yield decreases rapidly from a maximum around the low energy limit of the spectrometer up to the GC energy, around 15 GeV/c for equatorial latitudes (electrons) where the high energy tail of the subGC component merges with the galactic CR spectrum above GC ( figure 1). Interestingly, the subGC lepton and proton distributions at low latitudes have strikingly similar shapes [2,3]. This indicates that the two populations could also have similar dynamical origins, providing a further motivation to investigate the lepton populations along the same lines as in I.…”

mentioning

confidence: 78%

“…After a period of latence, the field is regaining interest with the new generation of ambitious experimental projects. They should bring major improvements to the instrumental accuracy of the measurements and orders of magnitudes to the statistics of counting, with respect to previous experiments (see the references quoted in [2,3] for the current and historical context). Some new measurements of particle flux close to earth have been performed recently by the AMS experiment, providing a large sample of new data.…”

mentioning

confidence: 99%

“…The proton distributions measured below the earth geomagnetic cutoff (GC) by AMS [2] have been successfully interpreted recently in terms of interactions of the (proton) cosmic ray (CR) flux with the atmosphere [5]. This work is referred to as I in the following.…”

mentioning

confidence: 99%

See 2 more Smart Citations

Secondary electrons and positrons in near earth orbit

2001

View full text Add to dashboard Cite

The secondary e + and e − populations in near earth's orbit have been calculated by simulation. The results are in very good agreement with the recent AMS measurements. The e + over e − flux ratio for particles below the geomagnetic cutoff appears to be due to the geomagnetic East-West effect.The study of particle populations in the earth environment has been a field of intense research activity for more than 50 years [1]. After a period of latence, the field is regaining interest with the new generation of ambitious experimental projects. They should bring major improvements to the instrumental accuracy of the measurements and orders of magnitudes to the statistics of counting, with respect to previous experiments (see the references quoted in [2,3] for the current and historical context). Some new measurements of particle flux close to earth have been performed recently by the AMS experiment, providing a large sample of new data. These measurements open new prospects for high precision studies of the cosmic ray (CR)-atmosphere interactions and the dynamics of particles in the magnetosphere. This is of particular importance for the atmospheric neutrino issue, in the current context of this research field, since the knowledge of the (electron and muon) neutrino flux produced in the same decay chain of pions in the atmosphere is necessary for interpreting the results of the underground neutrino experiments [4]. Consequently, a good understanding of the electron and positron flux is highly relevant.The proton distributions measured below the earth geomagnetic cutoff (GC) by AMS [2] have been successfully interpreted recently in terms of interactions of the (proton) cosmic ray (CR) flux with the atmosphere [5]. This work is referred to as I in the following. Extending the work reported in I on protons, the present paper addresses the interpretation of the flux of positrons and electrons measured by AMS below the cutoff (subGC) [3] in the same phenomenological framework.The lepton distributions observed by AMS showed a few remarkable features, of which the main two follow. First, the kinetic energy spectra have a strong subGC (then secondary) component (figure 1), similar to those observed in the proton flux. Second, the ratio of the e + over e − flux is large in the equatorial region (≈ 4) and decreasing towards higher latitudes (≈ 1). The measured spectra extended from the kinetic energy threshold of the spectrometer at ≈0.15 GeV, up to about 30 GeV for e − and 3 GeV for e + . At low energy, the subGC secondary spectral yield decreases rapidly from a maximum around the low energy limit of the spectrometer up to the GC energy, around 15 GeV/c for equatorial latitudes (electrons) where 1

show abstract

mentioning

confidence: 78%

mentioning

confidence: 99%

See 1 more Smart Citation

Secondary electrons and positrons in near earth orbit

2001

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…We have simulated the induced γ−ray yield according to standard treatments (see, e.g., [18,19]) and as implemented in the Galprop software package [13]. We assume that the p and He cosmic ray fluxes in the Galaxy have the same energy spectra and relative normalization as those measured in the local neighborhood [20,21], and that the He fraction of the interstellar gas is 7%. We write the background flux, splitting it into two factors:…”

Section: The Background Componentmentioning

confidence: 99%

The Galactic center as a dark matter gamma-ray source

Cesarini¹

2004

Astroparticle Physics

View full text Add to dashboard Cite

The EGRET telescope has identified a gamma-ray source at the Galactic center. We point out here that the spectral features of this source are compatible with the gamma-ray flux induced by pair annihilations of dark matter weakly interacting massive particles (WIMPs). We show that the discrimination between this interpretation and other viable explanations will be possible with GLAST, the next major gamma-ray telescope in space, on the basis of both the spectral and the angular signature of the WIMP-induced component. If, on the other hand, the data will point to an alternative explanation, we prove that there will still be the possibility for GLAST to single out a weaker dark matter source at the Galactic center. The potential of GLAST has been explored both in the context of a generic simplified toy-model for WIMP dark matter, and in a more specific setup, the case of dark matter neutralinos in the minimal supergravity framework. In the latter, we find that even in the case of moderate dark matter densities in the Galactic center region, there are portions of the parameter space which will be probed by GLAST.

show abstract

Protons in near earth orbit

Cited by 196 publications

References 6 publications

Secondary electrons and positrons in near earth orbit

Secondary electrons and positrons in near earth orbit

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

The Galactic center as a dark matter gamma-ray source

Contact Info

Product

Resources

About