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1. Transport parameters from AMS-02 F/Si data and fluorine source abundance

Author: Bueno, E. Ferronato, Derome, L., Génolini, Y., Maurin, D., Tatischeff, V., and Vecchi, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The AMS-02 collaboration recently released cosmic-ray F/Si data of unprecedented accuracy. Cosmic-ray (CR) fluorine is predominantly produced by fragmentation of heavier progenitors, while silicon is mostly accelerated at source. This ratio is thus maximally sensitive to CR propagation. We study the compatibility of the transport parameters derived from the F/Si ratio with those obtained from the lighter (Li,Be,B)/C ratios. We also inspect the CR source abundance of F, one of the few elements with a high first ionisation potential but only moderately volatile, and a potentially key element to study the acceleration mechanism of CRs. We use the 1D diffusion model implemented in the USINE code and perform $\chi^2$ analyses accounting for several systematic effects (energy correlations in data, nuclear cross sections and solar modulation uncertainties). We also take advantage of the EXFOR nuclear database to update the F production cross sections for its most important progenitors (identified to be 56Fe, 32S, 28Si, 27Al, 24Mg, 22Ne, and 20Ne). The transport parameters obtained from AMS-02 F/Si data are compatible with those obtained from AMS-02 (Li,Be,B)/C data. The combined fit of all these ratios leads to a chi2/dof$\approx 1.1$, with $\lesssim 10\%$ adjustments of the B and F production cross sections (the latter are based on very few nuclear data points, and would strongly benefit from new measurements). The F/Si ratio is compatible with a pure secondary origin of F, with a best-fit relative source abundance (19F/28Si)$\sim 10^{-3}$ and an upper limit of $\sim 5\times 10^{-3}$. Unfortunately, this limit is not sufficient to test global acceleration models of CR nuclei, for which values at the level of $\sim 10^{-4}$ are required. Such levels could be attained with F/Si data of a few percent accuracy at a few tens of TV, possibly within reach of the next generation of CR experiments., Comment: 18 pages, 14 figures, 4 tables (1 new): more re-organisation (for referees), but results and conclusions still unchanged (matching accepted A&A version)
Published: 2022
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2. A simple determination of the halo size $L$ from $^{10}$Be/$^9$Be data

Author: Maurin, D., Bueno, E. Ferronato, and Derome, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The AMS-02 and HELIX experiments should soon provide $\mathrm{^{10}Be/^9Be}$ cosmic-ray data of unprecedented precision. We propose an analytical formula to quickly and accurately determine $L$ from these data. Our formula is validated against the full calculation performed with the propagation code \usine{}. We compare the constraints on $L$ set by Be/B and $\mathrm{^{10}Be/^9Be}$, relying on updated sets of production cross-sections. The best-fit $L$ from AMS-02 Be/B data is shifted from 5 kpc to 3.8 kpc when using the updated cross-sections. We obtained consistent results from the Be/B analysis with USINE, $L=3.8^{+2.8}_{-1.6}$ kpc (data and cross-section uncertainties), and from the analysis of $\mathrm{^{10}Be/^9Be}$ data with the simplified formula, $L=4.7\pm0.6$ (data uncertainties) $\pm2$ (cross-section uncertainties) kpc. The analytical formula indicates that improvements on $L$ thanks to future data will be limited by production cross-section uncertainties, unless either $\mathrm{^{10}Be/^9Be}$ measurements are extended up to several tens of GeV/n, or nuclear data for the production of $\mathrm{^{10}Be}$ and $\mathrm{^9Be}$ are improved; new data for the production cross-section of $\mathrm{^{16}O}$ into Be isotopes above a few GeV/n are especially desired., Comment: 9 pages, 2 tables, 5 figures (matches accepted A&A version): comparison to [De21] moved to appendix (also highlight impact of reacceleration)
Published: 2022
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3. The rigidity dependence of galactic cosmic-ray fluxes and its connection with the diffusion coefficient

Author: Vecchi, M., Batista, P. -I., Bueno, E. F., Derome, L., Génolini, Y., and Maurin, D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Thanks to tremendous experimental efforts, galactic cosmic-ray fluxes are being measured up to the unprecedented per cent precision level. The logarithmic slope of these fluxes is a crucial quantity that promises us information on the diffusion properties and the primary or secondary nature of the different species. However, these measured slopes are sometimes interpreted in the pure diffusive regime, guiding to misleading conclusions. In this paper, we have studied the propagation of galactic cosmic rays by computing the fluxes of species between H and Fe using the USINE code and considering all the relevant physical processes and an updated set of cross-section data. We show that the slope of the well-studied secondary-to-primary B/C ratio is distinctly different from the diffusion coefficient slope, by an offset of about 0.2 in the rigidity range in which the AMS-02 data reach their best precision (several tens of GV). Furthermore, we have demonstrated that none of the species from H to Fe follows the expectations of the pure-diffusive regime. We argue that these differences arise from propagation processes such as fragmentation, convection, and reacceleration, which cannot be neglected. On this basis, we also provide predictions for the spectral slope of elemental fluxes not yet analysed by the AMS collaboration., Comment: accepted for publication on Frontiers in Physics (High-Energy and Astroparticle Physics)
Published: 2022
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4. The importance of Fe fragmentation for LiBeB analyses: Is a Li primary source needed to explain AMS-02 data?

Author: Maurin, D., Bueno, E. Ferronato, Génolini, Y., Derome, L., and Vecchi, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Nuclear Experiment
Abstract: High-precision data from AMS-02 on Li, Be, and B provide the best constraints on Galactic cosmic-ray transport parameters. We re-evaluate the impact of Fe fragmentation on the Li, Be, and B modelling. We discuss the consequences on the transport parameter determination and reassess whether a primary source of Li is needed to match AMS-02 data. We renormalised several cross-section parametrisations to existing data for the most important reactions producing Li, Be, and B. We used the USINE code with these new cross-section sets to re-analyse Li/C, Be/C, and B/C AMS-02 data. We built three equally plausible cross-section sets. Compared to the initial cross-section sets, they lead to an average enhanced production of Li ($\sim20-50\%$) and Be ($\sim5-15\%$), while leaving the B flux mostly unchanged. In particular, Fe fragmentation is found to contribute to up to 10\% of the Li and Be fluxes. Used in the combined analysis of AMS-02 Li/C, Be/C, and B/C data, the fit is significantly improved, with an enhanced diffusion coefficient ($\sim 20\%)$. The three updated cross-section sets are found to either slightly undershoot or overshoot the Li/C and B/C ratios: this strongly disfavours evidence for a primary source of Li in cosmic rays. We stress that isotopic cosmic-ray ratios of Li (and to a lesser extent Be), soon to be released by AMS-02, are also impacted by the use of these updated sets. Almost no nuclear data exist for the production of Li and B isotopes from Ne, Mg, Si, and Fe, whereas these reactions are estimated to account for $\sim 20\%$ of the total production. New nuclear measurements would be appreciated and help to better exploit the high-precision AMS-02 cosmic-ray data., Comment: 20 pages, 16 figures, 2 tables (matches accepted A&A version): corrected sign for $\delta_l$ (typo in plotting script) + couple of sentences added (XS modelling, results for various propagation configurations)
Published: 2022
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5. The cosmic ray energetics and mass for the international space station (ISS-CREAM) instrument

Author: Yoon, Y.S., Amare, Y., Angelaszek, D., Anthony, N., Cheryian, K., Choi, G.H., Copley, M., Coutu, S., Derome, L., Eraud, L., Hagenau, L., Han, J.H., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kang, S.C., Kim, H.J., Kim, K.C., Kim, M.H., Lee, H.Y., Lee, J., Lee, M.H., Liang, J., Lu, L., Lutz, L., Menchaca-Rocha, A., Mitchell, J.W., Mognet, S.I., Morton, S., Nester, M., Nutter, S., Park, H., Park, I.H., Park, J.M., Picot-Clémente, N., Seo, E.S., Smith, J.R., Walpole, P., Weinmann, R.P., Wu, J., and Zhang, H.G.
Published: 2024
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6. Galactic halo size in the light of recent AMS-02 data

Author: Weinrich, N., Boudaud, M., Derome, L., Génolini, Y., Lavalle, J., Maurin, D., Salati, P., Serpico, P., and Weymann-Despres, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The vertical diffusive halo size of the Galaxy, $L$, is a key parameter for dark matter indirect searches. It can be better determined thanks to recent AMS-02 data. We set constraints on $L$ from Be/B and $^{10}$Be/Be data, and we performed a consistency check with positron data. We detail the dependence of Be/B and $^{10}$Be/Be on $L$ and forecast on which energy range better data would be helpful for future $L$ improvements. We used USINE v3.5 for the propagation of nuclei, and $e^+$ were calculated with the pinching method of Boudaud et al. (2017). The current AMS-02 Be/B ($\sim3\%$ precision) and ACE-CRIS $^{10}$Be/Be ($\sim 10\%$ precision) data bring similar and consistent constraints on $L$. The AMS-02 Be/B data alone constrain $L=5^{+3}_{-2}$~kpc at a 68\% confidence level (spanning different benchmark transport configurations), a range for which most models do not overproduce positrons. Future experiments need to deliver percent-level accuracy on $^{10}$Be/$^9$Be anywhere below 10 GV to further constrain $L$. Forthcoming AMS-02, HELIX, and PAMELA $^{10}$Be/$^9$Be results will further test and possibly tighten the limits derived here. Elemental ratios involving radioactive species with different lifetimes (e.g. Al/Mg and Cl/Ar) are also awaited to provide complementary and robuster constraints., Comment: 15 pages, 10 figures, 6 tables. Additional references and few clarifications (matches A&A accepted version)
Published: 2020
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7. Fitting B/C cosmic-ray data in the AMS-02 era: A cookbook

Author: Derome, L., Maurin, D., Salati, P., Boudaud, M., Génolini, Y., and Kunzé, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract: AMS-02 on the International Space Station has been releasing data of unprecedented accuracy. This poses new challenges for their interpretation. We refine the methodology to get a statistically sound determination of the cosmic-ray propagation parameters. We inspect the numerical precision of the model calculation, nuclear cross-section uncertainties, and energy correlations in data systematic errors. We used the 1D diffusion model in USINE. Our $\chi^2$ analysis includes a covariance matrix of errors for AMS-02 systematics and nuisance parameters to account for cross-section uncertainties. Mock data were used to validate some of our choices. We show that any mis-modelling of nuclear cross-section values or the energy correlation length of the covariance matrix of errors biases the analysis. It also makes good models ($\chi^2_{\rm min}/{\rm dof}\approx1$) appear as excluded ($\chi^2_{\rm min}/{\rm dof}\gg1$). We provide a framework to mitigate these effects (AMS-02 data are interpreted in a companion paper). New production cross-section data and the publication by the AMS-02 collaboration of a covariance matrix of errors for each data set would be an important step towards an unbiased view of cosmic-ray propagation in the Galaxy., Comment: 24 pages, 23 figures, 3 tables: affiliations corrected
Published: 2019
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8. Proton and Helium Spectra from the CREAM-III Flight

Author: Yoon, Y. S., Anderson, T., Barrau, A., Conklin, N. B., Coutu, S., Derome, L., Han, J. H., Jeon, J. A., Kim, K. C., Kim, M. H., Lee, H. Y., Lee, J., Lee, M. H., Lee, S. E., Link, J. T., Menchaca-Rocha, A., Mitchell, J. W., Mognet, S. I., Nutter, S., Park, I. H., Picot-Clemente, N., Putze, A., Seo, E. S., Smith, J., and Wu, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Primary cosmic-ray elemental spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass (CREAM) experiment since 2004. The third CREAM payload (CREAM-III) flew for 29 days during the 2007-2008 Antarctic season. Energies of incident particles above 1 TeV are measured with a calorimeter. Individual elements are clearly separated with a charge resolution of ~0.12 e (in charge units) and ~0.14 e for protons and helium nuclei, respectively, using two layers of silicon charge detectors. The measured proton and helium energy spectra at the top of the atmosphere are harder than other existing measurements at a few tens of GeV. The relative abundance of protons to helium nuclei is 9.53+-0.03 for the range of 1 TeV/n to 63 TeV/n. The ratio is considerably smaller than other measurements at a few tens of GeV/n. The spectra become softer above ~20 TeV. However, our statistical uncertainties are large at these energies and more data are needed.
Published: 2017
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9. Neutron monitors and muon detectors for solar modulation studies: 2. $\phi$ time series

Author: Ghelfi, A., Maurin, D., Cheminet, A., Derome, L., Hubert, G., and Melot, F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: The level of solar modulation at different times (related to the solar activity) is a central question of solar and galactic cosmic-ray physics. In the first paper of this series, we have established a correspondence between the uncertainties on ground-based detectors count rates and the parameter $\phi$ (modulation level in the force-field approximation) reconstructed from these count rates. In this second paper, we detail a procedure to obtain a reference $\phi$ time series from neutron monitor data. We show that we can have an unbiased and accurate $\phi$ reconstruction ($\Delta\phi/\phi\simeq 10\%$). We also discuss the potential of Bonner spheres spectrometers and muon detectors to provide $\phi$ time series. Two by-products of this calculation are updated $\phi$ values for the cosmic-ray database and a web interface to retrieve and plot $\phi$ from the 50's to today (\url{http://lpsc.in2p3.fr/crdb})., Comment: 15 pages, 5 figures, 2 tables. AdSR, in press. Web interface to get modulation parameter phi(t): new tab in http://lpsc.in2p3.fr/crdb
Published: 2016
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10. UCTM2: An updated User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics

Author: Bourrion, O., Boyer, B., Derome, L., and Pignol, G.
Subjects: Physics - Instrumentation and Detectors
Abstract: We developed a highly integrated and versatile electronic module to equip small nuclear physics experiments and lab teaching classes: the User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics (UCTM). It is configurable through a Graphical User Interface (GUI) and provides a large number of possible trigger conditions without any Hardware Description Language (HDL) required knowledge. This new version significantly enhances the previous capabilities by providing two additional features: signal digitization and time measurements. The design, performances and a typical application are presented., Comment: 14 pages, 9 figures. arXiv admin note: text overlap with arXiv:1110.2917
Published: 2016
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11. High precision particle astrophysics as a new window on the universe with an Antimatter Large Acceptance Detector In Orbit (ALADInO)

Author: Battiston, R., Bertucci, B., Adriani, O., Ambrosi, G., Baudouy, B., Blasi, P., Boezio, M., Campana, D., Derome, L., De Mitri, I., Di Felice, V., Donato, F., Duranti, M., Formato, V., Grasso, D., Gebauer, I., Iuppa, R., Masi, N., Maurin, D., Mazziotta, M. N., Musenich, R., Nozzoli, F., Papini, P., Picozza, P., Pearce, M., Pospíšil, S., Rossi, L., Tomassetti, N., Vagelli, V., and Wu, X.
Published: 2021
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12. The Alpha Magnetic Spectrometer (AMS) on the international space station: Part II — Results from the first seven years

Author: Aguilar, M., Ali Cavasonza, L., Ambrosi, G., Arruda, L., Attig, N., Barao, F., Barrin, L., Bartoloni, A., Başeğmez-du Pree, S., Bates, J., Battiston, R., Behlmann, M., Beischer, B., Berdugo, J., Bertucci, B., Bindi, V., de Boer, W., Bollweg, K., Borgia, B., Boschini, M.J., Bourquin, M., Bueno, E.F., Burger, J., Burger, W.J., Burmeister, S., Cai, X.D., Capell, M., Casaus, J., Castellini, G., Cervelli, F., Chang, Y.H., Chen, G.M., Chen, H.S., Chen, Y., Cheng, L., Chou, H.Y., Chouridou, S., Choutko, V., Chung, C.H., Clark, C., Coignet, G., Consolandi, C., Contin, A., Corti, C., Cui, Z., Dadzie, K., Dai, Y.M., Delgado, C., Della Torre, S., Demirköz, M.B., Derome, L., Di Falco, S., Di Felice, V., Díaz, C., Dimiccoli, F., von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Freeman, C., Galaktionov, Y., Gámez, C., García-López, R.J., Gargiulo, C., Gast, H., Gebauer, I., Gervasi, M., Giovacchini, F., Gómez-Coral, D.M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guo, K.H., Haino, S., Han, K.C., Hashmani, R.K., He, Z.H., Heber, B., Hsieh, T.H., Hu, J.Y., Huang, Z.C., Hungerford, W., Incagli, M., Jang, W.Y., Jia, Yi, Jinchi, H., Kanishev, K., Khiali, B., Kim, G.N., Kirn, Th., Konyushikhin, M., Kounina, O., Kounine, A., Koutsenko, V., Kuhlman, A., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., Lazzizzera, I., Lebedev, A., Lee, H.T., Lee, S.C., Leluc, C., Li, J.Q., Li, M., Li, Q., Li, S., Li, T.X., Li, Z.H., Light, C., Lin, C.H., Lippert, T., Liu, Z., Lu, S.Q., Lu, Y.S., Luebelsmeyer, K., Luo, J.Z., Lyu, S.S., Machate, F., Mañá, C., Marín, J., Marquardt, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Menchaca-Rocha, A., Meng, Q., Mo, D.C., Molero, M., Mott, P., Mussolin, L., Ni, J.Q., Nikonov, N., Nozzoli, F., Oliva, A., Orcinha, M., Palermo, M., Palmonari, F., Paniccia, M., Pashnin, A., Pauluzzi, M., Pensotti, S., Phan, H.D., Plyaskin, V., Pohl, M., Porter, S., Qi, X.M., Qin, X., Qu, Z.Y., Quadrani, L., Rancoita, P.G., Rapin, D., Reina Conde, A., Rosier-Lees, S., Rozhkov, A., Rozza, D., Sagdeev, R., Schael, S., Schmidt, S.M., Schulz von Dratzig, A., Schwering, G., Seo, E.S., Shan, B.S., Shi, J.Y., Siedenburg, T., Solano, C., Song, J.W., Sonnabend, R., Sun, Q., Sun, Z.T., Tacconi, M., Tang, X.W., Tang, Z.C., Tian, J., Ting, Samuel C.C., Ting, S.M., Tomassetti, N., Torsti, J., Tüysüz, C., Urban, T., Usoskin, I., Vagelli, V., Vainio, R., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J.P., Wang, L.Q., Wang, N.H., Wang, Q.L., Wang, S., Wang, X., Wang, Z.X., Wei, J., Weng, Z.L., Wu, H., Xiong, R.Q., Xu, W., Yan, Q., Yang, Y., Yi, H., Yu, Y.J., Yu, Z.Q., Zannoni, M., Zhang, C., Zhang, F., Zhang, F.Z., Zhang, J.H., Zhang, Z., Zhao, F., Zheng, Z.M., Zhuang, H.L., Zhukov, V., Zichichi, A., Zimmermann, N., and Zuccon, P.
Published: 2021
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13. Non-parametric determination of H and He interstellar fluxes from cosmic-ray data

Author: Ghelfi, A., Barao, F., Derome, L., and Maurin, D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract: Top-of-atmosphere (TOA) cosmic-ray (CR) fluxes from satellites and balloon-borne experiments are snapshots of the solar activity imprinted on the interstellar (IS) fluxes. Given a series of snapshots, the unknown IS flux shape and the level of modulation (for each snapshot) can be recovered. We wish (i) to provide the most accurate determination of the IS H and He fluxes from TOA data alone, (ii) to obtain the associated modulation levels (and uncertainties) while fully accounting for the correlations with the IS flux uncertainties, and (iii) to inspect whether the minimal force-field approximation is sufficient to explain all the data at hand. Using H and He TOA measurements, including the recent high-precision AMS, BESS-Polar, and PAMELA data, we performed a non-parametric fit of the IS fluxes $J^{\rm IS}_{\rm H,~He}$ and modulation level $\phi_i$ for each data-taking period. We relied on a Markov chain Monte Carlo (MCMC) engine to extract the probability density function and correlations (hence the credible intervals) of the sought parameters. Although H and He are the most abundant and best measured CR species, several datasets had to be excluded from the analysis because of inconsistencies with other measurements. From the subset of data passing our consistency cut, we provide ready-to-use best-fit and credible intervals for the H and He IS fluxes from MeV/n to PeV/n energy (with a relative precision in the range [2-10\%] at 1$\sigma$). Given the strong correlation between $J^{\rm IS}$ and $\phi_i$ parameters, the uncertainties on $J^{\rm IS}$ translate into $\Delta\phi\approx \pm 30$~MV (at 1$\sigma$) for all experiments. We also find that the presence of $^3$He in He data biases $\phi$ towards higher $\phi$ values by $\sim 30$~MV. The force-field approximation gives an excellent ($\chi^2/$dof$=1.02$) description of the recent high-precision TOA H and He fluxes., Comment: 10 pages, 5 figures, 3 tables (matches A&A accepted version) + Erratum for Eq. (8) and Table 3 (submitted to A&A)
Published: 2015
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14. Neutron monitors and muon detectors for solar modulation studies: Interstellar flux, yield function, and assessment of critical parameters in count rate calculations

Author: Maurin, D., Cheminet, A., Derome, L., Ghelfi, A., and Hubert, G
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract: Particles count rates at given Earth location and altitude result from the convolution of (i) the interstellar (IS) cosmic-ray fluxes outside the solar cavity, (ii) the time-dependent modulation of IS into Top-of-Atmosphere (TOA) fluxes, (iii) the rigidity cut-off (or geomagnetic transmission function) and grammage at the counter location, (iv) the atmosphere response to incoming TOA cosmic rays (shower development), and (v) the counter response to the various particles/energies in the shower. Count rates from neutron monitors or muon counters are therefore a proxy to solar activity. In this paper, we review all ingredients, discuss how their uncertainties impact count rate calculations, and how they translate into variation/uncertainties on the level of solar modulation $\varphi$ (in the simple Force-Field approximation). The main uncertainty for neutron monitors is related to the yield function. However, many other effects have a significant impact, at the 5-10\% level on $\varphi$ values. We find no clear ranking of the dominant effects, as some depend on the station position and/or the weather and/or the season. An abacus to translate any variation of count rates (for neutron and $\mu$ detectors) to a variation of the solar modulation $\varphi$ is provided., Comment: 28 pages, 16 figures, 9 tables, match accepted version in AdSR (minor corrections, Dorman (1974,2004,2009) reference textbooks added)
Published: 2014
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15. On-orbit performance of the top and bottom counting detectors for the ISS-CREAM experiment on the international space station

Author: Kang, S.C., Amare, Y., Anderson, T., Angelaszek, D., Anthony, N., Cheryian, K., Choi, G.H., Copley, M., Coutu, S., Derome, L., Eraud, L., Hagenau, L., Han, J.H., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kim, H.J., Kim, K.C., Kim, M.H., Lee, H.Y., Lee, J., Lee, M.H., Liang, J., Link, J.T., Lu, L., Lundquist, J.P., Lutz, L., Menchaca-Rocha, A., Mernik, T., Mitchell, J.W., Mognet, S.I., Morton, S., Nester, M., Nutter, S., Ofoha, O., Park, H., Park, I.H., Park, J.M., Picot-Clemente, N., Quinn, R., Seo, E.S., Smith, J.R., Takeishi, R., Walpole, P., Weinmann, R.P., Wu, J., and Yoon, Y.S.
Published: 2019
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16. Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer

Author: Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Bagwell, C, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Belyaev, N, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Bolster, J, Borchiellini, M, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Dass, A, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Faldi, F, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guracho, A, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Huang, B, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Karagöz, G, Khiali, B, Kim, G, Kirn, T, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lavecchia, G, Lazzizzera, I, Lee, H, Lee, S, Li, H, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Liang, M, Lin, C, Lippert, T, Liu, J, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, S, Luo, X, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Ocampo-Peleteiro, J, Oliva, A, Orcinha, M, Ottupara, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Romaneehsen, L, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schultz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Siedenburg, T, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Tian, Y, Ting, S, Tomassetti, N, Torsti, J, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Wu, Y, Xiao, J, Xiong, R, Xiong, X, Xu, W, Yan, Q, Yang, H, Yang, Y, Yashin, I, Yelland, A, Yi, H, You, Y, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Aguilar, M., Ali Cavasonza, L., Alpat, B., Ambrosi, G., Arruda, L., Attig, N., Bagwell, C., Barao, F., Barrin, L., Bartoloni, A., Başeğmez-du Pree, S., Battiston, R., Belyaev, N., Berdugo, J., Bertucci, B., Bindi, V., Bollweg, K., Bolster, J., Borchiellini, M., Borgia, B., Boschini, M. J., Bourquin, M., Bueno, E. F., Burger, J., Burger, W. J., Cai, X. D., Capell, M., Casaus, J., Castellini, G., Cervelli, F., Chang, Y. H., Chen, G. M., Chen, G. R., Chen, H., Chen, H. S., Chen, Y., Cheng, L., Chou, H. Y., Chouridou, S., Choutko, V., Chung, C. H., Clark, C., Coignet, G., Consolandi, C., Contin, A., Corti, C., Cui, Z., Dadzie, K., Dass, A., Delgado, C., Della Torre, S., Demirköz, M. B., Derome, L., Di Falco, S., Di Felice, V., Díaz, C., Dimiccoli, F., von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Faldi, F., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Gámez, C., García-López, R. J., Gargiulo, C., Gast, H., Gervasi, M., Giovacchini, F., Gómez-Coral, D. M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guracho, A. N., Haino, S., Han, K. C., Hashmani, R. K., He, Z. H., Heber, B., Hsieh, T. H., Hu, J. Y., Huang, B. W., Incagli, M., Jang, W. Y., Jia, Yi, Jinchi, H., Karagöz, G., Khiali, B., Kim, G. N., Kirn, Th., Kounina, O., Kounine, A., Koutsenko, V., Krasnopevtsev, D., Kuhlman, A., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., LaVecchia, G., Lazzizzera, I., Lee, H. T., Lee, S. C., Li, H. L., Li, J. Q., Li, M., Li, Q., Li, Q. Y., Li, S., Li, S. L., Li, J. H., Li, Z. H., Liang, J., Liang, M. J., Lin, C. H., Lippert, T., Liu, J. H., Lu, S. Q., Lu, Y. S., Luebelsmeyer, K., Luo, J. Z., Luo, S. D., Luo, Xi, Machate, F., Mañá, C., Marín, J., Marquardt, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Medvedeva, T., Menchaca-Rocha, A., Meng, Q., Mikhailov, V. V., Molero, M., Mott, P., Mussolin, L., Negrete, J., Nikonov, N., Nozzoli, F., Ocampo-Peleteiro, J., Oliva, A., Orcinha, M., Ottupara, M. A., Palermo, M., Palmonari, F., Paniccia, M., Pashnin, A., Pauluzzi, M., Pensotti, S., Plyaskin, V., Poluianov, S., Qin, X., Qu, Z. Y., Quadrani, L., Rancoita, P. G., Rapin, D., Reina Conde, A., Robyn, E., Romaneehsen, L., Rozhkov, A., Rozza, D., Sagdeev, R., Schael, S., Schultz von Dratzig, A., Schwering, G., Seo, E. S., Shan, B. S., Siedenburg, T., Song, J. W., Song, X. J., Sonnabend, R., Strigari, L., Su, T., Sun, Q., Sun, Z. T., Tacconi, M., Tang, X. W., Tang, Z. C., Tian, J., Tian, Y., Ting, Samuel C. C., Ting, S. M., Tomassetti, N., Torsti, J., Urban, T., Usoskin, I., Vagelli, V., Vainio, R., Valencia-Otero, M., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J. P., Wang, C. X., Wang, L., Wang, L. Q., Wang, N. H., Wang, Q. L., Wang, S., Wang, X., Wang, Yu, Wang, Z. M., Wei, J., Weng, Z. L., Wu, H., Wu, Y., Xiao, J. N., Xiong, R. Q., Xiong, X. Z., Xu, W., Yan, Q., Yang, H. T., Yang, Y., Yashin, I. I., Yelland, A., Yi, H., You, Y. H., Yu, Y. M., Yu, Z. Q., Zannoni, M., Zhang, C., Zhang, F., Zhang, F. Z., Zhang, J., Zhang, J. H., Zhang, Z., Zhao, F., Zheng, C., Zheng, Z. M., Zhuang, H. L., Zhukov, V., Zichichi, A., Zuccon, P., Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Bagwell, C, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Belyaev, N, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Bolster, J, Borchiellini, M, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Dass, A, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Faldi, F, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guracho, A, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Huang, B, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Karagöz, G, Khiali, B, Kim, G, Kirn, T, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lavecchia, G, Lazzizzera, I, Lee, H, Lee, S, Li, H, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Liang, M, Lin, C, Lippert, T, Liu, J, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, S, Luo, X, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Ocampo-Peleteiro, J, Oliva, A, Orcinha, M, Ottupara, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Romaneehsen, L, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schultz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Siedenburg, T, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Tian, Y, Ting, S, Tomassetti, N, Torsti, J, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Wu, Y, Xiao, J, Xiong, R, Xiong, X, Xu, W, Yan, Q, Yang, H, Yang, Y, Yashin, I, Yelland, A, Yi, H, You, Y, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Aguilar, M., Ali Cavasonza, L., Alpat, B., Ambrosi, G., Arruda, L., Attig, N., Bagwell, C., Barao, F., Barrin, L., Bartoloni, A., Başeğmez-du Pree, S., Battiston, R., Belyaev, N., Berdugo, J., Bertucci, B., Bindi, V., Bollweg, K., Bolster, J., Borchiellini, M., Borgia, B., Boschini, M. J., Bourquin, M., Bueno, E. F., Burger, J., Burger, W. J., Cai, X. D., Capell, M., Casaus, J., Castellini, G., Cervelli, F., Chang, Y. H., Chen, G. M., Chen, G. R., Chen, H., Chen, H. S., Chen, Y., Cheng, L., Chou, H. Y., Chouridou, S., Choutko, V., Chung, C. H., Clark, C., Coignet, G., Consolandi, C., Contin, A., Corti, C., Cui, Z., Dadzie, K., Dass, A., Delgado, C., Della Torre, S., Demirköz, M. B., Derome, L., Di Falco, S., Di Felice, V., Díaz, C., Dimiccoli, F., von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Faldi, F., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Gámez, C., García-López, R. J., Gargiulo, C., Gast, H., Gervasi, M., Giovacchini, F., Gómez-Coral, D. M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guracho, A. N., Haino, S., Han, K. C., Hashmani, R. K., He, Z. H., Heber, B., Hsieh, T. H., Hu, J. Y., Huang, B. W., Incagli, M., Jang, W. Y., Jia, Yi, Jinchi, H., Karagöz, G., Khiali, B., Kim, G. N., Kirn, Th., Kounina, O., Kounine, A., Koutsenko, V., Krasnopevtsev, D., Kuhlman, A., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., LaVecchia, G., Lazzizzera, I., Lee, H. T., Lee, S. C., Li, H. L., Li, J. Q., Li, M., Li, Q., Li, Q. Y., Li, S., Li, S. L., Li, J. H., Li, Z. H., Liang, J., Liang, M. J., Lin, C. H., Lippert, T., Liu, J. H., Lu, S. Q., Lu, Y. S., Luebelsmeyer, K., Luo, J. Z., Luo, S. D., Luo, Xi, Machate, F., Mañá, C., Marín, J., Marquardt, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Medvedeva, T., Menchaca-Rocha, A., Meng, Q., Mikhailov, V. V., Molero, M., Mott, P., Mussolin, L., Negrete, J., Nikonov, N., Nozzoli, F., Ocampo-Peleteiro, J., Oliva, A., Orcinha, M., Ottupara, M. A., Palermo, M., Palmonari, F., Paniccia, M., Pashnin, A., Pauluzzi, M., Pensotti, S., Plyaskin, V., Poluianov, S., Qin, X., Qu, Z. Y., Quadrani, L., Rancoita, P. G., Rapin, D., Reina Conde, A., Robyn, E., Romaneehsen, L., Rozhkov, A., Rozza, D., Sagdeev, R., Schael, S., Schultz von Dratzig, A., Schwering, G., Seo, E. S., Shan, B. S., Siedenburg, T., Song, J. W., Song, X. J., Sonnabend, R., Strigari, L., Su, T., Sun, Q., Sun, Z. T., Tacconi, M., Tang, X. W., Tang, Z. C., Tian, J., Tian, Y., Ting, Samuel C. C., Ting, S. M., Tomassetti, N., Torsti, J., Urban, T., Usoskin, I., Vagelli, V., Vainio, R., Valencia-Otero, M., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J. P., Wang, C. X., Wang, L., Wang, L. Q., Wang, N. H., Wang, Q. L., Wang, S., Wang, X., Wang, Yu, Wang, Z. M., Wei, J., Weng, Z. L., Wu, H., Wu, Y., Xiao, J. N., Xiong, R. Q., Xiong, X. Z., Xu, W., Yan, Q., Yang, H. T., Yang, Y., Yashin, I. I., Yelland, A., Yi, H., You, Y. H., Yu, Y. M., Yu, Z. Q., Zannoni, M., Zhang, C., Zhang, F., Zhang, F. Z., Zhang, J., Zhang, J. H., Zhang, Z., Zhao, F., Zheng, C., Zheng, Z. M., Zhuang, H. L., Zhukov, V., Zichichi, A., and Zuccon, P.
Abstract: We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38×106 sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167±0.006, for Ne/Si is 0.833±0.025, for Mg/Si is 0.994±0.029, and for C/O is 0.836±0.025. These values are determined independent of cosmic-ray propagation.
Published: 2023

17. The ISS-CREAM Silicon Charge Detector for identification of the charge of cosmic rays up to Z = 26: Design, fabrication and ground-test performance

Author: Lee, J., Amare, Y., Anderson, T., Angelaszek, D., Anthony, N., Cheryian, K., Choi, G.H., Copley, M., Coutu, S., Derome, L., Eraud, L., Hagenau, L., Han, J.H., Hong, G., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kang, S.C., Kim, H.J., Kim, K.C., Kim, M.H., Lee, H.Y., Lee, M.H., Liang, J., Link, J.T., Lu, L., Lutz, L., Menchaca-Rocha, A., Mernik, T., Mitchell, J.W., Mognet, S.I., Morton, S., Nester, M., Nutter, S., Ofoha, O., Park, H., Park, I.H., Park, J.M., Picot-Clemente, N., Quinn, R., Seo, E.S., Smith, J.R., Walpole, P., Weinmann, R.P., Wu, J., and Yoon, Y.S.
Published: 2019
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18. The boronated scintillator detector of the ISS-CREAM experiment

Author: Amare, Y., Anderson, T., Angelaszek, D., Anthony, N., Cheryian, K., Choi, G.H., Copley, M., Coutu, S., Derome, L., Eraud, L., Hagenau, L., Han, J.H., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kang, S.C., Kim, H.J., Kim, K.C., Kim, M.H., Lee, H.Y., Lee, J., Lee, M.H., Liang, J., Link, J.T., Lu, L., Lutz, L., Menchaca-Rocha, A., Mernik, T., Mitchell, J.W., Mognet, S.I., Morton, S., Nester, M., Nutter, S., Ofoha, O., Park, H., Park, I.H., Park, J.M., Picot-Clémente, N., Quinn, R., Seo, E.S., Smith, J.R., Walpole, P., Weinmann, R.P., Wu, J., and Yoon, Y.S.
Published: 2019
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19. Measurement of delayed fluorescence in plastic scintillator from 1 to 10 [formula omitted]

Author: Nutter, S., Amare, Y., Anderson, T., Angelaszek, D., Anthony, N., Cheryian, k., Choi, G.H., Copley, M., Coutu, S., Derome, L., Eraud, L., Hagenau, L., Han, J.H., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kang, S.C., Kim, H.J., Kim, K.C., Kim, M.H., Lee, H.Y., Lee, J., Lee, M.H., Liang, J., Link, J.T., Lu, L., Lutz, L., Menchaca-Rocha, A., Mernik, T., Mitchell, J.W., Mognet, S.I., Morton, S., Nester, M., Ofoha, O., Park, H., Park, I.H., Park, J.M., Picot-Clémente, N., Quinn, R., Seo, E.S., Smith, J.R., Walpole, P., Weinmann, R.P., Wu, J., and Yoon, Y.S.
Published: 2019
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20. UCTM: A User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics

Author: Bourrion, O., Boyer, B., and Derome, L.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Physics Education, Physics - Instrumentation and Detectors
Abstract: A configurable trigger scaler and delay NIM module has been designed to equip nuclear physics experiments and lab teaching classes. It is configurable through a Graphical User Interface (GUI) and provides a large number of possible trigger conditions without any Hardware Description Language (HDL) required knowledge. The design, performances and typical applications are presented., Comment: 11 pages, 10 figures
Published: 2011
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21. Constraining Galactic cosmic-ray parameters with Z<=2 nuclei

Author: Coste, B., Derome, L., Maurin, D., and Putze, A.
Subjects: Astrophysics - Galaxy Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The secondary-to-primary B/C ratio is widely used to study Galactic cosmic-ray propagation processes. The 2H/4He and 3He/4He ratios probe a different Z/A regime, therefore testing the `universality' of propagation. We revisit the constraints on diffusion-model parameters set by the quartet (1H, 2H, 3He, 4He), using the most recent data as well as updated formulae for the inelastic and production cross-sections. The analysis relies on the USINE propagation package and a Markov Chain Monte Carlo technique to estimate the probability density functions of the parameters. Simulated data are also used to validate analysis strategies. The fragmentation of CNO cosmic rays (resp. NeMgSiFe) on the ISM during their propagation contributes to 20% (resp. 20%) of the 2H and 15% (resp. 10%) of the 3He flux at high energy. The C to Fe elements are also responsible for up to 10% of the 4He flux measured at 1 GeV/n. The analysis of 3He/4He (and to a less extent 2H/4He) data shows that the transport parameters are consistent with those from the B/C analysis: the diffusion model with delta~0.7 (diffusion slope), Vc~20 km/s (galactic wind), Va~40 km/s (reacceleration) is favoured, but the combination delta~0.2, Vc~0, and Va~80 km/s is a close second. The confidence intervals on the parameters show that the constraints set by the quartet data are competitive with those brought by the B/C data. These constraints are tighter when adding the 3He (or 2H) flux measurements, and the tightest when further adding the He flux. For the latter, the analysis of simulated and real data show an increased sensitivity to biases. Using secondary-to-primary ratio along with a loose prior on the source parameters is recommended to get the most robust constraints on the transport parameters., Comment: 17 pages, 7 tables, 20 figures (submitted to A&A)
Published: 2011
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22. Design and construction of a Cherenkov imager for charge measurement of nuclear cosmic rays

Author: Bourrion, O., Bernard, Ch., Bondoux, D., Bouly, J. L., Bouvier, J., Boyer, B., Brinet, M., Buenerd, M., Damieux, G., Derome, L., Eraud, L., Foglio, R., Fombaron, D., Grondin, D., Lee, M. H., Lutz, L., Marton, M., Menchaca-Rocha, A., Pelissier, A., Périé, J. N., Putze, A., Roudier, S., Sallaz-Damaz, Y., Seo, E. S., Scordilis, J. P., and Yoon, Y. S.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: A proximity focusing Cherenkov imager called CHERCAM, has been built for the charge measurement of nuclear cosmic rays with the CREAM instrument. It consists of a silica aerogel radiator plane across from a detector plane equipped with 1,600 1" diameter photomultipliers. The two planes are separated by a ring expansion gap. The Cherenkov light yield is proportional to the charge squared of the incident particle. The expected relative light collection accuracy is in the few percents range. It leads to an expected single element separation over the range of nuclear charge Z of main interest 1 < Z < 26. CHERCAM is designed to fly with the CREAM balloon experiment. The design of the instrument and the implemented technical solutions allowing its safe operation in high altitude conditions (radiations, low pressure, cold) are presented., Comment: 24 pages, 19 figures
Published: 2011
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23. A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays: II. Results for the diffusion model combining B/C and radioactive nuclei

Author: Putze, A., Derome, L., and Maurin, D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: On-going measurements of the cosmic radiation (nuclear, electronic, and gamma-ray) are shedding new light on cosmic-ray physics. A comprehensive picture of these data relies on an accurate determination of the transport and source parameters of propagation models. A Markov Chain Monte Carlo is used to obtain these parameters in a diffusion model. From the measurement of the B/C ratio and radioactive cosmic-ray clocks, we calculate their probability density functions, with a special emphasis on the halo size L of the Galaxy and the local underdense bubble of size r_h. The analysis relies on the USINE code for propagation and on a Markov Chain Monte Carlo technique (Putze et al. 2009, paper I of this series) for the parameter determination. As found in previous studies, the B/C best-fit model favours diffusion/convection/reacceleration (Model III) over diffusion/reacceleration (Model II). A combined fit on B/C and the isotopic ratios (10Be/9Be, 26Al/27Al, 36Cl/Cl) leads to L ~ 8 kpc and r_h ~ 120 pc for the best-fit Model III. This value for r_h is consistent with direct measurements of the local interstallar medium. For Model II, L ~ 4 kpc and r_h is consistent with zero. We showed the potential and usefulness of the Markov Chain Monte Carlo technique in the analysis of cosmic-ray measurements in diffusion models. The size of the diffusive halo depends crucially on the value of the diffusion slope delta, and also on the presence/absence of the local underdensity damping effect on radioactive nuclei. More precise data from on-going experiments are expected to clarify this issue., Comment: 20 pages, 14 figures, minor language corrections to match the A&A accepted version
Published: 2010
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24. Systematic uncertainties on the cosmic-ray transport parameters: Is it possible to reconcile B/C data with delta = 1/3 or delta = 1/2?

Author: Maurin, D., Putze, A., and Derome, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The B/C ratio is used in cosmic-ray physics to constrain the transport parameters. However, from the same set of data, the various published values show a puzzling large scatter of these parameters. We investigate the impact of using different inputs (gas density and hydrogen fraction in the Galactic disc, source spectral shape, low-energy dependence of the diffusion coefficient, and nuclear fragmentation cross-sections) on the best-fit values of the transport parameters. We quantify the systematics produced when varying these inputs, and compare them to statistical uncertainties. We discuss the consequences for the slope of the diffusion coefficient delta. The analysis relies on the propagation code USINE interfaced with the Minuit minimisation routines. We find the typical systematic uncertainties to be larger than the statistical ones. The several published values of delta (from 0.3 to 0.8) can be recovered when varying the low-energy shape of the diffusion coefficient and the convective wind strength. Models including a convective wind are characterised by delta > 0.6, which cannot be reconcile with the expected theoretical values (1/3 and 1/2). However, from a statistical point of view (chi^2 analysis), models with both reacceleration and convection-hence large delta-are favoured. The next favoured models in line yield delta that can be accommodated with 1/3 and 1/2, but require a strong upturn of the diffusion coefficient at low energy (and no convection). To date, using the best statistical tools, the transport parameter determination is still plagued by many unknowns at low energy (~ GeV/n). To disentangle between all these configurations, measurements of the B/C ratio at TeV/n energies and/or combination with other secondary-to-primary ratios is necessary., Comment: 12 pages, 7 figures, minor language corrections to match the A&A accepted version
Published: 2010
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25. A Markov Chain Monte Carlo for Galactic Cosmic Ray physics: I. Method and results for the Leaky Box Model

Author: Putze, A., Derome, L., Maurin, D., Perotto, L., and Taillet, R.
Subjects: Astrophysics
Abstract: Propagation of charged cosmic-rays in the Galaxy depends on the transport parameters, whose number can be large depending on the propagation model under scrutiny. A standard approach for determining these parameters is a manual scan, leading to an inefficient and incomplete coverage of the parameter space. We implement a Markov Chain Monte Carlo (MCMC), which is well suited to multi-parameter determination. Its specificities (burn-in length, acceptance, and correlation length) are discussed in the phenomenologically well-understood Leaky-Box Model. From a technical point of view, a trial function based on binary-space partitioning is found to be extremely efficient, allowing a simultaneous determination of up to nine parameters, including transport and source parameters, such as slope and abundances. Our best-fit model includes both a low energy cut-off and reacceleration, whose values are consistent with those found in diffusion models. A Kolmogorov spectrum for the diffusion slope (delta=1/3) is excluded. The marginalised probability-density function for delta and alpha (the slope of the source spectra) are delta~0.55-0.60 and alpha~2.14-2.17, depending on the dataset used and the number of free parameters in the fit. All source-spectrum parameters (slope and abundances) are positively correlated among themselves and with the reacceleration strength, but are negatively correlated with the other propagation parameters. A forthcoming study will extend our analysis to more physical diffusion models., Comment: 18 pages, 15 figures, one brief section 2 added on the method (matches the A&A accepted version)
Published: 2008
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26. The RICH detector of the AMS-02 experiment: status and physics prospects

Author: Pereira, Rui, Aguilar-Benitez, M., Arruda, L., Barao, F., Baret, B., Barrau, A., Barreira, G., Belmont, E., Berdugo, J., Borges, J., Buenerd, M., Casadei, D., Casaus, J., Cortina, E., Costado, M., Crespo, D., Delgado, C., Diaz, C., Derome, L., Goncalves, P., Garcia-Lopez, R., de la Guia, C., Herrero, A., Lanciotti, E., Laurenti, G., Malinin, A., Mana, C., Marin, J., Mangin-Brinet, M., Martinez, G., Menchaca-Rocha, A., Palomares, C., Pimenta, M., Putze, A., Sallaz-Damaz, Y., Seo, E. S., Sevilla, I., Torrento, A., Vargas-Trevino, M., and Veziant, O.
Subjects: Astrophysics
Abstract: The Alpha Magnetic Spectrometer (AMS), whose final version AMS-02 is to be installed on the International Space Station (ISS) for at least 3 years, is a detector designed to measure charged cosmic ray spectra with energies up to the TeV region and with high energy photon detection capability up to a few hundred GeV. It is equipped with several subsystems, one of which is a proximity focusing RICH detector with a dual radiator (aerogel+NaF) that provides reliable measurements for particle velocity and charge. The assembly and testing of the AMS RICH is currently being finished and the full AMS detector is expected to be ready by the end of 2008. The RICH detector of AMS-02 is presented. Physics prospects are briefly discussed., Comment: 5 pages. Contribution to the 10th ICATPP Conference on Astroparticle, Particle, Space Physics, Detectors and Medical Physics Applications (Como 2007). Presenter: Rui Pereira
Published: 2008
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27. The AMS-RICH velocity and charge reconstruction

Author: Barao, F., Aguilar-Benitez, M., Arruda, L., Baret, B., Barrau, A., Barreira, G., Belmont, E., Berdugo, J., Borges, J., Buenerd, M., Casadei, D., Casaus, J., Cortina, E., Costado, M., Crespo, D., Delgado, C., Diaz, C., Derome, L., Goncalves, P., Garcia-Lopez, R., de la Guia, C., Herrero, A., Lanciotti, E., Laurenti, G., Malinin, A., Mana, C., Marin, J., Mangin-Brinet, M., Martinez, G., Menchaca-Rocha, A., Palomares, C., Pereira, R., Pimenta, M., Putze, A., Sallaz-Damaz, Y., Seo, E. S., Sevilla, I., Torrento, A., Vargas-Trevino, M., and Veziant, O.
Subjects: Astrophysics
Abstract: The AMS detector, to be installed on the International Space Station, includes a Ring Imaging Cerenkov detector with two different radiators, silica aerogel (n=1.05) and sodium fluoride (n=1.334). This detector is designed to provide very precise measurements of velocity and electric charge in a wide range of cosmic nuclei energies and atomic numbers. The detector geometry, in particular the presence of a reflector for acceptance purposes, leads to complex Cerenkov patterns detected in a pixelized photomultiplier matrix. The results of different reconstruction methods applied to test beam data as well as to simulated samples are presented. To ensure nominal performances throughout the flight, several detector parameters have to be carefully monitored. The algorithms developed to fulfill these requirements are presented. The velocity and charge measurements provided by the RICH detector endow the AMS spectrometer with precise particle identification capabilities in a wide energy range. The expected performances on light isotope separation are discussed., Comment: Contribution to the ICRC07, Merida, Mexico (2007); Presenter: F. Barao
Published: 2007

28. Nuclear Cosmic Rays propagation in the Atmosphere

Author: Putze, A., Derome, L., Maurin, D., and Buénerd, M.
Subjects: Astrophysics
Abstract: The transport of the nuclear cosmic ray flux in the atmosphere is studied and the atmospheric corrections to be applied to the measurements are calculated. The contribution of the calculated corrections to the accuracy of the experimental results are discussed and evaluated over the kinetic energy range 10-10$^{3}$ GeV/n. The Boron (B) and Carbon (C) elements system is used as a test case. It is shown that the required corrections become largely dominant at the highest energies investigated. The results are discussed., Comment: Proc. of 30th International Cosmic Ray Conference, Merida, Mexico; 4 pages
Published: 2007

29. Simulation of neutrino and charged particle production and propagation in the atmosphere

Author: Derome, L.
Subjects: Astrophysics, High Energy Physics - Phenomenology
Abstract: A precise evaluation of the secondary particle production and propagation in the atmosphere is very important for the atmospheric neutrino oscillation studies. The issue is addressed with the extension of a previously developed full 3-Dimensional Monte-Carlo simulation of particle generation and transport in the atmosphere, to compute the flux of secondary protons, muons and neutrinos. Recent balloon borne experiments have performed a set of accurate flux measurements for different particle species at different altitudes in the atmosphere, which can be used to test the calculations for the atmospheric neutrino production, and constrain the underlying hadronic models. The simulation results are reported and compared with the latest flux measurements. It is shown that the level of precision reached by these experiments could be used to constrain the nuclear models used in the simulation. The implication of these results for the atmospheric neutrino flux calculation are discussed., Comment: 11 pages, 9 figures
Published: 2006
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30. The Ring Imaging Cherenkov detector (RICH) of the AMS experiment

Author: Barao, F., Benitez, M. Aguilar, Alcaraz, J., Arruda, L., Barrau, A., Barreira, G., Belmont, E., Berdugo, J., Brinet, M., Buenerd, M., Casadei, D., Casaus, J., Cortina, E., Delgado, C., Diaz, C., Derome, L., Eraud, L., Garcia-Lopez, R. J., Gallin-Martel, L., Giovacchini, F., Goncalves, P., Lanciotti, E., Laurenti, G., Malinine, A., Mana, C., Marin, J., Martinez, G., Menchaca-Rocha, A., Molla, M., Palomares, C., Panniello, M., Pereira, R., Pimenta, M., Protasov, K., Sanchez, E., Seo, E-S., Sevilla, N., Torrento, A., Vargas-Trevino, M., and Veziant, O.
Subjects: Astrophysics
Abstract: The Alpha Magnetic Spectrometer (AMS) experiment to be installed on the International Space Station (ISS) will be equipped with a proximity focusing Ring Imaging Cherenkov (RICH) detector for measuring the electric charge and velocity of the charged cosmic particles. A RICH prototype consisting of 96 photomultiplier units, including a piece of the conical reflector, was built and its performance evaluated with ion beam data. Preliminary results of the in-beam tests performed with ion fragments resulting from collisions of a 158 GeV/c/nuc primary beam of Indium ions (CERN SPS) on a Pb target are reported. The collected data included tests to the final front-end electronics and to different aerogel radiators. Cherenkov rings for a large range of charged nuclei and with reflected photons were observed. The data analysis confirms the design goals. Charge separation up to Fe and velocity resolution of the order of 0.1% for singly charged particles are obtained., Comment: 29th International Conference on Cosmic Rays (Pune, India)
Published: 2006

31. Flux of light antimatter nuclei near earth, induced by Cosmic Rays in the Galaxy and in the atmosphere

Author: Duperray, R., Baret, B., Maurin, D., Boudoul, G., Barrau, A., Derome, L., Protasov, K., and Buenerd, M.
Subjects: Astrophysics
Abstract: The fluxes of light antinuclei A<=4 induced near earth by Cosmic Ray intera ctions with the interstellar matter in the Galaxy and with the Earth atmosphere, are calculated in a phenomenological framework. The hadronic production cross section for antinucleons is based on a recent parametrization of a wide set of accelerator data. The production of light nuclei is calculated using coalescence models. For the standard coalescence model, the coalescence radius is fitted to the available experimental data. The non annihilating inelastic scattering process for the antideuterons is discussed and taken into account for the first time via a more realistic procedure than used so far for antiprotons., Comment: 22 pages, 18 figures, 3 tables. Accepted for publication in Phys. Rev. D
Published: 2005
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32. A simulation study of Top and Bottom Counting Detectors in ISS-CREAM experiment for cosmic ray electron physics

Author: Park, J.M., Amare, Y., Anderson, T., Angelaszek, D., Anthony, N., Arnold, H., Choi, G.H., Copley, M., Coutu, S., Derome, L., Ebongue, C., Eraud, L., Faddis, I., Han, J.H., Howley, I.J., Huh, H.G., Hwang, Y.S., Hyun, H.J., Im, S., Jeon, H.B., Jeon, J.A., Jeong, S., Kang, S.C., Kim, D.Y., Kim, H.J., Kim, K.C., Kim, M.H., King, P., Lee, H.Y., Lee, J., Lee, M.H., Liang, J., Link, J.T., Lutz, L., Menchaca-Rocha, A., Mitchell, J.W., Morton, S., Nester, M., Nutter, S., Ofoha, O., Park, H., Park, I.H., Picot-Clemente, N., Seo, E.S., Smith, J.R., Walpole, P., Weinmann, R.P., Wu, J., Yon, B., and Yoon, Y.S.
Published: 2018
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33. The AMS-02 RICH Imager Prototype - In-Beam Tests with 20 GeV/c per Nucleon Ions -

Author: Buenerd, M., Aguayo, P., Benitez, M. Aguilar, Arruda, L., Barao, F., Barrau, A., Baret, B., Belmont, E., Berdugo, J., Boudoul, G., Borges, J., Casadei, D., Casaus, J., Delgado, C., Diaz, C., Derome, L., Eraud, L., Gallin-Martel, L., Giovacchini, F., Goncalves, P., Lanciotti, E., Laurenti, G., Malinine, A., Mana, C., Marin, J., Martinez, G., Menchaca-Rocha, A., Palomares, C., Pimenta, M., Protasov, K., Sanchez, E., Seo, E-S., Sevilla, I., Torrento, A., and Vargas-Trevino, M.
Subjects: Astrophysics
Abstract: A prototype of the AMS Cherenkov imager (RICH) has been tested at CERN by means of a low intensity 20 GeV/c per nucleon ion beam obtained by fragmentation of a primary beam of Pb ions. Data have been collected with a single beam setting, over the range of nuclear charges 2
Published: 2003

34. Secondary proton flux induced by cosmic ray interactions with the atmosphere

Author: Baret, B., Derome, L., Huang, C. Y., and Buenerd, M.
Subjects: Astrophysics
Abstract: The atmospheric secondary proton flux is studied for altitudes extending from sea level up to the top of atmosphere by means of a 3-dimensional Monte-Carlo simulation procedure successfully used previously to account for flux measurements of protons, light nuclei, and electrons-positrons below the geomagnetic cutoff (satellite data), and of muons and antiprotons (balloon data). The calculated flux are compared with the experimental measurements from sea level uo to high float ballon altitudes. The agreement between data and simulation results are very good at all altitudes, including the lowest ones, where the calculations become extremely sensitive to the proton production cross section. The results are discussed in this context. The calculations are extended to the study of quasi trapped particles above the atmosphere to about 5 Earth radii, for prospective purpose., Comment: 7 pages, 5 figures, submitted to Phys. Rev. D
Published: 2003
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35. Secondary antiproton flux induced by cosmic ray interactions with the atmosphere

Author: Huang, C. Y., Derome, L., and Buenerd, M.
Subjects: Astrophysics
Abstract: The atmospheric secondary antiproton flux is studied for detection altitudes extending from sea level up to about 3 earth radii, by means of a 3-dimensional Monte-Carlo simulation, successfully applied previously on other satellite and balloon data. The calculated antiproton flux at mountain altitude is found in fair agreement with the recent BESS measurements. The flux at balloon altitude is also in agreement with calculations performed in previous studies and used for the analysis of balloon data. The flux at sea level is found to be significant. The antineutron flux is also evaluated. The antiproton flux is prospectively explored at large distance from earth up to around 2 10$^4$ km. The results are discussed in the context of the forthcoming measurements by large acceptance experiments., Comment: 12 pages, 9 figures, 1 table, submitted to Phys. Rev. D
Published: 2003
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36. An improved gamma-ray limit on the density of PBHs

Author: Barrau, A., Boudoul, G., and Derome, L.
Subjects: Astrophysics
Abstract: Gamma-rays are, with antiprotons, a very efficient way to derive upper limits on the density of evaporating black holes. They have been successfully used in the last decades to severely constrain the amount of Primordial Black Holes (PBHs) in our Universe. This article suggests a little refinement, based on the expected background, to improve this limit by a factor of three. The resulting value is : Omega_PBH < 3.3E-9., Comment: To appear in the 28th ICRC conference proceedings
Published: 2003

37. A model for A=3 antinuclei production in proton-nucleus collisions

Author: Duperray, R. P., Protasov, K. V., Derome, L., and Buenerd, M.
Subjects: Nuclear Theory
Abstract: A simple coalescence model based on the same diagrammatic approach of antimatter production in hadronic collisions as used previously for antideuterons is used here for the hadroproduction of mass 3 antinuclei. It is shown that the model is able to reproduce the existing experimental data on Tbar and 3hebar production without any additional parameter., Comment: 7 figures. submitted to Eur. Phys. J. A
Published: 2003
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38. Atmospheric neutrino flux from 3-dimensional simulation

Author: Liu, Yong, Derome, L., and Buenerd, M.
Subjects: Astrophysics, High Energy Physics - Phenomenology
Abstract: The atmospheric muon and neutrino flux have been simulated using the same approach which successfully accounted for the recent secondary proton, electron and positron flux measurements in orbit by the AMS experiment. For the muon flux, a good agreement is obtained with the CAPRICE and HEAT data for altitudes ranging from sea level up to about 38 km. The general features of the calculated atmospheric neutrino flux are reported and discussed. The flux obtained at the Super-Kamiokande experiment location are reported and compared with other calculations. For low neutrino energies the flux obtained is significantly smaller than that used in the data analysis of underground experiment. The simulation results for the SOUDAN experiment site are also reported., Comment: 33 pages, 27 figures, 12 tables, final version for Phys. Rev. D
Published: 2002
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39. Origin of light nuclei in near earth orbit

Author: Derome, L. and Buenerd, M.
Subjects: Astrophysics, Nuclear Experiment
Abstract: The possible sources of light nuclei populations observed recently below the geomagnetic cutoff by the AMS experiment are discussed in terms of nuclear processes: fragmentation of the incoming flux of cosmic helium on atmospheric nuclei, and nuclear coalescence from proton and helium induced reactions. Results of simulations for deuterium, tritium, helium 3 and 4, are presented., Comment: 11 pages, 4 figures
Published: 2001
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40. Secondary electrons and positrons in near earth orbit

Author: Derome, L., Buenerd, M., and Liu, Yong
Subjects: Astrophysics
Abstract: 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., Comment: Final version for Phys. Lett. B: Title changed, new references added, minor changes in text
Published: 2001
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41. Origin of the high energy proton component below the geomagnetic cutoff in near earth orbit

Author: Derome, L., Buenerd, M., Barrau, A., Bouchet, A., Menchaca-Rocha, A., and Thuillier, T.
Subjects: Astrophysics
Abstract: The high flux proton component observed by AMS below the geomagnetic cutoff can be well accounted for by assuming these particles to be secondaries originating from the interaction of Cosmic Ray protons with the atmosphere. Simulation results are reported, Comment: 7 pages, Latex, 4 Postscript figures. Final version (minor corrections) for Physics Letters. B
Published: 2000
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42. Correction to: High precision particle astrophysics as a new window on the universe with an Antimatter Large Acceptance Detector In Orbit (ALADInO)

Author: Battiston, R., Bertucci, B., Adriani, O., Ambrosi, G., Baudouy, B., Blasi, P., Boezio, M., Campana, D., Derome, L., De Mitri, I., Di Felice, V., Donato, F., Duranti, M., Formato, V., Grasso, D., Gebauer, I., Iuppa, R., Masi, N., Maurin, D., Mazziotta, M. N., Musenich, R., Nozzoli, F., Papini, P., Picozza, P., Pearce, M., Pospíšil, S., Rossi, L., Tomassetti, N., Vagelli, V., and Wu, X.
Published: 2021
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43. Neutron monitors and muon detectors for solar modulation studies: 2. ϕ time series

Author: Ghelfi, A., Maurin, D., Cheminet, A., Derome, L., Hubert, G., and Melot, F.
Published: 2017
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44. Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer

Author: Aguilar, M., Ali Cavasonza, L., Alpat, B., Ambrosi, G., Arruda, L., Attig, N., Bagwell, C., Barao, F., Barrin, L., Bartoloni, A., Başeğmez-du Pree, S., Battiston, R., Belyaev, N., Berdugo, J., Bertucci, B., Bindi, V., Bollweg, K., Bolster, J., Borchiellini, M., Borgia, B., Boschini, M. J., Bourquin, M., Bueno, E. F., Burger, J., Burger, W. J., Cai, X. D., Capell, M., Casaus, J., Castellini, G., Cervelli, F., Chang, Y. H., Chen, G. M., Chen, G. R., Chen, H., Chen, H. S., Chen, Y., Cheng, L., Chou, H. Y., Chouridou, S., Choutko, V., Chung, C. H., Clark, C., Coignet, G., Consolandi, C., Contin, A., Corti, C., Cui, Z., Dadzie, K., Dass, A., Delgado, C., Della Torre, S., Demirköz, M. B., Derome, L., Di Falco, S., Di Felice, V., Díaz, C., Dimiccoli, F., von Doetinchem, P., Dong, F., Donnini, F., Duranti, M., Egorov, A., Eline, A., Faldi, F., Feng, J., Fiandrini, E., Fisher, P., Formato, V., Gámez, C., García-López, R. J., Gargiulo, C., Gast, H., Gervasi, M., Giovacchini, F., Gómez-Coral, D. M., Gong, J., Goy, C., Grabski, V., Grandi, D., Graziani, M., Guracho, A. N., Haino, S., Han, K. C., Hashmani, R. K., He, Z. H., Heber, B., Hsieh, T. H., Hu, J. Y., Huang, B. W., Incagli, M., Jang, W. Y., Jia, Yi, Jinchi, H., Karagöz, G., Khiali, B., Kim, G. N., Kirn, Th., Kounina, O., Kounine, A., Koutsenko, V., Krasnopevtsev, D., Kuhlman, A., Kulemzin, A., La Vacca, G., Laudi, E., Laurenti, G., LaVecchia, G., Lazzizzera, I., Lee, H. T., Lee, S. C., Li, H. L., Li, J. Q., Li, M., Li, Q., Li, Q. Y., Li, S., Li, S. L., Li, J. H., Li, Z. H., Liang, J., Liang, M. J., Lin, C. H., Lippert, T., Liu, J. H., Lu, S. Q., Lu, Y. S., Luebelsmeyer, K., Luo, J. Z., Luo, S. D., Luo, Xi, Machate, F., Mañá, C., Marín, J., Marquardt, J., Martin, T., Martínez, G., Masi, N., Maurin, D., Medvedeva, T., Menchaca-Rocha, A., Meng, Q., Mikhailov, V. V., Molero, M., Mott, P., Mussolin, L., Negrete, J., Nikonov, N., Nozzoli, F., Ocampo-Peleteiro, J., Oliva, A., Orcinha, M., Ottupara, M. A., Palermo, M., Palmonari, F., Paniccia, M., Pashnin, A., Pauluzzi, M., Pensotti, S., Plyaskin, V., Poluianov, S., Qin, X., Qu, Z. Y., Quadrani, L., Rancoita, P. G., Rapin, D., Reina Conde, A., Robyn, E., Romaneehsen, L., Rozhkov, A., Rozza, D., Sagdeev, R., Schael, S., Schultz von Dratzig, A., Schwering, G., Seo, E. S., Shan, B. S., Siedenburg, T., Song, J. W., Song, X. J., Sonnabend, R., Strigari, L., Su, T., Sun, Q., Sun, Z. T., Tacconi, M., Tang, X. W., Tang, Z. C., Tian, J., Tian, Y., Ting, Samuel C. C., Ting, S. M., Tomassetti, N., Torsti, J., Urban, T., Usoskin, I., Vagelli, V., Vainio, R., Valencia-Otero, M., Valente, E., Valtonen, E., Vázquez Acosta, M., Vecchi, M., Velasco, M., Vialle, J. P., Wang, C. X., Wang, L., Wang, L. Q., Wang, N. H., Wang, Q. L., Wang, S., Wang, X., Wang, Yu, Wang, Z. M., Wei, J., Weng, Z. L., Wu, H., Wu, Y., Xiao, J. N., Xiong, R. Q., Xiong, X. Z., Xu, W., Yan, Q., Yang, H. T., Yang, Y., Yashin, I. I., Yelland, A., Yi, H., You, Y. H., Yu, Y. M., Yu, Z. Q., Zannoni, M., Zhang, C., Zhang, F., Zhang, F. Z., Zhang, J., Zhang, J. H., Zhang, Z., Zhao, F., Zheng, C., Zheng, Z. M., Zhuang, H. L., Zhukov, V., Zichichi, A., Zuccon, P., Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Bagwell, C, Barao, F, Barrin, L, Bartoloni, A, Başeğmez-du Pree, S, Battiston, R, Belyaev, N, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Bolster, J, Borchiellini, M, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Dass, A, Delgado, C, Della Torre, S, Demirköz, M, Derome, L, Di Falco, S, Di Felice, V, Díaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Faldi, F, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Gámez, C, García-López, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gómez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Guracho, A, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Huang, B, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Karagöz, G, Khiali, B, Kim, G, Kirn, T, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lavecchia, G, Lazzizzera, I, Lee, H, Lee, S, Li, H, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Liang, M, Lin, C, Lippert, T, Liu, J, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, S, Luo, X, Machate, F, Mañá, C, Marín, J, Marquardt, J, Martin, T, Martínez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Ocampo-Peleteiro, J, Oliva, A, Orcinha, M, Ottupara, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Romaneehsen, L, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schultz von Dratzig, A, Schwering, G, Seo, E, Shan, B, Siedenburg, T, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Tian, Y, Ting, S, Tomassetti, N, Torsti, J, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vázquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Wu, Y, Xiao, J, Xiong, R, Xiong, X, Xu, W, Yan, Q, Yang, H, Yang, Y, Yashin, I, Yelland, A, Yi, H, You, Y, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, and Zuccon, P
Subjects: FIS/05 - ASTRONOMIA E ASTROFISICA, Astrophysics and Astronomy, FIS/01 - FISICA SPERIMENTALE, Cosmic rays
Abstract: We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38 × 106 sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167±0.006, for Ne/Si is 0.833±0.025, for Mg/Si is 0.994±0.029, and for C/O is 0.836±0.025. These values are determined independent of cosmic-ray propagation.
Published: 2023

45. Properties of Cosmic Aluminum Nuclei: Results from the Alpha Magnetic Spectrometer

Author: Liu, Z, Paniccia, M, Zhang, C, Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Plyaskin, V, Pohl, M, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Liu Z., Paniccia M., Zhang C., Aguilar M., Ali Cavasonza L., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Chen Y., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Krasnopevtsev D., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Medvedeva T., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Plyaskin V., Pohl M., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., von Dratzig A. S., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Solano C., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Acosta M. V., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., Zuccon P., Liu, Z, Paniccia, M, Zhang, C, Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Krasnopevtsev, D, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Medvedeva, T, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Plyaskin, V, Pohl, M, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Liu Z., Paniccia M., Zhang C., Aguilar M., Ali Cavasonza L., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Chen Y., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Krasnopevtsev D., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Medvedeva T., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Plyaskin V., Pohl M., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., von Dratzig A. S., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Solano C., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Acosta M. V., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., and Zuccon P.
Abstract: We report the properties of aluminum (Al) nuclei in cosmic rays measured in the rigidity range 2.15 GV to 3.0 TV with 0.51 million nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. We observed that above 6 GV the Al spectrum is well described by the weighted sum of the silicon spectrum (primary cosmic rays) and the fluorine spectrum (secondary cosmic rays). The fraction of the primary component increases with rigidity and becomes dominant at highest rigidities. Al/Si abundance ratio at the source is determined independent of cosmic ray propagation.
Published: 2022

46. Observation of Z>2 trapped nuclei by AMS on ISS

Author: Giovacchini, F, Oliva, A, Valencia-Otero, M, Aguilar, M, Ali Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valente, E, Valtonen, E, Vazquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Giovacchini F., Oliva A., Valencia-Otero M., Aguilar M., Ali Cavasonza L., Allen M. S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Chen Y., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Liu Z., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Lyu S. S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Mo D. C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Schulz von Dratzig A., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang C., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., Zuccon P., Giovacchini, F, Oliva, A, Valencia-Otero, M, Aguilar, M, Ali Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beranek, B, Berdugo, J, Bertucci, B, Bindi, V, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Chen, Y, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Orcinha, M, Palermo, M, Palmonari, F, Paniccia, M, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, Schulz von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valente, E, Valtonen, E, Vazquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, Giovacchini F., Oliva A., Valencia-Otero M., Aguilar M., Ali Cavasonza L., Allen M. S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beranek B., Berdugo J., Bertucci B., Bindi V., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Chen Y., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Liu Z., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Lyu S. S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Mo D. C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Orcinha M., Palermo M., Palmonari F., Paniccia M., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., Schulz von Dratzig A., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang C., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., and Zuccon P.
Abstract: The Alpha Magnetic Spectrometer (AMS-02) is a high energy particle physics experiment operating continuously aboard the International Space Station (ISS) since the 19th of May of 2011. A component of trapped Z>2 ions located in the South Atlantic Anomaly (SAA) has been detected traversing the instrument both in down-going and up-going directions.
Published: 2022

47. Properties of Iron Primary Cosmic Rays: Results from the Alpha Magnetic Spectrometer

Author: Chen, Y, Paniccia, M, Aguilar, M, Ali Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, de Boer, W, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vazquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Chen Y., Paniccia M., Aguilar M., Ali Cavasonza L., Allen M. S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beischer B., Berdugo J., Bertucci B., Bindi V., de Boer W., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Liu Z., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Lyu S. S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Mo D. C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., von Dratzig A. S., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Solano C., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang C., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., Zimmermann N., Zuccon P., Chen, Y, Paniccia, M, Aguilar, M, Ali Cavasonza, L, Allen, M, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Barao, F, Barrin, L, Bartoloni, A, Basegmez-Du Pree, S, Battiston, R, Behlmann, M, Beischer, B, Berdugo, J, Bertucci, B, Bindi, V, de Boer, W, Bollweg, K, Borgia, B, Boschini, M, Bourquin, M, Bueno, E, Burger, J, Burger, W, Burmeister, S, Cai, X, Capell, M, Casaus, J, Castellini, G, Cervelli, F, Chang, Y, Chen, G, Chen, H, Cheng, L, Chou, H, Chouridou, S, Choutko, V, Chung, C, Clark, C, Coignet, G, Consolandi, C, Contin, A, Corti, C, Cui, Z, Dadzie, K, Delgado, C, Della Torre, S, Demirkoz, M, Derome, L, Di Falco, S, Di Felice, V, Diaz, C, Dimiccoli, F, von Doetinchem, P, Dong, F, Donnini, F, Duranti, M, Egorov, A, Eline, A, Feng, J, Fiandrini, E, Fisher, P, Formato, V, Freeman, C, Galaktionov, Y, Gamez, C, Garcia-Lopez, R, Gargiulo, C, Gast, H, Gervasi, M, Giovacchini, F, Gomez-Coral, D, Gong, J, Goy, C, Grabski, V, Grandi, D, Graziani, M, Haino, S, Han, K, Hashmani, R, He, Z, Heber, B, Hsieh, T, Hu, J, Incagli, M, Jang, W, Jia, Y, Jinchi, H, Kanishev, K, Khiali, B, Kim, G, Kirn, T, Konyushikhin, M, Kounina, O, Kounine, A, Koutsenko, V, Kuhlman, A, Kulemzin, A, La Vacca, G, Laudi, E, Laurenti, G, Lazzizzera, I, Lebedev, A, Lee, H, Lee, S, Li, J, Li, M, Li, Q, Li, S, Li, Z, Liang, J, Light, C, Lin, C, Lippert, T, Liu, J, Liu, Z, Lu, S, Lu, Y, Luebelsmeyer, K, Luo, J, Luo, X, Lyu, S, Machate, F, Mana, C, Marin, J, Marquardt, J, Martin, T, Martinez, G, Masi, N, Maurin, D, Menchaca-Rocha, A, Meng, Q, Mikhailov, V, Mo, D, Molero, M, Mott, P, Mussolin, L, Negrete, J, Nikonov, N, Nozzoli, F, Oliva, A, Orcinha, M, Palermo, M, Palmonari, F, Pashnin, A, Pauluzzi, M, Pensotti, S, Phan, H, Piandani, R, Plyaskin, V, Poluianov, S, Qin, X, Qu, Z, Quadrani, L, Rancoita, P, Rapin, D, Reina Conde, A, Robyn, E, Rosier-Lees, S, Rozhkov, A, Rozza, D, Sagdeev, R, Schael, S, von Dratzig, A, Schwering, G, Seo, E, Shakfa, Z, Shan, B, Siedenburg, T, Solano, C, Song, J, Song, X, Sonnabend, R, Strigari, L, Su, T, Sun, Q, Sun, Z, Tacconi, M, Tang, X, Tang, Z, Tian, J, Ting, S, Tomassetti, N, Torsti, J, Tuysuz, C, Urban, T, Usoskin, I, Vagelli, V, Vainio, R, Valencia-Otero, M, Valente, E, Valtonen, E, Vazquez Acosta, M, Vecchi, M, Velasco, M, Vialle, J, Wang, C, Wang, L, Wang, N, Wang, Q, Wang, S, Wang, X, Wang, Y, Wang, Z, Wei, J, Weng, Z, Wu, H, Xiong, R, Xu, W, Yan, Q, Yang, Y, Yashin, I, Yi, H, Yu, Y, Yu, Z, Zannoni, M, Zhang, C, Zhang, F, Zhang, J, Zhang, Z, Zhao, F, Zheng, C, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zimmermann, N, Zuccon, P, Chen Y., Paniccia M., Aguilar M., Ali Cavasonza L., Allen M. S., Alpat B., Ambrosi G., Arruda L., Attig N., Barao F., Barrin L., Bartoloni A., Basegmez-Du Pree S., Battiston R., Behlmann M., Beischer B., Berdugo J., Bertucci B., Bindi V., de Boer W., Bollweg K., Borgia B., Boschini M. J., Bourquin M., Bueno E. F., Burger J., Burger W. J., Burmeister S., Cai X. D., Capell M., Casaus J., Castellini G., Cervelli F., Chang Y. H., Chen G. M., Chen G. R., Chen H. S., Cheng L., Chou H. Y., Chouridou S., Choutko V., Chung C. H., Clark C., Coignet G., Consolandi C., Contin A., Corti C., Cui Z., Dadzie K., Delgado C., Della Torre S., Demirkoz M. B., Derome L., Di Falco S., Di Felice V., Diaz C., Dimiccoli F., von Doetinchem P., Dong F., Donnini F., Duranti M., Egorov A., Eline A., Feng J., Fiandrini E., Fisher P., Formato V., Freeman C., Galaktionov Y., Gamez C., Garcia-Lopez R. J., Gargiulo C., Gast H., Gervasi M., Giovacchini F., Gomez-Coral D. M., Gong J., Goy C., Grabski V., Grandi D., Graziani M., Haino S., Han K. C., Hashmani R. K., He Z. H., Heber B., Hsieh T. H., Hu J. Y., Incagli M., Jang W. Y., Jia Y., Jinchi H., Kanishev K., Khiali B., Kim G. N., Kirn Th., Konyushikhin M., Kounina O., Kounine A., Koutsenko V., Kuhlman A., Kulemzin A., La Vacca G., Laudi E., Laurenti G., Lazzizzera I., Lebedev A., Lee H. T., Lee S. C., Li J. Q., Li M., Li Q., Li S., Li J. H., Li Z. H., Liang J., Light C., Lin C. H., Lippert T., Liu J. H., Liu Z., Lu S. Q., Lu Y. S., Luebelsmeyer K., Luo J. Z., Luo X., Lyu S. S., Machate F., Mana C., Marin J., Marquardt J., Martin T., Martinez G., Masi N., Maurin D., Menchaca-Rocha A., Meng Q., Mikhailov V. V., Mo D. C., Molero M., Mott P., Mussolin L., Negrete J., Nikonov N., Nozzoli F., Oliva A., Orcinha M., Palermo M., Palmonari F., Pashnin A., Pauluzzi M., Pensotti S., Phan H. D., Piandani R., Plyaskin V., Poluianov S., Qin X., Qu Z. Y., Quadrani L., Rancoita P. G., Rapin D., Reina Conde A., Robyn E., Rosier-Lees S., Rozhkov A., Rozza D., Sagdeev R., Schael S., von Dratzig A. S., Schwering G., Seo E. S., Shakfa Z., Shan B. S., Siedenburg T., Solano C., Song J. W., Song X. J., Sonnabend R., Strigari L., Su T., Sun Q., Sun Z. T., Tacconi M., Tang X. W., Tang Z. C., Tian J., Ting S. C. C., Ting S. M., Tomassetti N., Torsti J., Tuysuz C., Urban T., Usoskin I., Vagelli V., Vainio R., Valencia-Otero M., Valente E., Valtonen E., Vazquez Acosta M., Vecchi M., Velasco M., Vialle J. P., Wang C. X., Wang L., Wang L. Q., Wang N. H., Wang Q. L., Wang S., Wang X., Wang Y., Wang Z. M., Wei J., Weng Z. L., Wu H., Xiong R. Q., Xu W., Yan Q., Yang Y., Yashin I. I., Yi H., Yu Y. M., Yu Z. Q., Zannoni M., Zhang C., Zhang F., Zhang F. Z., Zhang J. H., Zhang Z., Zhao F., Zheng C., Zheng Z. M., Zhuang H. L., Zhukov V., Zichichi A., Zimmermann N., and Zuccon P.
Abstract: We report the observation of new properties of primary iron (Fe) cosmic rays in the rigidity range 2.65 GV to 3.0 TV with 0.62 million iron nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. Above 80.5 GV the rigidity dependence of the cosmic ray Fe flux is identical to the rigidity dependence of the primary cosmic ray He, C, and O fluxes, with the Fe/O flux ratio being constant at 0.155±0.006. This shows that unexpectedly Fe and He, C, and O belong to the same class of primary cosmic rays which is different from the primary cosmic rays Ne, Mg, and Si class.
Published: 2022

48. Temporal structures in electron spectra and charge sign effects in galactic cosmic rays

Author: Aguilar, M. (M.), Cavasonza, L. A. (L. Ali), Ambrosi, G. (G.), Arruda, L. (L.), Attig, N. (N.), Bagwell, C. (C.), Barao, F. (F.), Barrin, L. (L.), Bartoloni, A. (A.), Basegmez-du Pree, S. (S.), Battiston, R. (R.), Behlmann, M. (M.), Belyaev, N. (N.), Berdugo, J. (J.), Bertucci, B. (B.), Bindi, V. (V.), Bollweg, K. (K.), Bolster, J. (J.), Borgia, B. (B.), Boschini, M. J. (M. J.), Bourquin, M. (M.), Bueno, E. F. (E. F.), Burger, J. (J.), Burger, W. J. (W. J.), Burmeister, S. (S.), Cai, X. D. (X. D.), Capell, M. (M.), Casaus, J. (J.), Castellini, G. (G.), Cervelli, F. (F.), Chang, Y. H. (Y. H.), Chen, G. M. (G. M.), Chen, G. R. (G. R.), Chen, H. S. (H. S.), Chen, Y. (Y.), Cheng, L. (L.), Chou, H. Y. (H. Y.), Chouridou, S. (S.), Choutko, V. (V.), Chung, C. H. (C. H.), Clark, C. (C.), Coignet, G. (G.), Consolandi, C. (C.), Contin, A. (A.), Corti, C. (C.), Cui, Z. (Z.), Dadzie, K. (K.), Dass, A. (A.), Delgado, C. (C.), Della Torre, S. (S.), Demirkoez, M. B. (M. B.), Derome, L. (L.), Di Falco, S. (S.), Di Felice, V. (V.), Diaz, C. (C.), Dimiccoli, F. (F.), von Doetinchem, P. (P.), Dong, F. (F.), Donnini, F. (F.), Duranti, M. (M.), Egorov, A. (A.), Eline, A. (A.), Faldi, F. (F.), Feng, J. (J.), Fiandrini, E. (E.), Fisher, P. (P.), Formato, V. (V.), Freeman, C. (C.), Gamez, C. (C.), Garcia-Lopez, R. J. (R. J.), Gargiulo, C. (C.), Gast, H. (H.), Gervasi, M. (M.), Giovacchini, F. (F.), Gomez-Coral, D. M. (D. M.), Gong, J. (J.), Goy, C. (C.), Grabski, V. (V.), Grandi, D. (D.), Graziani, M. (M.), Guracho, A. N. (A. N.), Haino, S. (S.), Han, K. C. (K. C.), Hashmani, R. K. (R. K.), He, Z. H. (Z. H.), Heber, B. (B.), Hsieh, T. H. (T. H.), Hu, J. Y. (J. Y.), Incagli, M. (M.), Jang, W. Y. (W. Y.), Jia, Y. (Yi), Jinchi, H. (H.), Karagoez, G. (G.), Khiali, B. (B.), Kim, G. N. (G. N.), Kirn, T. (Th.), Kounina, O. (O.), Kounine, A. (A.), Koutsenko, V. (V.), Krasnopevtsev, D. (D.), Kuhlman, A. (A.), Kulemzin, A. (A.), La Vacca, G. (G.), Laudi, E. (E.), Laurenti, G. (G.), LaVecchia, G. (G.), Lazzizzera, I. (I.), Lee, H. T. (H. T.), Lee, S. C. (S. C.), Li, H. L. (H. L.), Li, J. Q. (J. Q.), Li, M. (M.), Li, Q. (Q.), Li, Q. Y. (Q. Y.), Li, S. (S.), Li, S. L. (S. L.), Li, J. H. (J. H.), Li, Z. H. (Z. H.), Liang, J. (J.), Liang, M. J. (M. J.), Light, C. (C.), Lin, C. H. (C. H.), Lippert, T. (T.), Liu, J. H. (J. H.), Lu, S. Q. (S. Q.), Lu, Y. S. (Y. S.), Luebelsmeyer, K. (K.), Luo, J. Z. (J. Z.), Luo, X. (Xi), Machate, F. (F.), Mana, C. (C.), Marin, J. (J.), Marquardt, J. (J.), Martin, T. (T.), Martinez, G. (G.), Masi, N. (N.), Maurin, D. (D.), Medvedeva, T. (T.), Menchaca-Rocha, A. (A.), Meng, Q. (Q.), Mikhailov, V. V. (V. V.), Molero, M. (M.), Mott, P. (P.), Mussolin, L. (L.), Negrete, J. (J.), Nikonov, N. (N.), Nozzoli, F. (F.), Ocampo-Peleteiro, J. (J.), Oliva, A. (A.), Orcinha, M. (M.), Palermo, M. (M.), Palmonari, F. (F.), Paniccia, M. (M.), Pashnin, A. (A.), Pauluzzi, M. (M.), Pensotti, S. (S.), Plyaskin, V. (V.), Pohl, M. (M.), Poluianov, S. (S.), Qin, X. (X.), Qu, Z. Y. (Z. Y.), Quadrani, L. (L.), Rancoita, P. G. (P. G.), Rapin, D. (D.), Conde, A. R. (A. Reina), Robyn, E. (E.), Rosier-Lees, S. (S.), Rozhkov, A. (A.), Rozza, D. (D.), Sagdeev, R. (R.), Schael, S. (S.), von Dratzig, A. S. (A. Schultz), Schwering, G. (G.), Seo, E. S. (E. S.), Shan, B. S. (B. S.), Siedenburg, T. (T.), Song, J. W. (J. W.), Song, X. J. (X. J.), Sonnabend, R. (R.), Strigari, L. (L.), Su, T. (T.), Sun, Q. (Q.), Sun, Z. T. (Z. T.), Tacconi, M. (M.), Tang, X. W. (X. W.), Tang, Z. C. (Z. C.), Tian, J. (J.), Ting, S. C. (Samuel C. C.), Ting, S. M. (S. M.), Tomassetti, N. (N.), Torsti, J. (J.), Urban, T. (T.), Usoskin, I. (I.), Vagelli, V. (V.), Vainio, R. (R.), Valencia-Otero, M. (M.), Valente, E. (E.), Valtonen, E. (E.), Acosta, M. V. (M. Vazquez), Vecchi, M. (M.), Velasco, M. (M.), Vialle, J. P. (J. P.), Wang, C. X. (C. X.), Wang, L. (L.), Wang, L. Q. (L. Q.), Wang, N. H. (N. H.), Wang, Q. L. (Q. L.), Wang, S. (S.), Wang, X. (X.), Wang, Y. (Yu), Wang, Z. M. (Z. M.), Wei, J. (J.), Weng, Z. L. (Z. L.), Wu, H. (H.), Xiong, R. Q. (R. Q.), Xu, W. (W.), Yan, Q. (Q.), Yang, Y. (Y.), Yashin, I. I. (I. I.), Yelland, A. (A.), Yi, H. (H.), Yu, Y. M. (Y. M.), Yu, Z. Q. (Z. Q.), Zannoni, M. (M.), Zhang, C. (C.), Zhang, F. (F.), Zhang, F. Z. (F. Z.), Zhang, J. H. (J. H.), Zhang, Z. (Z.), Zhao, F. (F.), Zheng, C. (C.), Zheng, Z. M. (Z. M.), Zhuang, H. L. (H. L.), Zhukov, V. (V.), Zichichi, A. (A.), Zuccon, P. (P.), Aguilar, M. (M.), Cavasonza, L. A. (L. Ali), Ambrosi, G. (G.), Arruda, L. (L.), Attig, N. (N.), Bagwell, C. (C.), Barao, F. (F.), Barrin, L. (L.), Bartoloni, A. (A.), Basegmez-du Pree, S. (S.), Battiston, R. (R.), Behlmann, M. (M.), Belyaev, N. (N.), Berdugo, J. (J.), Bertucci, B. (B.), Bindi, V. (V.), Bollweg, K. (K.), Bolster, J. (J.), Borgia, B. (B.), Boschini, M. J. (M. J.), Bourquin, M. (M.), Bueno, E. F. (E. F.), Burger, J. (J.), Burger, W. J. (W. J.), Burmeister, S. (S.), Cai, X. D. (X. D.), Capell, M. (M.), Casaus, J. (J.), Castellini, G. (G.), Cervelli, F. (F.), Chang, Y. H. (Y. H.), Chen, G. M. (G. M.), Chen, G. R. (G. R.), Chen, H. S. (H. S.), Chen, Y. (Y.), Cheng, L. (L.), Chou, H. Y. (H. Y.), Chouridou, S. (S.), Choutko, V. (V.), Chung, C. H. (C. H.), Clark, C. (C.), Coignet, G. (G.), Consolandi, C. (C.), Contin, A. (A.), Corti, C. (C.), Cui, Z. (Z.), Dadzie, K. (K.), Dass, A. (A.), Delgado, C. (C.), Della Torre, S. (S.), Demirkoez, M. B. (M. B.), Derome, L. (L.), Di Falco, S. (S.), Di Felice, V. (V.), Diaz, C. (C.), Dimiccoli, F. (F.), von Doetinchem, P. (P.), Dong, F. (F.), Donnini, F. (F.), Duranti, M. (M.), Egorov, A. (A.), Eline, A. (A.), Faldi, F. (F.), Feng, J. (J.), Fiandrini, E. (E.), Fisher, P. (P.), Formato, V. (V.), Freeman, C. (C.), Gamez, C. (C.), Garcia-Lopez, R. J. (R. J.), Gargiulo, C. (C.), Gast, H. (H.), Gervasi, M. (M.), Giovacchini, F. (F.), Gomez-Coral, D. M. (D. M.), Gong, J. (J.), Goy, C. (C.), Grabski, V. (V.), Grandi, D. (D.), Graziani, M. (M.), Guracho, A. N. (A. N.), Haino, S. (S.), Han, K. C. (K. C.), Hashmani, R. K. (R. K.), He, Z. H. (Z. H.), Heber, B. (B.), Hsieh, T. H. (T. H.), Hu, J. Y. (J. Y.), Incagli, M. (M.), Jang, W. Y. (W. Y.), Jia, Y. (Yi), Jinchi, H. (H.), Karagoez, G. (G.), Khiali, B. (B.), Kim, G. N. (G. N.), Kirn, T. (Th.), Kounina, O. (O.), Kounine, A. (A.), Koutsenko, V. (V.), Krasnopevtsev, D. (D.), Kuhlman, A. (A.), Kulemzin, A. (A.), La Vacca, G. (G.), Laudi, E. (E.), Laurenti, G. (G.), LaVecchia, G. (G.), Lazzizzera, I. (I.), Lee, H. T. (H. T.), Lee, S. C. (S. C.), Li, H. L. (H. L.), Li, J. Q. (J. Q.), Li, M. (M.), Li, Q. (Q.), Li, Q. Y. (Q. Y.), Li, S. (S.), Li, S. L. (S. L.), Li, J. H. (J. H.), Li, Z. H. (Z. H.), Liang, J. (J.), Liang, M. J. (M. J.), Light, C. (C.), Lin, C. H. (C. H.), Lippert, T. (T.), Liu, J. H. (J. H.), Lu, S. Q. (S. Q.), Lu, Y. S. (Y. S.), Luebelsmeyer, K. (K.), Luo, J. Z. (J. Z.), Luo, X. (Xi), Machate, F. (F.), Mana, C. (C.), Marin, J. (J.), Marquardt, J. (J.), Martin, T. (T.), Martinez, G. (G.), Masi, N. (N.), Maurin, D. (D.), Medvedeva, T. (T.), Menchaca-Rocha, A. (A.), Meng, Q. (Q.), Mikhailov, V. V. (V. V.), Molero, M. (M.), Mott, P. (P.), Mussolin, L. (L.), Negrete, J. (J.), Nikonov, N. (N.), Nozzoli, F. (F.), Ocampo-Peleteiro, J. (J.), Oliva, A. (A.), Orcinha, M. (M.), Palermo, M. (M.), Palmonari, F. (F.), Paniccia, M. (M.), Pashnin, A. (A.), Pauluzzi, M. (M.), Pensotti, S. (S.), Plyaskin, V. (V.), Pohl, M. (M.), Poluianov, S. (S.), Qin, X. (X.), Qu, Z. Y. (Z. Y.), Quadrani, L. (L.), Rancoita, P. G. (P. G.), Rapin, D. (D.), Conde, A. R. (A. Reina), Robyn, E. (E.), Rosier-Lees, S. (S.), Rozhkov, A. (A.), Rozza, D. (D.), Sagdeev, R. (R.), Schael, S. (S.), von Dratzig, A. S. (A. Schultz), Schwering, G. (G.), Seo, E. S. (E. S.), Shan, B. S. (B. S.), Siedenburg, T. (T.), Song, J. W. (J. W.), Song, X. J. (X. J.), Sonnabend, R. (R.), Strigari, L. (L.), Su, T. (T.), Sun, Q. (Q.), Sun, Z. T. (Z. T.), Tacconi, M. (M.), Tang, X. W. (X. W.), Tang, Z. C. (Z. C.), Tian, J. (J.), Ting, S. C. (Samuel C. C.), Ting, S. M. (S. M.), Tomassetti, N. (N.), Torsti, J. (J.), Urban, T. (T.), Usoskin, I. (I.), Vagelli, V. (V.), Vainio, R. (R.), Valencia-Otero, M. (M.), Valente, E. (E.), Valtonen, E. (E.), Acosta, M. V. (M. Vazquez), Vecchi, M. (M.), Velasco, M. (M.), Vialle, J. P. (J. P.), Wang, C. X. (C. X.), Wang, L. (L.), Wang, L. Q. (L. Q.), Wang, N. H. (N. H.), Wang, Q. L. (Q. L.), Wang, S. (S.), Wang, X. (X.), Wang, Y. (Yu), Wang, Z. M. (Z. M.), Wei, J. (J.), Weng, Z. L. (Z. L.), Wu, H. (H.), Xiong, R. Q. (R. Q.), Xu, W. (W.), Yan, Q. (Q.), Yang, Y. (Y.), Yashin, I. I. (I. I.), Yelland, A. (A.), Yi, H. (H.), Yu, Y. M. (Y. M.), Yu, Z. Q. (Z. Q.), Zannoni, M. (M.), Zhang, C. (C.), Zhang, F. (F.), Zhang, F. Z. (F. Z.), Zhang, J. H. (J. H.), Zhang, Z. (Z.), Zhao, F. (F.), Zheng, C. (C.), Zheng, Z. M. (Z. M.), Zhuang, H. L. (H. L.), Zhukov, V. (V.), Zichichi, A. (A.), and Zuccon, P. (P.)
Abstract: We present the precision measurements of 11 years of daily cosmic electron fluxes in the rigidity interval from 1.00 to 41.9 GV based on 2.0 x 10⁸ electrons collected with the Alpha Magnetic Spectrometer (AMS) aboard the International Space Station. The electron fluxes exhibit variations on multiple timescales. Recurrent electron flux variations with periods of 27 days, 13.5 days, and 9 days are observed. We find that the electron fluxes show distinctly different time variations from the proton fluxes. Remarkably, a hysteresis between the electron flux and the proton flux is observed with a significance of greater than 6 sigma at rigidities below 8.5 GV. Furthermore, significant structures in the electron-proton hysteresis are observed corresponding to sharp structures in both fluxes. This continuous daily electron data provide unique input to the understanding of the charge sign dependence of cosmic rays over an 11-year solar cycle.
Published: 2023

49. Properties of cosmic-ray sulfur and determination of the composition of primary cosmic-ray carbon, neon, magnesium, and sulfur:ten-year results from the Alpha Magnetic Spectrometer

Author: Aguilar, M. (M.), Cavasonza, L. A. (L. Ali), Alpat, B. (B.), Ambrosi, G. (G.), Arruda, L. (L.), Attig, N. (N.), Bagwell, C. (C.), Barao, F. (F.), Barrin, L. (L.), Bartoloni, A. (A.), Basegmez-du Pree, S. (S.), Battiston, R. (R.), Belyaev, N. (N.), Berdugo, J. (J.), Bertucci, B. (B.), Bindi, V. (V.), Bollweg, K. (K.), Bolster, J. (J.), Borchiellini, M. (M.), Borgia, B. (B.), Boschini, M. J. (M. J.), Bourquin, M. (M.), Bueno, E. F. (E. F.), Burger, J. (J.), Burger, W. J. (W. J.), Cai, X. D. (X. D.), Capell, M. (M.), Casaus, J. (J.), Castellini, G. (G.), Cervelli, F. (F.), Chang, Y. H. (Y. H.), Chen, G. M. (G. M.), Chen, G. R. (G. R.), Chen, H. (H.), Chen, H. S. (H. S.), Chen, Y. (Y.), Cheng, L. (L.), Chou, H. Y. (H. Y.), Chouridou, S. (S.), Choutko, V. (V.), Chung, C. H. (C. H.), Clark, C. (C.), Coignet, G. (G.), Consolandi, C. (C.), Contin, A. (A.), Corti, C. (C.), Cui, Z. (Z.), Dadzie, K. (K.), Dass, A. (A.), Delgado, C. (C.), Della Torre, S. (S.), Demirkoz, M. B. (M. B.), Derome, L. (L.), Di Falco, S. (S.), Di Felice, V. (V.), Diaz, C. (C.), Dimiccoli, F. (F.), von Doetinchem, P. (P.), Dong, F. (F.), Donnini, F. (F.), Duranti, M. (M.), Egorov, A. (A.), Eline, A. (A.), Faldi, F. (F.), Feng, J. (J.), Fiandrini, E. (E.), Fisher, P. (P.), Formato, V. (V.), Gamez, C. (C.), Garcia-Lopez, R. J. (R. J.), Gargiulo, C. (C.), Gast, H. (H.), Gervasi, M. (M.), Giovacchini, F. (F.), Gomez-Coral, D. M. (D. M.), Gong, J. (J.), Goy, C. (C.), Grabski, V. (V.), Grandi, D. (D.), Graziani, M. (M.), Guracho, A. N. (A. N.), Haino, S. (S.), Han, K. C. (K. C.), Hashmani, R. K. (R. K.), He, Z. H. (Z. H.), Heber, B. (B.), Hsieh, T. H. (T. H.), Hu, J. Y. (J. Y.), Huang, B. W. (B. W.), Incagli, M. (M.), Jang, W. Y. (W. Y.), Jia, Y. (Yi), Jinchi, H. (H.), Karagoz, G. (G.), Khiali, B. (B.), Kim, G. N. (G. N.), Kirn, T. (Th.), Kounina, O. (O.), Kounine, A. (A.), Koutsenko, V. (V.), Krasnopevtsev, D. (D.), Kuhlman, A. (A.), Kulemzin, A. (A.), La Vacca, G. (G.), Laudi, E. (E.), Laurenti, G. (G.), LaVecchia, G. (G.), Lazzizzera, I. (I.), Lee, H. T. (H. T.), Lee, S. C. (S. C.), Li, H. L. (H. L.), Li, J. Q. (J. Q.), Li, M. (M.), Li, Q. (Q.), Li, Q. Y. (Q. Y.), Li, S. (S.), Li, S. L. (S. L.), Li, J. H. (J. H.), Li, Z. H. (Z. H.), Liang, J. (J.), Liang, M. J. (M. J.), Lin, C. H. (C. H.), Lippert, T. (T.), Liu, J. H. (J. H.), Lu, S. Q. (S. Q.), Lu, Y. S. (Y. S.), Luebelsmeyer, K. (K.), Luo, J. Z. (J. Z.), Luo, S. D. (S. D.), Luo, X. (Xi), Machate, F. (F.), Mana, C. (C.), Marin, J. (J.), Marquardt, J. (J.), Martin, T. (T.), Martinez, G. (G.), Masi, N. (N.), Maurin, D. (D.), Medvedeva, T. (T.), Menchaca-Rocha, A. (A.), Meng, Q. (Q.), Mikhailov, V. V. (V. V.), Molero, M. (M.), Mott, P. (P.), Mussolin, L. (L.), Negrete, J. (J.), Nikonov, N. (N.), Nozzoli, F. (F.), Ocampo-Peleteiro, J. (J.), Oliva, A. (A.), Orcinha, M. (M.), Ottupara, M. A. (M. A.), Palermo, M. (M.), Palmonari, F. (F.), Paniccia, M. (M.), Pashnin, A. (A.), Pauluzzi, M. (M.), Pensotti, S. (S.), Plyaskin, V. (V.), Poluianov, S. (Stepan), Qin, X. (X.), Qu, Z. Y. (Z. Y.), Quadrani, L. (L.), Rancoita, P. G. (P. G.), Rapin, D. (D.), Conde, A. R. (A. Reina), Robyn, E. (E.), Romaneehsen, L. (L.), Rozhkov, A. (A.), Rozza, D. (D.), Sagdeev, R. (R.), Schael, S. (S.), von Dratzig, A. S. (A. Schultz), Schwering, G. (G.), Seo, E. S. (E. S.), Shan, B. S. (B. S.), Siedenburg, T. (T.), Song, J. W. (J. W.), Song, X. J. (X. J.), Sonnabend, R. (R.), Strigari, L. (L.), Su, T. (T.), Sun, Q. (Q.), Sun, Z. T. (Z. T.), Tacconi, M. (M.), Tang, X. W. (X. W.), Tang, Z. C. (Z. C.), Tian, J. (J.), Tian, Y. (Y.), Ting, S. C. (Samuel C. C.), Urban, T. (T.), Usoskin, I. (Ilya), Vagelli, V. (V.), Vainio, R. (R.), Valencia-Otero, M. (M.), Valente, E. (E.), Valtonen, E. (E.), Acosta, M. V. (M. Vazquez), Vecchi, M. (M.), Velasco, M. (M.), Vialle, J. P. (J. P.), Wang, C. X. (C. X.), Wang, L. (L.), Wang, L. Q. (L. Q.), Wang, N. H. (N. H.), Wang, Q. L. (Q. L.), Wang, S. (S.), Wang, X. (X.), Wang, Y. (Yu), Wang, Z. M. (Z. M.), Wei, J. (J.), Weng, Z. L. (Z. L.), Wu, H. (H.), Wu, Y. (Y.), Xiao, J. N. (J. N.), Xiong, R. Q. (R. Q.), Xiong, X. Z. (X. Z.), Xu, W. (W.), Yan, Q. (Q.), Yang, H. T. (H. T.), Yang, Y. (Y.), Yashin, I. I. (I. I.), Yelland, A. (A.), Yi, H. (H.), You, Y. H. (Y. H.), Yu, Y. M. (Y. M.), Yu, Z. Q. (Z. Q.), Zannoni, M. (M.), Zhang, C. (C.), Zhang, F. (F.), Zhang, F. Z. (F. Z.), Zhang, J. (J.), Zhang, J. H. (J. H.), Zhang, Z. (Z.), Zhao, F. (F.), Zheng, C. (C.), Zheng, Z. M. (Z. M.), Zhuang, H. L. (H. L.), Zhukov, V. (V.), Zichichi, A. (A.), Zuccon, P. (P.), Aguilar, M. (M.), Cavasonza, L. A. (L. Ali), Alpat, B. (B.), Ambrosi, G. (G.), Arruda, L. (L.), Attig, N. (N.), Bagwell, C. (C.), Barao, F. (F.), Barrin, L. (L.), Bartoloni, A. (A.), Basegmez-du Pree, S. (S.), Battiston, R. (R.), Belyaev, N. (N.), Berdugo, J. (J.), Bertucci, B. (B.), Bindi, V. (V.), Bollweg, K. (K.), Bolster, J. (J.), Borchiellini, M. (M.), Borgia, B. (B.), Boschini, M. J. (M. J.), Bourquin, M. (M.), Bueno, E. F. (E. F.), Burger, J. (J.), Burger, W. J. (W. J.), Cai, X. D. (X. D.), Capell, M. (M.), Casaus, J. (J.), Castellini, G. (G.), Cervelli, F. (F.), Chang, Y. H. (Y. H.), Chen, G. M. (G. M.), Chen, G. R. (G. R.), Chen, H. (H.), Chen, H. S. (H. S.), Chen, Y. (Y.), Cheng, L. (L.), Chou, H. Y. (H. Y.), Chouridou, S. (S.), Choutko, V. (V.), Chung, C. H. (C. H.), Clark, C. (C.), Coignet, G. (G.), Consolandi, C. (C.), Contin, A. (A.), Corti, C. (C.), Cui, Z. (Z.), Dadzie, K. (K.), Dass, A. (A.), Delgado, C. (C.), Della Torre, S. (S.), Demirkoz, M. B. (M. B.), Derome, L. (L.), Di Falco, S. (S.), Di Felice, V. (V.), Diaz, C. (C.), Dimiccoli, F. (F.), von Doetinchem, P. (P.), Dong, F. (F.), Donnini, F. (F.), Duranti, M. (M.), Egorov, A. (A.), Eline, A. (A.), Faldi, F. (F.), Feng, J. (J.), Fiandrini, E. (E.), Fisher, P. (P.), Formato, V. (V.), Gamez, C. (C.), Garcia-Lopez, R. J. (R. J.), Gargiulo, C. (C.), Gast, H. (H.), Gervasi, M. (M.), Giovacchini, F. (F.), Gomez-Coral, D. M. (D. M.), Gong, J. (J.), Goy, C. (C.), Grabski, V. (V.), Grandi, D. (D.), Graziani, M. (M.), Guracho, A. N. (A. N.), Haino, S. (S.), Han, K. C. (K. C.), Hashmani, R. K. (R. K.), He, Z. H. (Z. H.), Heber, B. (B.), Hsieh, T. H. (T. H.), Hu, J. Y. (J. Y.), Huang, B. W. (B. W.), Incagli, M. (M.), Jang, W. Y. (W. Y.), Jia, Y. (Yi), Jinchi, H. (H.), Karagoz, G. (G.), Khiali, B. (B.), Kim, G. N. (G. N.), Kirn, T. (Th.), Kounina, O. (O.), Kounine, A. (A.), Koutsenko, V. (V.), Krasnopevtsev, D. (D.), Kuhlman, A. (A.), Kulemzin, A. (A.), La Vacca, G. (G.), Laudi, E. (E.), Laurenti, G. (G.), LaVecchia, G. (G.), Lazzizzera, I. (I.), Lee, H. T. (H. T.), Lee, S. C. (S. C.), Li, H. L. (H. L.), Li, J. Q. (J. Q.), Li, M. (M.), Li, Q. (Q.), Li, Q. Y. (Q. Y.), Li, S. (S.), Li, S. L. (S. L.), Li, J. H. (J. H.), Li, Z. H. (Z. H.), Liang, J. (J.), Liang, M. J. (M. J.), Lin, C. H. (C. H.), Lippert, T. (T.), Liu, J. H. (J. H.), Lu, S. Q. (S. Q.), Lu, Y. S. (Y. S.), Luebelsmeyer, K. (K.), Luo, J. Z. (J. Z.), Luo, S. D. (S. D.), Luo, X. (Xi), Machate, F. (F.), Mana, C. (C.), Marin, J. (J.), Marquardt, J. (J.), Martin, T. (T.), Martinez, G. (G.), Masi, N. (N.), Maurin, D. (D.), Medvedeva, T. (T.), Menchaca-Rocha, A. (A.), Meng, Q. (Q.), Mikhailov, V. V. (V. V.), Molero, M. (M.), Mott, P. (P.), Mussolin, L. (L.), Negrete, J. (J.), Nikonov, N. (N.), Nozzoli, F. (F.), Ocampo-Peleteiro, J. (J.), Oliva, A. (A.), Orcinha, M. (M.), Ottupara, M. A. (M. A.), Palermo, M. (M.), Palmonari, F. (F.), Paniccia, M. (M.), Pashnin, A. (A.), Pauluzzi, M. (M.), Pensotti, S. (S.), Plyaskin, V. (V.), Poluianov, S. (Stepan), Qin, X. (X.), Qu, Z. Y. (Z. Y.), Quadrani, L. (L.), Rancoita, P. G. (P. G.), Rapin, D. (D.), Conde, A. R. (A. Reina), Robyn, E. (E.), Romaneehsen, L. (L.), Rozhkov, A. (A.), Rozza, D. (D.), Sagdeev, R. (R.), Schael, S. (S.), von Dratzig, A. S. (A. Schultz), Schwering, G. (G.), Seo, E. S. (E. S.), Shan, B. S. (B. S.), Siedenburg, T. (T.), Song, J. W. (J. W.), Song, X. J. (X. J.), Sonnabend, R. (R.), Strigari, L. (L.), Su, T. (T.), Sun, Q. (Q.), Sun, Z. T. (Z. T.), Tacconi, M. (M.), Tang, X. W. (X. W.), Tang, Z. C. (Z. C.), Tian, J. (J.), Tian, Y. (Y.), Ting, S. C. (Samuel C. C.), Urban, T. (T.), Usoskin, I. (Ilya), Vagelli, V. (V.), Vainio, R. (R.), Valencia-Otero, M. (M.), Valente, E. (E.), Valtonen, E. (E.), Acosta, M. V. (M. Vazquez), Vecchi, M. (M.), Velasco, M. (M.), Vialle, J. P. (J. P.), Wang, C. X. (C. X.), Wang, L. (L.), Wang, L. Q. (L. Q.), Wang, N. H. (N. H.), Wang, Q. L. (Q. L.), Wang, S. (S.), Wang, X. (X.), Wang, Y. (Yu), Wang, Z. M. (Z. M.), Wei, J. (J.), Weng, Z. L. (Z. L.), Wu, H. (H.), Wu, Y. (Y.), Xiao, J. N. (J. N.), Xiong, R. Q. (R. Q.), Xiong, X. Z. (X. Z.), Xu, W. (W.), Yan, Q. (Q.), Yang, H. T. (H. T.), Yang, Y. (Y.), Yashin, I. I. (I. I.), Yelland, A. (A.), Yi, H. (H.), You, Y. H. (Y. H.), Yu, Y. M. (Y. M.), Yu, Z. Q. (Z. Q.), Zannoni, M. (M.), Zhang, C. (C.), Zhang, F. (F.), Zhang, F. Z. (F. Z.), Zhang, J. (J.), Zhang, J. H. (J. H.), Zhang, Z. (Z.), Zhao, F. (F.), Zheng, C. (C.), Zheng, Z. M. (Z. M.), Zhuang, H. L. (H. L.), Zhukov, V. (V.), Zichichi, A. (A.), and Zuccon, P. (P.)
Abstract: We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38 x 10⁶ sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167 ± 0.006, for Ne/Si is 0.833 ± 0.025, for Mg/Si is 0.994 ± 0.029, and for C/O is 0.836 ± 0.025. These values are determined independent of cosmic-ray propagation.
Published: 2023

50. Injury and death of various Salmonella serotypes due to acidic conditions

Author: Cox, N.A., Richardson, K.E., Cosby, D.E., Berrang, M.E., Cason, J.A., Rigsby, L.L., Holcombe, N., and DeRome, L.
Published: 2016
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