Observation of the Identical Rigidity Dependence of He, C, and O Cosmic Rays at High Rigidities by the Alpha Magnetic Spectrometer on the International Space Station

Aguilar, M.; Cavasonza, L. Ali; Alpat, B.; Ambrosi, G.; Arruda, L.; Attig, N.; Aupetit, S.; Azzarello, P.; Bachlechner, A.; Barão, F.; Barrau, A.; Barrin, L.; Bartoloni, Alessandro; Basara, L.; Pree, Seth; Battarbee, Markus; Battiston, R.; Becker, U.; Behlmann, M.; Beischer, B.; Berdugo, J.; Bertucci, B.; Bindel, K. F.; Bindi, V.; Boer, W. De; Bollweg, K.; Bonnivard, V.; Borgia, B.; Boschini, M.; Bourquin, M.; Bueno, E. F.; Burger, J. D.; Burger, W. J.; Cadoux, F.; Cai, Xudong; Capell, M.; Caroff, S.; Casaus, J.; Castellini, G.; Cervelli, F.; Chae, M. J.; Chang, Y. H.; Chen, A. I.; Chen, G. M.; Chen, H. S.; Cheng, Lin; Chou, H. Y.; Choumilov, E.; Choutko, V.; Chung, C. H.; Clark, C. H. Douglas; Clavero, R.; Coignet, G.; Consolandi, C.; Contin, A.; Corti, C.; Creus, W.; Crispoltoni, M.; Cui, Z.; Dadzie, K.; Dai, Ye; Datta, A.; Mendez, C. Delgado; Torre, S. Della; Demakov, O.; Demirköz, B.; Derome, L.; Falco, S. Di; Dimiccoli, F.; Díaz, C.; Doetinchem, P. von; Dong, Fang; Donnini, F.; Duranti, M.; D’Urso, D.; Egorov, A.; Eline, A.; Eronen, T.; Feng, J. H.; Fiandrini, E.; Fisher, P. H.; Formato, V.; Galaktionov, Yu.; Gallucci, G.; García-López, R. J.; Gargiulo, C.; Gast, H.; Gebauer, I.; Gervasi, M.; Ghelfi, A.; Giovacchini, F.; Gómez-Coral, D. M.; Gong, J.; Goy, C.; Grabski, V.; Grandi, D.; Graziani, M.; Guo, Kexin; Haino, S.; Han, K.; He, Z. H.; Heil, M.; Hoffman, J.; Hsieh, Timothy H.; Huang, Hai; Huang, Z. C.; Huh, C.; Incagli, M.; Ionica, M.; Jang, W. Y.; Jia, Yi; Jinchi, H.; Kang, Sinchul; Kanishev, K.; Khiali, B.; Kim, G. N.; Kim, K. S.; Kirn, T.; Koňák, Čestmı́r; Kounina, O.; Kounine, A.; Koutsenko, V.; Kulemzin, A.; Vacca, G. La; Laudi, E.; Laurenti, G.; Lazzizzera, I.; Lebedev, A.; Lee, H. T.; Lee, S. C.; Leluc, C.; Li, H. S.; Li, J. Q.; Li, Q.; Li, T. X.; Li, Y.; Li, Z. H.; Li, Z. Y.; Lim, S. I.; Lin, Chao-Hung; Lipari, P.; Lippert, Th.; Liu, D.; Liu, Hu; Lordello, V. D.; Lu, S. Q.; Lu, Yao; Luebelsmeyer, K.; Luo, Feng; Luo, Junzhou; Lyu, Shaoyu; Machate, F.; Mañá, C.; Marín, J.; Martin, Thierry; Martínez, G.; Masi, N.; Maurin, D.; Menchaca‐Rocha, A.; Meng, Qiao; Mikuni, V. M.; Mo, Dong-Chuan; Mott, P. H.; Nelson, T. K.; Ni, Jiangqun; Nikonov, N.; Nozzoli, F.; Oliva, A.; Orcinha, M.; Palmonari, F.; Palomares, C.; Paniccia, M.; Pauluzzi, M.; Pensotti, S.; Perrina, C.; Phan, H. D.; Picot-Clémente, N.; Pilo, F.; Pizzolotto, C.; Plyaskin, V.; Pohl, M.; Poireau, V.; Quadrani, L.; Qi, X. M.; Qin, X.; Qu, Z. Y.; Räihä, T. S.; Rancoita, P. G.; Rapin, D.; Ricol, J. S.; Rosier‐Lees, S.; Rozhkov, A.; Rozza, D.; Sagdeev, R. Z.; Schael, S.; Schmidt, Susann; Dratzig, A. Schulz von; Schwering, G.; Seo, E. S.; Shan, B. S.; Shi, J. Y.; Siedenburg, T.; Son, D. C.; Song, Jiwei; Tacconi, M.; Tang, X.; Tang, Zhicheng; Tescaro, D.; Ting, Samuel C.C.; Ting, S. M.; Tomassetti, Nicola; Torsti, J.; Türkoğlu, C.; Urban, T.; Vagelli, V.; Valente, E.; Валтонен, Э.; Acosta, Mónica Vázquez; Vecchi, M.; Velasco, M.; Vialle, J. P.; Vitale, V.; Vitillo, S.; Wang, L. Q.; Wang, N. H.; Wang, Q. L.; Wang, X.; Wang, X. Q.; Wang, Z. X.; Wei, Chuncheng; Weng, Z.; Whitman, K.; Wu, H. R.; Wu, X.; Xiong, R. Q.; Xu, W.; Yan, Qi; Yang, Jiawei; Yang, Min; Yang, Y.; Han, Yi; Yu, Yongji; Yu, Zhao-Huan; Zannoni, M.; Zeissler, S.; Zhang, C.; Zhang, F.; Zhang, J.; Zhang, J. H.; Zhang, S. W.; Zhang, Z.; Zheng, Z. M.; Zhuang, H. L.; Жуков, В.; Zichichi, A.; Zimmermann, N.; Zuccon, P.

doi:10.1103/physrevlett.119.251101

Cited by 278 publications

(276 citation statements)

References 54 publications

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“…15 −0.10 . There is clear evidence that the hardening is also present in the spectra of helium and other primary nuclei [2,4,22], and the results are consistent with the hypothesis that the feature has a "universal" shape when studied as a function of rigidity (even if the values of the slopes of different particle types are not equal).…”

Section: Discussionsupporting

confidence: 70%

The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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Recent observations of cosmic ray protons in the energy range 10 2 -10 5 GeV have revealed that the spectrum cannot be described by a simple power law. A hardening of the spectrum around an energy of order few hundred GeV, first observed by the magnetic spectrometers PAMELA and AMS02, has now been confirmed by several calorimeter detectors (ATIC, CREAM, CALET, NUCLEON and DAMPE). These new measurements reach higher energy and indicate that the hardening corresponds to a larger step in spectral index than what estimated by the magnetic spectrometers. Data at still higher energy (by CREAM, NUCLEON and DAMPE) show that the proton spectrum undergoes a marked softening at E ≈ 10 4 GeV. Understanding the origin of these unexpected spectral features is a significant challenge for models of the Galactic cosmic rays. An important open question is whether additional features are present in the proton spectrum between the softening and the "Knee". Extensive Air Shower detectors, using unfolding procedures that require the modeling of cosmic ray showers in the atmosphere, estimated the proton flux below and around the Knee (at E 3 PeV). These results however have large systematic uncertainties and are in poor agreement with each other. The measurement in the PeV energy range, recently presented by IceTop/IceCube, indicates a proton flux higher than extrapolations of the direct measurements calculated assuming a constant slope, and therefore requires the existence of an additional spectral hardening below the Knee. A clarification of this point is very important for an understanding of the origin of the Galactic cosmic rays, and is also essential for a precise calculation of the spectra of atmospheric neutrinos in the energy range (E 10 TeV) where they constitute the foreground for the emerging astrophysical ν signal.

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Section: Discussionsupporting

confidence: 70%

The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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“…A subsequent release of the spectra of other primary and secondary species by AMS-02 was eagerly awaited. First, AMS-02 confirmed a clear distinction in the rigidity dependencies between the groups of mostly primary nuclei, He, C, O (Aguilar et al 2017), and secondary nuclei, Li, Be, B (Aguilar et al 2018b), while the nuclei within each group have similar spectra. Nitrogen that is half-primary/halfsecondary fell in between (Aguilar et al 2018c).…”

Section: Scenarios Of a Spectral Break At 300 Gvmentioning

confidence: 81%

“…Recent observation of blue-shifted absorption lines of partly ionized 7 Be in the spectrum of a classical nova V339 Del about 40-50 days after the explosion (Tajitsu et al 2015) is the first observational evidence that the mechanism proposed in 1970s is working indeed (Hernanz 2015). The (Aguilar et al 2017). The experimental data points for carbon are shown by violet triangles, and for oxygen by red diamonds.…”

Section: Lithium Anomalymentioning

confidence: 92%

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

Boschini

Torre

Gervasi

et al. 2020

ApJ

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Local interstellar spectra (LIS) of secondary cosmic ray (CR) nuclei, lithium, beryllium, boron, and partially secondary nitrogen, are derived in the rigidity range from 10 MV to ∼200 TV using the most recent experimental results combined with the state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. The lithium spectrum appears somewhat flatter at high energies compared to other secondary species that may imply a primary lithium component. Two propagation packages, GALPROP and HELMOD, are combined to provide a single framework that is run to reproduce direct measurements of CR species at different modulation levels, and at both polarities of the solar magnetic field. An iterative maximum-likelihood method is developed that uses GALPROP-predicted LIS as input to HELMOD, which provides the modulated spectra for specific time periods of the selected experiments for the model-data comparison. The proposed LIS accommodate the low-energy interstellar spectra measured by Voyager 1, HEAO-3, and ACE/CRIS as well as the high-energy observations by PAMELA, AMS-02, and earlier experiments that are made deep in the heliosphere. The interstellar and heliospheric propagation parameters derived in this study are consistent with our earlier results for propagation of CR protons, helium, carbon, oxygen, antiprotons, and electrons.

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“…In this section we present our results obtained through a single multi-variate fitting procedure to compare AMS-02 experimental data with theoretical spectra computed as discussed in the previous sections. For each value of the halo half-thickness H we minimise the χ 2 with respect to the AMS-02 data on Be/C, B/C and Be/B [6] and C, N, O [4,47], the latter data limited to rigidities larger than 10 GV, so as to make the results only weakly dependent upon the uncertainties typical of the low energies and, most important, because as discussed in §II, the weighted slab model used here can be reliably applied to unstable isotopes only at such energies.…”

Section: A Secondary Over Primary Ratiosmentioning

confidence: 99%

AMS-02 beryllium data and its implication for cosmic ray transport

et al. 2020

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The flux of unstable secondary Cosmic Ray nuclei, produced by spallation processes in the Interstellar Medium, can be used to constrain the residence time of Cosmic Rays inside the Galaxy. Among them, 10 Be is especially useful because of its relatively long half-life of 1.39 Myr . In the framework of the diffusive halo model we describe Cosmic Ray transport taking into account all relevant interaction channels and accounting for the decay of unstable secondary nuclei. We then compare our results with the data collected by the Alpha Magnetic Spectrometer (AMS-02) on board the International Space Station for the flux ratios Be/C, B/C, C/O and Be/B as well as C and O absolute fluxes. These measurements, and especially the Be/B ratio, allow us to single out the flux of 10 Be and infer a best fit propagation time of CRs in the Galaxy. Our results show that, if the cross sections for the production of secondary elements through spallation are taken at face value, AMS-02 measurements are compatible with the standard picture based on CR diffusion in a halo of size H ∼ 3 − 6 kpc. Taking into account the uncertainties in the cross sections, this conclusion becomes less reliable, although still compatible with the standard picture. Implications of our findings for alternative models of CR transport are discussed.

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Observation of the Identical Rigidity Dependence of He, C, and O Cosmic Rays at High Rigidities by the Alpha Magnetic Spectrometer on the International Space Station

Cited by 278 publications

References 54 publications

The shape of the cosmic ray proton spectrum

The shape of the cosmic ray proton spectrum

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

AMS-02 beryllium data and its implication for cosmic ray transport

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