Observation of New Properties of Secondary Cosmic Rays Lithium, Beryllium, and Boron by the Alpha Magnetic Spectrometer on the International Space Station

Aguilar, M.; Cavasonza, L. Ali; 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; 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.; 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.; Palermo, 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.; 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.120.021101

Cited by 239 publications

(260 citation statements)

References 41 publications

(73 reference statements)

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“…Other discrepancies, such as those reported in Figure 5 for beryllium, boron, and nitrogen when comparing to the HEAO-3 data (Engelmann et al 1990), are an indication of the systematic uncertainties of the instrument. This is demonstrated by the excellent agreement of spectra of boron and nitrogen with AMS-02 data (Aguilar et al 2018b) in the whole energy range from 2 GV -2 TV.…”

Section: Spectral Parametersmentioning

confidence: 53%

“…For our case this means that there is a source of primary lithium and that this lithium may be observed in CRs for the first time, thanks to the high statistics and precision achieved by the AMS-02 experiment (Aguilar et al 2018b). Though the absolute mass of lithium produced by novae is relatively small, the lithium abundance of the ejecta is comparable to that found in CRs given that the total mass of the ejecta is 10 −5 M − 10 −4 M .…”

Section: Lithium Anomalymentioning

confidence: 77%

“…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%

“…Our model calculations of CR lithium (in the I-scenario) as compared to the AMS-02 data(Aguilar et al 2018b). Black dot-dashed line shows only secondary component.…”

mentioning

confidence: 99%

See 3 more Smart Citations

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.

show abstract

Section: Spectral Parametersmentioning

confidence: 53%

Section: Lithium Anomalymentioning

confidence: 77%

Section: Scenarios Of a Spectral Break At 300 Gvmentioning

confidence: 81%

“…Our model calculations of CR lithium (in the I-scenario) as compared to the AMS-02 data(Aguilar et al 2018b). Black dot-dashed line shows only secondary component.…”

mentioning

confidence: 99%

See 2 more Smart Citations

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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“…The resulting level of field amplification and, as a consequence, the resulting maximum achievable energy, depends on the efficiency of particle acceleration and on the particle spectrum . Recent evidence suggests that the latter must be steep: this inference comes both from gamma-ray observations of SNRs and from models of CR propagation through the Galaxy, supplied with the findings by AMS-02 (Aguilar et al 2016(Aguilar et al , 2018 about the slope of the diffusion coefficient (see e.g. Amato and Blasi (2018) for a review).…”

Section: Unveiling the Nature Of The Main Sources Of Crs In The Galaxymentioning

confidence: 99%

High-Energy Particles and Radiation in Star-Forming Regions

et al. 2020

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Non-thermal particles and high-energy radiation can play a role in the dynamical processes in star-forming regions and provide an important piece of the multiwavelength observational picture of their structure and components. Powerful stellar winds and supernovae in compact clusters of massive stars and OB associations are known to be favourable sites of high-energy particle acceleration and sources of non-thermal radiation and neutrinos. Namely, young massive stellar clusters are likely sources of the PeV (petaelectronvolt) regime cosmic rays (CRs). They can also be responsible for the cosmic ray composition, e.g., 22 Ne/ 20 Ne anomalous isotopic ratio in CRs. Efficient particle acceleration can be accompanied by super-adiabatic amplification of the fluctuating magnetic fields in the systems converting a part of kinetic power of the winds and supernovae into the magnetic energy through the CR-driven instabilities. The escape and CR propagation in the vicinity of the sources are affected by the non-linear CR feedback. These effects are expected to be important in starburst galaxies, which produce high-energy neutrinos and gamma-rays. We give a brief review of the theoreti-A. M. Bykov

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No room to hide: implications of cosmic-ray upscattering for GeV-scale dark matter

Alvey

Bringmann

Kolešová

2023

J. High Energ. Phys.

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The irreducible upscattering of cold dark matter by cosmic rays opens up the intriguing possibility of detecting even light dark matter in conventional direct detection experiments or underground neutrino detectors. The mechanism also significantly enhances sensitivity to models with very large nuclear scattering rates, where the atmosphere and rock overburden efficiently stop standard non-relativistic dark matter particles before they could reach the detector. In this article, we demonstrate that cosmic-ray upscattering essentially closes the window for strongly interacting dark matter in the (sub-)GeV mass range. Arriving at this conclusion crucially requires a detailed treatment of both nuclear form factors and inelastic dark matter-nucleus scattering, as well as including the full momentum-transfer dependence of scattering amplitudes. We illustrate the latter point by considering three generic situations where such a momentum-dependence is particularly relevant, namely for interactions dominated by the exchange of light vector or scalar mediators, respectively, and for dark matter particles of finite size. As a final concrete example, we apply our analysis to a putative hexaquark state, which has been suggested as a viable baryonic dark matter candidate. Once again, we find that the updated constraints derived in this work close a significant part of otherwise unconstrained parameter space.

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Observation of New Properties of Secondary Cosmic Rays Lithium, Beryllium, and Boron by the Alpha Magnetic Spectrometer on the International Space Station

Cited by 239 publications

References 41 publications

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

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

High-Energy Particles and Radiation in Star-Forming Regions

No room to hide: implications of cosmic-ray upscattering for GeV-scale dark matter

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