Direct Measurement of the Cosmic-Ray Carbon and Oxygen Spectra from 
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Adriani, O.; Akaike, Yosui; Asano, Kentaro; Asaoka, Y.; Bagliesi, M. G.; Berti, Eugenio; Bigongiari, G.; Binns, W. R.; Bongi, M.; Brogi, P.; Bruno, A.; Buckley, J. H.; Cannady, N.; Castellini, G.; Checchia, C.; Cherry, M. L.; Collazuol, G.; Ebisawa, Ken; Fuke, H.; Gonzi, S.; Guzik, T. G.; Hams, T.; Hibino, K.; Ichimura, M.; Ioka, Kunihito; Ishizaki, W.; Israel, M. H.; Kasahara, K.; Kataoka, J.; Kataoka, Ryuho; Katayose, Y.; Kato, C.; Kawanaka, Norita; Kawakubo, Y.; Kobayashi, Kazuyoshi; Kohri, Kazunori; Krawczynski, H.; Krizmanic, John F.; Link, J. T.; Maestro, P.; Marrocchesi, P. S.; Messineo, A.; Mitchell, J. W.; Miyake, Shoko; Моисеев, А. А.; Mori, M.; Mori, N.; Motz, H.; Munakata, K.; Nakahira, S.; Nishimura, Jun; Nolfo, G. A. de; Okuno, S.; Ormes, J. F.; Ospina, N.; Ozawa, S.; Pacini, Lorenzo; Palma, F.; Papini, P.; Rauch, B. F.; Ricciarini, S.; Sakai, Kazuhiro; Sakamoto, T.; Sasaki, Misao; Shimizu, Yuki; Shiomi, A.; Sparvoli, R.; Спиллантини, П.; Stolzi, Francesco; Sugita, S.; Suh, J. E.; Sulaj, A.; Takita, M.; Tamura, T.; Terasawa, T.; Torii, Shoji; Tsunesada, Y.; Uchihori, Y.; Vannuccini, E.; Wefel, J. P.; Yamaoka, K.; Yanagita, S.; Yoshida, A.; Yoshida, Kenji

doi:10.1103/physrevlett.125.251102

Cited by 46 publications

(26 citation statements)

References 44 publications

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“…At this point it is hard to draw any firm conclusion on the origin of this discrepancy, but there is a serious possibility that the problem with the Iron spectrum may be of experimental nature and that only a detailed comparison between different techniques and different analyses can unveil the source of the disagreement. It is probably useful to stress that other discrepancies would deserve the same attention, such as the marked difference between the C and O spectra of AMS-02 compared with those of PAMELA [63] and CALET [64]. At low energies the effects of nuclear fragmentation inside the ex-periment itself are rather large and for heavy elements, such as Iron, this effect requires a careful correction.…”

Section: Discussionmentioning

confidence: 99%

Intermediate mass and heavy Galactic cosmic-ray nuclei: the case of new AMS-02 measurements

Schroer,

Evoli,

Blasi

2021

Preprint

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The recent measurement of the spectra of heavy nuclei carried out with the AMS-02 experiment provided us with the most complete set of data on cosmic ray fluxes to date, and allowed us to test the standard model for the transport of these particles through the Galaxy to the finest details. We show that the parameters derived from lighter primary and secondary elements in the cosmic radiation also lead to a good description of the data on heavier nuclei, with no need to invoke different injection spectra for such nuclei, provided the whole chain of fragmentation is properly accounted for. The only exception to this finding is represented by iron nuclei, which show a very unusual trend at rigidity 100 GV. This trend reflects in a Fe/O ratio that is at odds with the results of the standard model of cosmic ray transport, and is in contradiction with data collected by HEAO, ACE-CRIS and Voyager at lower energy. We speculate on possible origins of such findings.

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Section: Discussionmentioning

confidence: 99%

Intermediate mass and heavy Galactic cosmic-ray nuclei: the case of new AMS-02 measurements

Schroer,

Evoli,

Blasi

2021

Preprint

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“…The cosmic-ray Boron-to-Carbon (secondary-to-primary) ratio has been measured up to ∼ 2 GeV/nucleon and the spectra of Carbon through Iron nuclei have been measured up to approximately 2 TeV/nucleon [27,28,29,30,31,32,33]. In order to measure the Boron-to-Carbon ratio near 500 GeV/nucleon and the spectra of cosmic-ray nuclei up to 20 TeV/nucleon on a space instrument with limited mass, where a heavy calorimeter or magnetic spectrometer is probably not feasible, a TRD with sensitivity covering the Lorentz factor range 500 < γ < 2 × 10 4 may be a viable approach.…”

Section: Numerical Examplementioning

confidence: 99%

Extending the Lorentz Factor Range and Sensitivity of Transition Radiation with Compound Radiators

Alnussirat,

Cherry

2022

Preprint

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Transition radiation detectors (TRDs) have been used to identify high-energy particles (in particular, to separate electrons from heavier particles) in accelerator experiments. In space, they have been used to identify cosmic-ray electrons and measure the energies of cosmic-ray nuclei. To date, radiators have consisted of regular configurations of foils with fixed values of foil thickness and spacing (or foam or fiber radiators with comparable average dimensions) that have operated over a relatively restricted range of Lorentz factors. In order to extend the applicability of future TRDs (for example, to identify 0.5 -3 TeV pions, kaons, and protons in the far forward region in a future accelerator experiment or to measure the energy spectrum of cosmic-ray nuclei up to 20 TeV/nucleon or higher), there is a need to increase the signal strength and extend the range of Lorentz factors that can be measured in a single detector. A possible approach is to utilize compound radiators consisting of varying radiator parameters. We discuss the case of a compound radiator and derive the yield produced in a TRD with an arbitrary configuration of foil thicknesses and spacings.

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“…Moreover, cosmic rays captured with suitable instruments on space satellites from nearby interplanetary space have been found to include several radioactive isotopes, including 14 C, 36 Cl, 26 Al, 10 Be, 59 Ni, and others. Data from satellites (Israel et al 2005(Israel et al , 2018, high-altitude balloons (Walsh et al 2019), and the space station (Adriani et al 2020) have been used to constrain the propagation, specifically the path lengths traversed, for cosmic rays, as their spallation reactions on heavier nuclei such as Fe have created these radioisotopes. For the case of 59 Ni, its detection constrains the time between ejection from its nucleosynthesis source and the acceleration to cosmic-ray energies, because 59 Ni only decays through electron capture, and thus remains stable once fully ionised in cosmic rays after acceleration (Mewaldt et al 2001;Wiedenbeck et al 2001).…”

Section: Radioactivity and Astrophysical Studiesmentioning

confidence: 99%

Radioactive isotopes in the interstellar medium

Diehl

2021

Astrophys Space Sci

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Radioactive components of the interstellar medium provide an entirely-different and new aspect to the studies of the interstellar medium. Injected from sources of nucleosynthesis, unstable nuclei decay along their trajectories. Measurements can occur through characteristic gamma rays that are emitted with the decay, or in cosmic material samples through abundances of parent and daughter isotopes as they change with decay. The dynamics and material flows within interstellar medium are thus accessible to measurement, making use of the intrinsic clock that radioactive decay provides. We describe how measurements of radioactive decay have obtained a break-through in studies of the interstellar medium, after first summarizing the characteristics of radioactivity and the sources of unstable nuclei.

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Direct Measurement of the Cosmic-Ray Carbon and Oxygen Spectra from 10 GeV/n to 2.2 T

Cited by 46 publications

References 44 publications

Intermediate mass and heavy Galactic cosmic-ray nuclei: the case of new AMS-02 measurements

Intermediate mass and heavy Galactic cosmic-ray nuclei: the case of new AMS-02 measurements

Extending the Lorentz Factor Range and Sensitivity of Transition Radiation with Compound Radiators

Radioactive isotopes in the interstellar medium

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