Relativistic Interaction of<sup>22</sup>Ne and<sup>26</sup>Mg in Hydrogen and the Cosmic‐Ray Implications

Chen, C.‐X.; Albergo, S.; Caccia, Z.; Costa, S.; Crawford, H. J.; Cronqvist, M.; Engelage, J.; Greiner, L.; Guzik, T. G.; Insolia, A.; Knott, C. N.; Lindstrom, P. J.; McMahon, M.; Mitchell, J. W.; Potenza, R.; Russo, G.; Soutoul, A.; Testard, O.; Tull, C. E.; Tuvé, C.; Waddington, C. J.; Webber, W. R.; Wefel, J. P.

doi:10.1086/303881

Cited by 22 publications

(3 citation statements)

References 30 publications

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“…In line with recent studies, all calling for more precise nuclear data for CRs [37,48,56,57,65], we therefore stress once more the urgent need for establishing a program of cross-section measurements at the O(100 GeV) energy scale. To conclude, we would like to quote Chen et al 1997 [66] from the Transport Collaboration: "With the shutdown of the LBL Bevalac and the pending closure of the Saclay Saturne accelerators, opportunities for obtaining cross-section measurements relevant to the interpretation of CR data are rapidly dwindling worldwide. Thus, future experiments will rely heavily upon cross-section predictions, and it is important to update our formulae using data (...) to ensure that the solutions to some astrophysical problems are not dominated by cross-section inaccuracies rather than by CR measurements".…”

Section: Discussionmentioning

confidence: 99%

Solar and nuclear physics uncertainties in cosmic-ray propagation

Tomassetti

2017

Phys. Rev. D

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Recent data released by the AMS experiment on the primary spectra and secondary-to-primary ratios in cosmic rays (CRs) can pose tight constraints to astrophysical models of CR acceleration and transport in the Galaxy, thereby providing a robust baseline of the astrophysical background for dark matter search via antimatter. However, models of CR propagation are affected by other important sources of uncertainties, notably from solar modulation and nuclear fragmentation, that cannot be improved with the sole use of the AMS data. The present work is aimed at assessing these uncertainties and their relevance in the interpretation of the new AMS data on the boron-to-carbon (B/C) ratio. Uncertainties from solar modulation are estimated using improved models of CR transport in the Heliosphere constrained against various type of measurements: monthly-resolved CR data collected by balloon-born or space missions, interstellar flux data from the Voyager-1 spacecraft, and counting rates from ground-based neutron monitor detectors. Uncertainties from nuclear fragmentation are estimated using semiempirical cross-section formulae constrained by measurements on isotopically-resolved and charge-changing reactions. We found that a proper data-driven treatment of solar modulation can guarantee the desired level of precision, in comparison with the improved accuracy of the recent data on the B/C ratio. On the other hand, nuclear uncertainties represent a serious limiting factor over a wide energy range. We therefore stress the need for establishing a dedicated program of cross-section measurements at the $\mathcal{O}$(100 GeV) energy scale.Comment: 15 pages, 10 figures, 3 tables - matches published versio

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Section: Discussionmentioning

confidence: 99%

Solar and nuclear physics uncertainties in cosmic-ray propagation

Tomassetti

2017

Phys. Rev. D

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“…This includes the new primary cross sections in hydrogen targets for C through Ni at 600 MeV nucleon~1 as described in Webber et al (1998aWebber et al ( , 1998b, as well as the hydrogen cross sections for essentially all of the secondary nuclei from Li through Mn also at 600 MeV nucleon~1 reported in Webber et al (1998c). The energy dependence of these isotopic cross sections is updated and extended as well, using our earlier charge changing cross sections measured between 300 and 1700 MeV nucleon~1 (Webber et al 1990) and at 15 GeV nucleon~1 (Webber et al 1994) and assuming that the isotopic fractions are generally independent of energy as conÐrmed by these earlier measurements and those of the Transport Collaboration (Chen et al 1997). …”

Section: Cross Sectionsmentioning

confidence: 99%

The Modified Weighted Slab Technique: Models and Results

Jones

Lukasiak

Птускин

et al. 2001

ApJ

184

222

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In an attempt to understand the source and propagation of Galactic cosmic rays, we have employed the modiÐed weighted slab technique along with recent values of the relevant cross sections to compute primary to secondary ratios including B/C and sub-Fe/Fe for di †erent Galactic propagation models. The models that we have considered are the disk-halo di †usion model, the dynamical halo wind model, the turbulent di †usion model, and a model with minimal reacceleration. The modiÐed weighted slab technique will be brieÑy discussed and a more detailed description of the models will be given. We will also discuss the impact that the various models have on the problem of anisotropy at high energy and discuss what properties of a particular model bear on this issue. Subject headings : cosmic rays È di †usion È magnetic Ðelds È shock waves THE APPLICATION OF THE MODIFIED WEIGHTED SLAB TECHNIQUE TO SIMPLIFIED MODELSThe weighted slab technique has long been used in studying the propagation of cosmic rays in the Galaxy from their points of origin to their observation points near the Earth (Davis 1960 ;Ginzburg & Syrovatskii 1964 ;Ginzburg & Ptuskin 1976 ;Lezniak 1979 ; also see Webber 1997). Several approximations are used in deriving this technique, among them the assumption that energy loss and/or gain is not signiÐcant and that the propagation in, and loss from, the Galaxy may be described by a function of energy per nucleon alone. Both of these simpliÐcations are known to be untrue : for low energies, ionization energy loss can be signiÐcant and rigidity, or energy per charge, is believed to be the parameter that best describes propagation.Ptuskin, Jones, & Ormes (1996) showed how the weighted slab technique could be made exact for Galactic propagation models in which energy gains and losses were proportional to the same mass density that determined nuclear fragmentation and time-dependent processes, e.g., radioactive decay, do not play a role. This modiÐcation allows for the fact that particles had di †erent (usually higher) energies in the past, and hence di †erent propagation properties, and that propagation is considered to be a function of rigidity, although energy per nucleon is the proper parameter for nuclear fragmentation calculations. Strictly, this technique is rigorous only for models in which the particle propagation parameters are proportional to a single function of energy for each particle species, and hence does not apply to Galactic wind models or turbulent di †usion models. However, most of these models may be closely approximated by simpliÐed homogeneous models in which the mean path length has an exponential distribution with a mean path length that is a particular function of rigidity. It is models of this type and approximation that we discuss in this study. In this paper we present some results of the numerical simulations where the most recent set of spallation cross sections were used.It should be noted that these models bear a similarity to the well-known leaky-box model in that they a...

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“…At the end of the 1980s, several CR and particle physicists gathered in the so-called "Transport Collaboration" [46], proposing a dedicated program focused on, but not restricted to, data from Z < 26 beams. A significant effort was made by Bill Webber and his colleagues, who measured a number of isotopic production cross sections using secondary ion beams on liquid hydrogen, carbon, and methylene CH 2 targets (and using a CH 2 -C subtraction technique) in the energy range ∼400-800 MeV/n [47][48][49][50][51][52][53][54][55][56][57][58][59]. The cross sections measured by the members of the Transport Collaboration and assembled from the literature along with the existing at that time semiempirical codes (WNEW and YIELDX [52,60,61]) were made available to the community through a dedicated web-site.…”

Section: Introductionmentioning

confidence: 99%

Current status and desired precision of the isotopic production cross sections relevant to astrophysics of cosmic rays: Li, Be, B, C, and N

et al. 2018

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The accuracy of the current generation of cosmic-ray (CR) experiments, such as AMS-02, PAMELA, CALET, and ISS-CREAM, is now reaching ∼1-3% in a wide range in energy per nucleon from GeV/n to multi-TeV/n. Their correct interpretation could potentially lead to discoveries of new physics and subtle effects that were unthinkable just a decade ago. However, a major obstacle in doing so is the current uncertainty in the isotopic production cross sections that can be as high as 20-50% or even larger in some cases. While there is a recently reached consensus in the astrophysics community that new measurements of cross sections are desirable, no attempt to evaluate the importance of particular reaction channels and their required accuracy has been made yet. It is, however, clear that it is a huge work that requires an incremental approach. The goal of this study is to provide the ranking of the isotopic cross sections contributing to the production of the most astrophysically important CR Li, Be, B, C, and N species. In this paper, we (i) rank the reaction channels by their importance for a production of a particular isotope, (ii) provide comparisons plots between the models and data used, and (iii) evaluate a generic beam time necessary to reach a 3% precision in the production cross-sections pertinent to the AMS-02 experiment. This first roadmap may become a starting point in the planning of new measurement campaigns that could be carried out in several nuclear and/or particle physics facilities around the world. A comprehensive evaluation of other isotopes Z ≤ 30 will be a subject of follow-up studies.

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Relativistic Interaction of²²Ne and²⁶Mg in Hydrogen and the Cosmic‐Ray Implications

Cited by 22 publications

References 30 publications

Solar and nuclear physics uncertainties in cosmic-ray propagation

Solar and nuclear physics uncertainties in cosmic-ray propagation

The Modified Weighted Slab Technique: Models and Results

Current status and desired precision of the isotopic production cross sections relevant to astrophysics of cosmic rays: Li, Be, B, C, and N

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Relativistic Interaction of22Ne and26Mg in Hydrogen and the Cosmic‐Ray Implications

Cited by 22 publications

References 30 publications

Solar and nuclear physics uncertainties in cosmic-ray propagation

Solar and nuclear physics uncertainties in cosmic-ray propagation

The Modified Weighted Slab Technique: Models and Results

Current status and desired precision of the isotopic production cross sections relevant to astrophysics of cosmic rays: Li, Be, B, C, and N

Contact Info

Product

Resources

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Relativistic Interaction of²²Ne and²⁶Mg in Hydrogen and the Cosmic‐Ray Implications