The elemental and isotopic composition of cosmic rays - Silicon to nickel

Young, J. S.; Freier, P. S.; Waddington, C. J.; Brewster, N. R.; Fickle, R. K.

doi:10.1086/158997

Cited by 69 publications

(31 citation statements)

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“…For 26 Al/ 27 Al, the data consist of a series of balloon flights (Webber 1982), and the ISEE-3 (Wiedenbeck 1983), Voyager (Lukasiak et al 1994), Ulysses , and ACE spacecrafts (Yanasak et al 2001). For 36 Cl/Cl, the data are from the CRISIS balloon (Young et al 1981), and from the Ulysses ) and ACE (Yanasak et al 2001) spacecrafts.…”

Section: D2 Isotopic and Elemental Ratios Of Radioactive Speciesmentioning

confidence: 99%

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

Putze

Derome

Maurin

2010

A&A

150

191

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Context. Ongoing measurements of the cosmic radiation (nuclear, electronic, and γ-ray) are providing additional insight into cosmicray physics. A comprehensive picture of these data relies on an accurate determination of the transport and source parameters of propagation models. Aims. A Markov Chain Monte Carlo method is used to obtain these parameters in a diffusion model. By measuring the B/C ratio and radioactive cosmic-ray clocks, we calculate their probability density functions, placing special emphasis on the halo size L of the Galaxy and the local underdense bubble of size r h . We also derive the mean, best-fit model parameters and 68% confidence level for the various parameters, and the envelopes of other quantities. Methods. The analysis relies on the USINE code for propagation and on a Markov Chain Monte Carlo technique previously developed by ourselves for the parameter determination. Results. The B/C analysis leads to a most probable diffusion slope δ = 0.86 +0.04 −0.04 for diffusion, convection, and reacceleration, or δ = 0.234 +0.006 −0.005 for diffusion and reacceleration. As found in previous studies, the B/C best-fit model favours the first configuration, hence pointing to a high value for δ. These results do not depend on L, and we provide simple functions to rescale the value of the transport parameters to any L. A combined fit on B/C and the isotopic ratios ( 10 Be/ 9 Be, 26 Al/ 27 Al, 36 Cl/Cl) leads to L = 8 +8 −7 kpc and r h = 120 +20 −20 pc for the best-fit model. This value for r h is consistent with direct measurements of the local interstallar medium. For the model with diffusion and reacceleration, L = 4 +1 −1 kpc and r h = 3 +70 −3 pc (consistent with zero). We vary δ, because its value is still disputed. For the model with Galactic winds, we find that between δ = 0.2 and 0.9, L varies from O(0) to O(2) if r h is forced to be 0, but it otherwise varies from O(0) to O(1) (with r h ∼ 100 pc for all δ > ∼ 0.3). The results from the elemental ratios Be/B, Al/Mg, and Cl/Ar do not allow independent checks of this picture because these data are not precise enough. Conclusions. 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 δ, and also on the presence/absence of the local underdensity damping effect on radioactive nuclei. More precise data from ongoing experiments are expected to clarify this issue.

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Section: D2 Isotopic and Elemental Ratios Of Radioactive Speciesmentioning

confidence: 99%

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

Putze

Derome

Maurin

2010

A&A

150

191

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“…10 Be (Webber et al 1973c), 36 Cl (Young et al 1981), 26 Al (Webber 1982), and 54 Mn . The CR leptons were identified in the early 60's with the first measurement of electrons -also called negatrons at that time - (Earl 1961;Meyer & Vogt 1961) and of the positron fraction (de Shong et al 1964;Hartman et al 1965;Agrinier et al 1965;Daniel & Stephens 1965b).…”

Section: Introductionmentioning

confidence: 99%

A database of charged cosmic rays

Maurin

Melot

Taillet

2014

A&A

170

161

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Aims. This paper gives a description of a new online database and associated online tools (data selection, data export, plots, etc.) for charged cosmic-ray measurements. The experimental setups (type, flight dates, techniques) from which the data originate are included in the database, along with the references to all relevant publications. Methods. The database relies on the MySQL5 engine. The web pages and queries are based on PHP, AJAX and the jquery, jquery.cluetip, jquery-ui, and table-sorter third-party libraries.Results. In this first release, we restrict ourselves to Galactic cosmic rays with Z ≤ 30 and a kinetic energy per nucleon up to a few tens of TeV/n. This corresponds to more than 200 different sub-experiments (i.e., different experiments, or data from the same experiment flying at different times) in as many publications. Conclusions. We set up a cosmic-ray database (CRDB) and provide tools to sort and visualise the data. New data can be submitted, providing the community with a collaborative tool to archive past and future cosmic-ray measurements.

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“…Öberg et al (2007) claimed that photodesorption dominates at the edge of dense clouds for small (0.1 μm) and large grains (of a few microns) and becomes comparable to the spot heating desorption inside the cloud (A v > 15). Léger et al (1985) estimated spot and impulsive (whole grain) heating desorption of about 70 molecules/cm 2 s by considering different heavy ions with Z < 28, energies between 20 and 1000 MeV/nucleon, and the abundances given by Young et al (1981).…”

Section: Astrophysical Implicationsmentioning

confidence: 99%

Laboratory simulation of heavy-ion cosmic-ray interaction with condensed CO

Duarte

Domaracka²,

Boduch³

et al. 2010

A&A

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Context. Within dense interstellar clouds, from their periphery to regions deep inside, ice mantles on dust grains are exposed to cosmic-ray irradiation. Various swift ions contribute from protons to iron in the keV to TeV energy range. Observations show that in some lines of sight condensed CO molecules are an important component of the ice. Aims. We irradiate CO ices with Ni ions of relatively high energy (50 and 537 MeV) to simulate the effects produced by fast heavy cosmic-ray ions in interstellar grain mantles. Methods. CO gas is condensed on a CsI substrate at 13 K and irradiated by 50 MeV 58 Ni 13+ and 537 MeV 64 Ni 24+ ions up to a final fluence of ≈1 × 10 13 cm −2 , at a flux of 1 × 10 9 cm −2 s −1 . The sputtering yields, the destruction rate of CO, and the rate of formation of new molecular species are measured in situ by Fourier transform infrared spectroscopy (FTIR). Results. The measured CO destruction cross-sections and sputtering yields induced by Ni ions are, respectively, (i) for 50 MeV, σ d = 1.0 × 10 −13 cm 2 and Y = 7 × 10 4 molecules/impact; (ii) for 537 MeV, σ d = 3.0 × 10 −14 cm 2 and Y = 5.85 × 10 4 molecules/impact. Based on the present and previous results, the desorption rates induced by H, Ni, and Fe ions are estimated for a wide range of energies. The contribution of the heavy ions is found to dominate over that of protons in the interstellar medium.

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The elemental and isotopic composition of cosmic rays - Silicon to nickel

Cited by 69 publications

References 0 publications

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

A database of charged cosmic rays

Laboratory simulation of heavy-ion cosmic-ray interaction with condensed CO

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