Measurement of charge changing and isotopic cross sections at ∼600 MeV/nucleon from the interactions of ∼30 separate beams of relativistic nuclei from<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>10</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">B</mml:mi></mml:math>to<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>55</mml:mn></mml:

Webber, W. R.; Soutoul, A.; Kish, J. C.; Rockstroh, J. M.; Cassagnou, Y.; Légrain, R.; Testard, O.

doi:10.1103/physrevc.58.3539

Cited by 45 publications

(41 citation statements)

References 17 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…2D histograms of the relative differences between various semi-empirical models currently used to calculate the production cross-sections σ b→a . Our reference model is Webber et al (2003) (Webber 03), and we compare it to the parameterisations from Webber et al (1990) (Webber 93), Webber et al (1998) (Webber 98) and Silberberg et al (1998) (S&T 00). The charges of the parent and child nuclei are given on the vertical and horizontal axes, respectively.…”

Section: Cross-section Modellingmentioning

confidence: 99%

“…Multiplying σ b→B by a factor κ while rescaling σ B Notes. The reference model used in our calculations of the fluxes is adapted from Webber et al (2003) (Webber 03) and is compared to previous releases by Webber et al (1990) (Webber 93) and Webber et al (1998) (Webber 98) as well as to the work from Silberberg et al (1998) (S&T 00). The dominant production channels, which involve the stable isotopes of carbon, nitrogen, and oxygen, are listed in boldface.…”

Section: Cross-section Modellingmentioning

confidence: 99%

“…For the production cross-sections σ b→a , one may chose between the semi-empirical approach proposed by Silberberg et al (1998), subsequently revised in 2000 and called here S&T 00, and the parameterisation provided by Webber et al (1990, hereafter Webber 93) and its updates of 1998 (Webber et al 1998) and 2003 (Webber et al 2003). We selected the last set of values as our reference model, to which we have compared the other parameterisations to gauge the uncertainties that affect, on average, the values of σ b→a .…”

Section: Cross-section Modellingmentioning

confidence: 99%

See 2 more Smart Citations

Theoretical uncertainties in extracting cosmic-ray diffusion parameters: the boron-to-carbon ratio

Génolini

Putze

Salati

et al. 2015

A&A

View full text Add to dashboard Cite

Context. PAMELA and, more recently, AMS-02, are ushering us into a new era of greatly reduced statistical uncertainties in experimental measurements of cosmic-ray fluxes. In particular, new determinations of traditional diagnostic tools such as the boron-tocarbon ratio (B/C) are expected to significantly reduce errors on cosmic-ray diffusion parameters, with important implications for astroparticle physics, ranging from inferring primary source spectra to indirect dark matter searches. Aims. It is timely to stress, however, that the conclusions obtained crucially depend on the framework in which the data are interpreted as well as on some nuclear input parameters. We aim at assessing the theoretical uncertainties affecting the outcome, with models as simple as possible while still retaining the key dependencies. Methods. We compared different semi-analytical, two-zone model descriptions of cosmic-ray transport in the Galaxy: infinite slab(1D), cylindrical symmetry (2D) with homogeneous sources, cylindrical symmetry (2D) with inhomogeneous source distribution. We tested for the effect of a primary source contamination in the boron flux by parametrically altering its flux. We also tested for nuclear cross-section uncertainties. All hypotheses were compared by χ 2 minimisation techniques to preliminary results from AMS-02. Results. We find that the main theoretical bias on the determination of the diffusion coefficient index δ (up to a factor two) is represented by the assumption that no injection of boron takes place at the source. The next most important uncertainty is represented by cross-section uncertainties, which reach ±20% in δ. As a comparison, nuclear uncertainties are more important than the shift in the best-fit when introducing a convective wind of velocity 30 km s −1 , with respect to a pure diffusive baseline model. Perhaps surprisingly, homogeneous 1D vs. 2D performances are similar in determining diffusion parameters. An inhomogeneous source distribution marginally alters the central value of the diffusion coefficient normalisation (at the 10%, 1σ level). However, the index of the diffusion coefficient δ is basically unaltered, as well as the goodness of fit. Conclusions. Our study suggests that, differently for instance from the leptonic case, realistic modelling of the geometry of the Galaxy and of the source distribution are of minor importance to correctly reproduce B/C data at high energies and thus, to a large extent, for the extraction of diffusion parameters. The ansatz on the lack of primary injection of boron represents the most serious bias and requires multi-messenger studies to be addressed. If this uncertainty could be lifted, nuclear uncertainties would still represent a serious concern; they degrade the systematic error on the inferred parameters to the 20% level, or three times the estimated experimental sensitivity. To reduce this, a new nuclear cross-section measurement campaign might be required.

show abstract

Section: Cross-section Modellingmentioning

confidence: 99%

Section: Cross-section Modellingmentioning

confidence: 99%

Section: Cross-section Modellingmentioning

confidence: 99%

See 1 more Smart Citation

Theoretical uncertainties in extracting cosmic-ray diffusion parameters: the boron-to-carbon ratio

Génolini

Putze

Salati

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…The third column of Table 1 Ni(p,2p) 59 Co were provided by W. R. Webber (1998, private communication). These values were obtained by extrapolating from recently measured cross sections for (p, pn) and (p, 2p) fragmentation of the nuclides 56 Fe (Webber et al 1998a) and 52 Cr (Webber et al 1998b) which, like 60 Ni, have four more neutrons than protons. At 600 MeV nucleon Ϫ1 the estimated cross sections for producing 59 Ni and 59 Co are 68 and 40 mbarn, respectively.…”

Section: Transport Calculationmentioning

confidence: 99%

Constraints on the Time Delay between Nucleosynthesis and Cosmic-Ray Acceleration from Observations of [TSUP]59[/TSUP]N[CLC]i[/CLC] and [TSUP]59[/TSUP]C[CLC]o[/CLC]

Wiedenbeck

Binns

Christian

et al. 1999

The Astrophysical Journal

101

View full text Add to dashboard Cite

Measurements of the abundances of cosmic-ray 59 Ni and 59 Co are reported from the Cosmic-Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer. These nuclides form a parent-daughter pair in a radioactive decay which can occur only by electron capture. This decay cannot occur once the nuclei are accelerated to high energies and stripped of their electrons. The CRIS data indicate that the decay of 59 Ni to 59 Co has occurred, leading to the conclusion that a time longer than the yr half-life of 59 Ni elapsed before the particles 4 7.6 # 10 were accelerated. Such long delays indicate the acceleration of old, stellar or interstellar material rather than fresh supernova ejecta. For cosmic-ray source material to have the composition of supernova ejecta would require that these ejecta not undergo significant mixing with normal interstellar gas before ∼10 5 yr has elapsed.

show abstract

“…Extensive experimental data [1][2][3][4] on the charge changing cross sections for several nuclei near the ␤ stability line exist in the literature. The currently available radioactive ion beam facilities help to produce, accelerate, and then use the beams of these radioactive nuclei as projectiles in further experimentation.…”

Section: Introductionmentioning

confidence: 99%

Microscopic investigations of mass and charge changing cross sections

Bhagwat

Gambhir

2004

Phys. Rev. C

View full text Add to dashboard Cite

The mass and the charge changing cross sections recently measured in inverse kinematics are investigated microscopically in the framework of Glauber model using the ground state point proton/neutron densities obtained in the relativistic mean field/relativistic Hartree-Bogoliubov approach. As illustrative examples, explicit results for the nuclei spanning different regions of the periodic table, incident on 12 C, hydrogen, and −CH 2 targets are presented. The present study gives an excellent account of the experiment.

show abstract

Measurement of charge changing and isotopic cross sections at ∼600 MeV/nucleon from the interactions of ∼30 separate beams of relativistic nuclei from10Bto55

Cited by 45 publications

References 17 publications

Theoretical uncertainties in extracting cosmic-ray diffusion parameters: the boron-to-carbon ratio

Theoretical uncertainties in extracting cosmic-ray diffusion parameters: the boron-to-carbon ratio

Constraints on the Time Delay between Nucleosynthesis and Cosmic-Ray Acceleration from Observations of [TSUP]59[/TSUP]N[CLC]i[/CLC] and [TSUP]59[/TSUP]C[CLC]o[/CLC]

Microscopic investigations of mass and charge changing cross sections

Contact Info

Product

Resources

About