Production of residual nuclei by proton-induced reactions on C, N, O, Mg, AI and Si

Bodemann, R.; Lange, H. J.; Leya, I.; Michel, R.; Schiekel, Th.; Rösel, R.; Herpers, U.; Hofmann, Hans; Dittrich, B.; Suter, M.; Wölfli, W.; Holmqvist, B.; Condé, H.; Malmborg, Petter

doi:10.1016/0168-583x(93)95077-i

Cited by 84 publications

(38 citation statements)

References 54 publications

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“…Reedy (1989) has explicitly modeled the production by α-particles of Li from O, and of Li and B from C. In his assessment, ∼10% of the production is by α-particles in the former case, ∼25% in the latter, equivalent to scaling factors 1.11 and 1.33, respectively. Comparison of p-and α-rates for a variety of light targetproduct combinations (taken from Bodemann et al 1993 andLange et al 1995) shows α-rates to be clearly higher than prates (as expected), but quite substantial variations among different target-product combinations. For our application, we have chosen a mean scaling factor of 1.33, which corresponds to a cross-section enhancement σ(α)/σ(p) ∼2.5, i.e., approximately the ratio of the geometrical cross-sections.…”

Section: Contribution By Gcr α-Particlesmentioning

confidence: 99%

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Spallation recoil II: Xenon evidence for young SiC grains

Ott

Altmaier

Herpers

et al. 2005

Meteoritics &Amp; Planetary Science

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We have determined the recoil range of spallation xenon produced by irradiation of Ba glass targets with approximatly 1190 and approximatly 268 MeV protons, using a catcher technique, where spallation products are measured in target and catcher foils. The inferred range for (sup 126)Xe produced in silicon carbide is approximatly 0.19 µm, which implies retention of approximatly 70% for (sup 126)Xe produced in "typical" presolar silicon carbide grains of 1 µm size. Recoil loss of spallation xenon poses a significantly smaller problem than loss of the spallation neon from SiC grains. Ranges differ for the various Xe isotopes and scale approximately linearly as function of the mass difference between the target element, Ba, and the product. As a consequence, SiC grains of various sizes will have differences in spallation Xe composition. In an additional experiment at approximatly 66 MeV, where the recoil ranges of (sup 22)Na and (sup 127)Xe produced on Ba glass were determined using gamma-spectrometry, we found no evidence for recoil ranges being systematically different at this lower energy. We have used the new data to put constraints on the possible presolar age of the SiC grains analyzed for Xe by Lewis et al. (1994). Uncertainties in the composition of the approximately normal Xe component in SiC (Xe-N) constitute the most serious problem in determining an age, surpassing remaining uncertainties in Xe retention and production rate. A possible interpretation is that spallation contributions are negligible and that trapped (sup 124)Xe/(sup 126)Xe is approximatly 5% lower in Xe-N than in Q-Xe. But also for other reasonable assumptions for the (sup 124)Xe/(sup 126)Xe ratio in Xe-N (e.g., as in Q-Xe), inferred exposure ages are considerably shorter than theoretically expected lifetimes for interstellar grains. A short presolar age is in line with observations by others (appearance, grain size distribution) that indicate little processing in the interstellar medium (ISM) of surviving (crystalline) SiC. This may be due to amorphization of SiC in the ISM on a much shorter time scale than destruction, with amorphous SiC not surviving processing in the early solar system. A large supply of relatively young grains may be connected to the proposed starburst origin (Clayton 2003) for the parent stars of the mainstream SiC grains

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Section: Contribution By Gcr α-Particlesmentioning

confidence: 99%

“…This was done by standard γ-ray spectrometry at University of Cologne (e.g., Bodemann et al 1993;Schiekel et al 1996;Gloris et al 2001;and references therein). The 127 Xe activities were also rather low and of limited value.…”

Section: γ-Ray Spectrometrymentioning

confidence: 99%

Spallation recoil II: Xenon evidence for young SiC grains

Ott

Altmaier

Herpers

et al. 2005

Meteoritics &Amp; Planetary Science

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“…7 Be) reaction cross section Figure 22 shows the excitation functions of the nat C(p, 7 Be), 27 Al (p, 7 Be), and nat Si(p, 7 Be) reactions obtained from other experimental data [37,38] and from calculation results with the ISOBAR þ GEM model employed in the PHITS code. The experimental data by Bodemann and Michel et al were systematically obtained by an activation technique and are therefore reliable for the validation of our results and model calculations.…”

Section: Comparison With the (Pmentioning

confidence: 99%

Differential cross sections on fragment (2 ≤ Z ≤ 9) production for carbon, aluminum and silicon induced by tens-of-MeV protons

Hagiwara

Sanami

Oishi

et al. 2012

Journal of Nuclear Science and Technology

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The double-differential cross sections (DDXs) for the inclusive reactions producing heavy nuclei with Z ¼ 2-9 (fragments) from carbon, aluminum, and silicon targets induced by 50 and 70 MeV protons are systematically measured at several angles (308, 608, 908, and 1358) using a specially developed Bragg curve counter and the energy-time-of-flight method. The DDXs of a silicon target for the proton-induced reaction producing fragments heavier than lithium were measured for the first time. The present results are compared with past experimental data, the LA150 evaluated data by the Los Alamos group and several intranuclear cascade models (Bertini and ISOBAR), and the JAEA-version quantum molecular dynamics model (JQMD) coupled with the Generalized Evaporation Model (GEM), which are implemented in the Particle and Heavy Ion Transport code System (PHITS). The present results agree well with the past experimental data and LA150 data for a -particle production. For the fragments heavier than lithium, the present results show forward-peak angular distributions rather than isotropic ones stored in LA150. Calculations with the ISOBAR and GEM models well reproduced our experimental results except for light fragments especially in the high-energy region.

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“…Proton References: a) Bodemann et al 1993;Michel et al 1995;Schiekel et al 1996. b) Lange et al 1995.…”

Section: Radionuclidesunclassified

“…The cross sections for the production of 36 Cl by the proton-and 4 He-induced reactions were taken from Goswami et al 2001 (and the references therein). For the production of 7 Be and 10 Be, the proton-induced experimental reaction cross sections were taken from Bodemann et al (1993), Michel et al (1995), andSchiekel et al (1996), whereas the 4 He-induced reaction cross sections were taken from Lange et al (1995). The estimates of the reaction cross sections for the 3 He-induced reactions are mostly theoretical, and were taken from Lee et al (1998) and Gounelle et al (2001).…”

Section: Nuclear Reaction Cross Sectionsmentioning

confidence: 99%

Numerical simulations of the production of extinct short‐lived nuclides by magnetic flaring in the early solar system

Sahijpal

Soni

2007

Meteorit & Planetary Scien

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Abstract-Using the X-ray flare observations of low-mass protostars, we developed numerical simulations of thermal processing and irradiation of protoCAIs in the magnetic reconnection ring within the X-wind formulation. Observed X-ray flare luminosities have been used to model various simulation flare characteristics. Several approximations have been made regarding the thermal evolution that involve condensation, evaporation, and coagulation of protoCAIs. Ensembles of refractory cores with ferromagnesian mantles were evolved for irradiation production of the shortlived nuclides 7 Be, 10 Be, 41 Ca, 36 Cl, 26 Al, and 53 Mn. Three distinct grain-size distributions of protoCAIs with refractory cores in the ranges of 32 μm-20 mm, 125 μm-16 mm, and 500 μm-13 mm were thermally evolved for irradiation. The latter two size distributions were found to result in the accumulation of protoCAIs in the reconnection ring during an X-wind cycle, and hence can account for the total inventory of 26 Al in the early solar system. The canonical value of ~5 × 10 −5 for 26 Al/ 27 Al can be inferred from the impulsive flare simulations by a suitable choice of simulation parameters. However, in most of the remaining simulations, the irradiation of protoCAIs by superflare(s) with Lx > 10 32 ergs s −1 subsequent to their thermal processing in the reconnection ring would be required to explain the experimental abundances of the short-lived nuclides. These superflares have never been reliably observed in young stellar objects. If they are real, they would be extremely rare. The paucity of these superflares could impose stringent constraints on the validity of the X-wind irradiation scenario as the source of the short-lived nuclides.

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Production of residual nuclei by proton-induced reactions on C, N, O, Mg, AI and Si

Cited by 84 publications

References 54 publications

Spallation recoil II: Xenon evidence for young SiC grains

Spallation recoil II: Xenon evidence for young SiC grains

Differential cross sections on fragment (2 ≤ Z ≤ 9) production for carbon, aluminum and silicon induced by tens-of-MeV protons

Numerical simulations of the production of extinct short‐lived nuclides by magnetic flaring in the early solar system

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