Thin-target cross sections of proton-induced reactions on barium and solar cosmic ray production rates of xenon-isotopes in lunar surface materials

Prescher, K.; Peiffer, F.; Stueck, R.; Michel, R.; Bodemann, R.; Rao, M. N.; Mathew, K. J.

doi:10.1016/0168-583x(91)95645-t

Cited by 17 publications

(7 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The excitation functions for the proton-induced reactions were taken in the case of krypton from the work of Gilabert et al (1998) and Regnier et al (1982) and, in the case of Xe, from Prescher et al (1991) and Mathews et al (1994) and references therein. Gaps in the experimental excitation functions were closed by interpolations based on the shapes of theoretical cross sections for these reactions calculated by the AREL code (Blann, 1994, pers.…”

Section: Resultsmentioning

confidence: 99%

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Gilabert

Lavielle

Michel

et al. 2002

Meteorit & Planetary Scien

Self Cite

View full text Add to dashboard Cite

Abstract-Two spherical targets made of gabbro with a radius of 25 ern and of steel with a radius of 10 cm were irradiated isotropically with 1600 MeV protons at the SATURNE synchrotron at Laboratoire National Satume (LNS)/CEN Saclay, in order to simulate the production of nuclides in meteorites induced by galactic cosmic-ray protons in space. These experiments supply depth-dependent production rate data for a wide range of radioactive and stable isotopes in up to 28 target elements. In this paper, we report results for 78Kr, 80-86Kr isotopes in Rb, Sr, Y and Zr and for 124Xe, 126Xe, 128-132Xe, 134Xe, 136Xeisotopes in Ba and La. Krypton and xenon concentrations have been measured at different depths in the spheres by using conventional mass spectrometry. Based on Monte-Carlo techniques, theoretical production rates are calculated by folding depth-dependent spectra ofprimary and secondary protons and secondary neutrons with the excitation functions of the relevant nuclear reactions. The comparison ofthe model calculation results with experimental data in the thick target experiments performed at LNS and previously at CERN have allowed adjustments of the poorly known excitation functions ofneutron-induced reactions. Thus, for the two experiments at SATURNE, excellent agreement is obtained between experimental and calculated production rates for most Kr and Xe isotopes in all investigated target elements. Only Xe production in Ba in the gabbro is underestimated by the calculations by -25%. This work validates the approach of the thin-target model calculations of cosmogenic nuclide production rates in the attempt ofmodeling the interaction of galactic cosmic-ray protons with stony and iron meteorites in space as well as with lunar samples.

show abstract

Section: Resultsmentioning

confidence: 99%

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Gilabert

Lavielle

Michel

et al. 2002

Meteorit & Planetary Scien

Self Cite

View full text Add to dashboard Cite

show abstract

“…We do not use the fourth spectrum considered by Reedy (1989), which is an estimate for the GCR source. Cross-sections were taken from Prescher et al (1991) for proton energies up to 30 MeV, and interpolated/mean values derived from Kaiser (1977), Mathew et al (1994), Gilabert et al (1997), and this work, at higher energies. Production rates for 126 Xe based on the three spectra vary between 2.2 × 10 −15 and 7.2 × 10 −15 cm 3 STP (ppm Ba) −1 (Ma) −1 , with a geometric mean of 3.74 × 10 −15 .…”

Section: Production On Ba By Gcr Protonsmentioning

confidence: 99%

Spallation recoil II: Xenon evidence for young SiC grains

Ott

Altmaier

Herpers

et al. 2005

Meteoritics &Amp; Planetary Science

Self Cite

View full text Add to dashboard Cite

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

show abstract

“…nat Ba( , ) 135 La nuclear reaction [15][16][17]. The recovery of the enriched 135 Ba was 90 ± 3%, so that after 7 irradiation and separation cycles the amount of the target material will be 50% caused by chemical loss.…”

Section: Resultsmentioning

confidence: 98%

“…Additionally, the target was cooled with water on its backside (13 ∘ C). Prior to production runs, a CaCO 3 target was used to test ther- respectively [15][16][17][18]. The detected radionuclides, -ray energies, -ray intensities, cross sections of the nuclear reactions and theoretically expected yields are summarized in Table 1 to get rid of the acetate and finally dried in a beaker to residue (Figure 1).…”

Section: Targetry and Irradiationmentioning

confidence: 99%

“…Detected radionuclides with -ray energies , intensities and origin (nuclear reaction), cross sections at 12 MeV used for calculation of theoretically expected yields Y for the given enrichment of the target[14][15][16][17][18]; * not detected due to the short half-life.Fig. 1: Scheme for the separation of 135 La from the irradiated [ 135 Ba]BaCO 3 target.mal target stability; no CO 2 outgasing was detected that would be present via 13 N activity release in the exhaust gas due to the nuclear reaction 16 O( , ) 13 N[23].…”

mentioning

confidence: 99%

See 1 more Smart Citation

Production of no-carrier-added ¹³⁵La at an 18 MeV cyclotron and its purification for investigations at a concentration range down to 10⁻¹⁵ mol/L

Mansel¹,

Franke²

2015

Radiochimica Acta

View full text Add to dashboard Cite

The production of non-commercially available 135 La by proton irradiation of an isotopically enriched [ 135 Ba]BaCO 3 target at a cyclotron is described. The purification of the radionuclide was performed by a La-selective resin. 135 La was separated in no-carrier-added (n.c.a) form in a nitric acid solution with a radiochemical yield of 83 ± 5% and a total activity per batch of 43 ± 3 MBq. The enriched [ 135 Ba]Ba was recycled to the carbonate form with a recovery of 90 ± 3%. On the basis of a detection limit of 1 Bq/mL, solutions of n.c.a. 135 La could be measured down to the 10 −15 mol/L concentration range.

show abstract

Thin-target cross sections of proton-induced reactions on barium and solar cosmic ray production rates of xenon-isotopes in lunar surface materials

Cited by 17 publications

References 25 publications

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Spallation recoil II: Xenon evidence for young SiC grains

Production of no-carrier-added ¹³⁵La at an 18 MeV cyclotron and its purification for investigations at a concentration range down to 10⁻¹⁵ mol/L

Contact Info

Product

Resources

About

Thin-target cross sections of proton-induced reactions on barium and solar cosmic ray production rates of xenon-isotopes in lunar surface materials

Cited by 17 publications

References 25 publications

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Production of krypton and xenon isotopes in thick stony and iron targets isotropically irradiated with 1600 MeV protons

Spallation recoil II: Xenon evidence for young SiC grains

Production of no-carrier-added 135La at an 18 MeV cyclotron and its purification for investigations at a concentration range down to 10−15 mol/L

Contact Info

Product

Resources

About

Production of no-carrier-added ¹³⁵La at an 18 MeV cyclotron and its purification for investigations at a concentration range down to 10⁻¹⁵ mol/L