Neutron‐induced gamma ray spectroscopy: Simulations for chemical mapping of planetary surfaces

Brückner, J.; Wänke, H.; Reedy, R. C.

doi:10.1029/jb092ib04p0e603

Cited by 23 publications

(8 citation statements)

References 30 publications

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“…The uranium line with the highest probability appears at 609 keV. However, it is too close to a background Ge peak at 596 keV with a high energy tail spreading up to ∼630 keV (so‐called “sawtooth” peak) [ Brückner et al , 1987]. The existence of such a high intensity interference made it difficult to determine the spectrum baseline below the uranium peak.…”

Section: Observation and Analysismentioning

confidence: 99%

Uranium on the Moon: Global distribution and U/Th ratio

Yamashita

Hasebe

Reedy

et al. 2010

Geophysical Research Letters

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Section: Observation and Analysismentioning

confidence: 99%

Uranium on the Moon: Global distribution and U/Th ratio

Yamashita

Hasebe

Reedy

et al. 2010

Geophysical Research Letters

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“…Several ground experiments using an accelerator beam and thick targets have been executed to simulate the radiation environments on the Moon and planets (Englert et al, 1987;Brückner et al, 1987;Brückner et al, 1992;Yamashita et al, 2006). Such experiments should be complimented by Monte Carlo numerical simulations because the energy region of GCR cannot be covered by an accelerator, and it is very difficult to physically prepare target materials which can confine secondary neutrons that produce gamma rays (Yamashita et al, 2004a).…”

Section: Introductionmentioning

confidence: 99%

Complexities of gamma-ray line intensities from the lunar surface

et al. 2008

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Assuming different abundances of the Apollo lunar soil samples and the average spectrum of galactic cosmic ray protons, energy spectra of neutrons and gamma rays and emission rates of gamma-ray lines from major elements have been estimated by using the reviewed Monte Carlo simulation library Geant4 and nuclear data. Previously, such libraries were not able to reproduce gamma-ray lines properly for the planetary application. Results clearly show that the emission rate of gamma rays heavily depends not only on the chemical abundance but also neutron flux within the lunar subsurface. While the intensities of gamma-ray lines are mostly proportional to elemental abundances, the intensity per unit elemental abundance can vary. Such a complex correlation is attributed to the change in neutron flux within the lunar subsurface and petrological restriction of elemental variation.

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“…Here the Fe 847-keV peak has interference from three peaks generated in the GRS and surrounding spacecraft material: a 844-keV Al peak (from 27 Mg), a 840-keV 54 Mn peak (electron capture with K-shell binding energy, 312-day half-life), and a 836-keV 54 Mn peak (L-shell binding energy). These four peaks sit atop a broad 834-keV Ge sawtooth-shape inelastic-scattering peak, whose shape is characteristic of neutron inelastic scattering occurring inside the Ge detector (Brückner et al, 1987). The count-rate analysis obtained from the peaks shown in Figs.…”

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confidence: 99%