Xenon and krypton isotopes in extraterrestrial regolith soils and in the solar wind

Pepin, R. O.; Becker, R. H.; Rider, Paul E.

doi:10.1016/0016-7037(96)80916-1

Cited by 96 publications

(90 citation statements)

References 34 publications

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“…9 shows the permil differences in isotopic composition of SW-Kr inferred by the analysis of lunar regolithic material (Pepin et al, 1995) relative to SW-Kr measured in Genesis Al-collectors in this study. While there is no statistical difference between these compositions within the rather large uncertainties, a distinct (~2‰/amu) mass fractionation is suggested, favoring the heavy isotopes in the lunar-derived SW compositions.…”

Section: Comparison With Solar Wind Kr and Xe Analyses Of Young Lunarmentioning

confidence: 75%

“…Author manuscript; available in PMC 2017 November 16. "Lunar" SW (blue, Pepin et al, 1995) and Q-gases (black, Busemann et al, 2000) vs.…”

Section: Resultsmentioning

confidence: 99%

“…First, only the degree of linear fractionation of pure SW is determined without any additional components. This produces a χ 2 = 10 and 8.7 for Xe and Kr, respectively ( Table 8), indicating that Q-Xe and Q-Kr cannot be a product of linear fractionation of SW. Before Genesis measurements the fractionated SW (from young lunar regolith, Pepin et al, 1995) differed from Q by only 2.2σ for both Xe and Kr allowing Ozima et al (1998) to conclude that they are related by some form of mass-dependent fractionation. Now this difference is 10σ and ~9σ, for Xe and Kr respectively, suggesting that simple massfractionation is not sufficient to make Q from SW.…”

Section: Composition Of Xe and Kr In Phase-qmentioning

confidence: 95%

“…Shown fractions are for major isotopes: 84 Kr and 132 Xe. d Pepin et al, 1995. e Similar to minimization made by Gilmour, 2010. f Meshik et al, 2012. …”

mentioning

confidence: 99%

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Heavy noble gases in solar wind delivered by Genesis mission

Meshik

Hohenberg

Pravdivtseva

et al. 2014

Geochimica et Cosmochimica Acta

100

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One of the major goals of the Genesis Mission was to refine our knowledge of the isotopic composition of the heavy noble gases in solar wind and, by inference, the Sun, which represents the initial composition of the solar system. This has now been achieved with permil precision: 36 124 Xe/ 132 Xe = .00491 ± .00007 (error-weighted averages of all published data). The Kr and Xe ratios measured in the Genesis solar wind collectors generally agree with the less precise values obtained from lunar soils and breccias, which have accumulated solar wind over hundreds of millions of years, suggesting little if any temporal variability of the isotopic composition of solar wind krypton and xenon. The higher precision for the initial composition of the heavy noble gases in the solar system allows (1) to confirm that, exept 136 Xe and 134 Xe, the mathematically derived U-Xe is equivalent to Solar Wind Xe and (2) to provide an opportunity for better understanding the relationship between the starting composition and Xe-Q (and Q-Kr), the dominant current "planetary" component, and its host, the mysterious phase-Q.

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Section: Comparison With Solar Wind Kr and Xe Analyses Of Young Lunarmentioning

confidence: 75%

“…Author manuscript; available in PMC 2017 November 16. "Lunar" SW (blue, Pepin et al, 1995) and Q-gases (black, Busemann et al, 2000) vs.…”

Section: Resultsmentioning

confidence: 99%

Section: Composition Of Xe and Kr In Phase-qmentioning

confidence: 95%

“…Shown fractions are for major isotopes: 84 Kr and 132 Xe. d Pepin et al, 1995. e Similar to minimization made by Gilmour, 2010. f Meshik et al, 2012. …”

mentioning

confidence: 99%

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Heavy noble gases in solar wind delivered by Genesis mission

Meshik

Hohenberg

Pravdivtseva

et al. 2014

Geochimica et Cosmochimica Acta

100

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show abstract

“…For Xe the excesses due to the decay of now extinct 129I are marginal. The most significant point to be noted is that a large number of temperature steps, generally at least one step of each sample, have a 129Xe/13øXe ratio lower than atmospheric and that the lowest measured value for this ratio is equal to that inferred for radiogenic-free meteoritic Xe components [Pepin et al, 1995]. This is the most diagnostic in determining the trapped Xe isotopic composition of this meteorite.…”

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confidence: 84%

Solar‐like trapped noble gases in the Brenham pallasite

Mathew¹,

Begemann²

1997

J. Geophys. Res.

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The evolution of MORB and plume mantle volatile budgets: Constraints from fission Xe isotopes in Southwest Indian Ridge basalts

Parai

Mukhopadhyay

2015

Geochem. Geophys. Geosyst.

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We present high-precision measurements of the fission isotopes of xenon (Xe) Xe is recycled in origin), consistent with results from studies of plume-influenced basalts from Iceland and the Rochambeau Rift. While significant regassing of the mantle is evident, we also find differences in the extent of degassing of the MORB and plume sources. MORB sources are consistently characterized by a lower fraction of fission Xe derived from Pu-fission, indicating a greater extent of degassing relative to the plume source. The prevalence of recycled atmospheric Xe in mantle sources indicates incorporation of depleted recycled material even into mantle sources with primitive He and Ne isotopic compositions. Consequently, depleted lithophile isotopic compositions in mantle sources with primitive He and Ne cannot be interpreted as evidence for a nonchondritic bulk silicate Earth.

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Xenon and krypton isotopes in extraterrestrial regolith soils and in the solar wind

Cited by 96 publications

References 34 publications

Heavy noble gases in solar wind delivered by Genesis mission

Heavy noble gases in solar wind delivered by Genesis mission

Solar‐like trapped noble gases in the Brenham pallasite

The evolution of MORB and plume mantle volatile budgets: Constraints from fission Xe isotopes in Southwest Indian Ridge basalts

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