Helium, neon, and argon in meteorites: A data collection

Schultz, L.; Franke, L.

doi:10.1111/j.1945-5100.2004.tb00083.x

Cited by 98 publications

(113 citation statements)

References 3 publications

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“…Thus, the probability that all 8 analyzed SEC grain batches from different sediment beds contain at least one grain from the solar gas-rich population is less than 10 −6 . Second, the range of solar 22 Ne concentrations in gas-rich L chondrites of ~(10-150) × 10 −8 cm 3 /g (Schultz and Franke 2004) is clearly lower than the range of 22 Ne concentrations found in the chromites (Fig. 4), although the chromites have a larger grain size and thus a lower surface-tovolume area than meteoritic matrix grains.…”

Section: Solar Noble Gasesmentioning

confidence: 92%

“…The bulk data of the ordinary chondrite Harleton given in Table 3 are from the data compilation of Schultz and Franke (2004). Gases from the ~100 mg bulk meteorite samples were extracted in a furnace by total fusion at T ≈ 2000 K in UHV and subsequently cleaned using liquidnitrogen-cooled activated charcoal traps and hot metal alloy getters (Zr-V-Fe, Zr-Al, Zr-Ti).…”

Section: Bulk Meteorite Samplesmentioning

confidence: 99%

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Noble gases in fossil micrometeorites and meteorites from 470 Myr old sediments from southern Sweden, and new evidence for the L‐chondrite parent body breakup event

Heck

Schmitz

Baur

et al. 2008

Meteorit & Planetary Scien

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Abstract-We present noble gas analyses of sediment-dispersed extraterrestrial chromite grains recovered from ~470 Myr old sediments from two quarries (Hällekis and Thorsberg) and of relict chromites in a coeval fossil meteorite from the Gullhögen quarry, all located in southern Sweden. Both the sediment-dispersed grains and the meteorite Gullhögen 001 were generated in the Lchondrite parent body breakup about 470 Myr ago, which was also the event responsible for the abundant fossil meteorites previously found in the Thorsberg quarry. Trapped solar noble gases in the sediment-dispersed chromite grains have partly been retained during ~470 Myr of terrestrial residence and despite harsh chemical treatment in the laboratory. This shows that chromite is highly retentive for solar noble gases. The solar noble gases imply that a sizeable fraction of the sedimentdispersed chromite grains are micrometeorites or fragments thereof rather than remnants of larger meteorites. The grains in the oldest sediment beds were rapidly delivered to Earth likely by direct injection into an orbital resonance in the inner asteroid belt, whereas grains in younger sediments arrived by orbital decay due to Poynting-Robertson (P-R) drag. The fossil meteorite Gullhögen 001 has a low cosmic-ray exposure age of ~0.9 Myr, based on new He and Ne production rates in chromite determined experimentally. This age is comparable to the ages of the fossil meteorites from Thorsberg, providing additional evidence for very rapid transfer times of material after the L-chondrite parent body breakup.

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Section: Solar Noble Gasesmentioning

confidence: 92%

Section: Bulk Meteorite Samplesmentioning

confidence: 99%

Noble gases in fossil micrometeorites and meteorites from 470 Myr old sediments from southern Sweden, and new evidence for the L‐chondrite parent body breakup event

Heck

Schmitz

Baur

et al. 2008

Meteorit & Planetary Scien

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“…This suggests they contain fewer pre-solar grains than carbonaceous chondrites or they were made of material that was more influenced by the solar wind irradiation because they accreted closer to the sun; the solar wind being the source of neon B. Schultz et al (2005), Mazor et al (1970), Schultz and Franke (2004) and Schelhass et al (1990). Figure 2.15 focuses on carbonaceous chondrites and shows the neon isotopic composition of the different sub-classes of carbonaceous chondrites.…”

Section: Neon A: Pre-solar Diamondsmentioning

confidence: 99%

Noble gas constraints on the origin and evolution of Earth’s volatiles

Moreira¹

2013

GeochemPersp

115

164

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“…In Fig. 5 we have plotted ( 21 Ne/ 22 Ne) c values (calculated as described in the chapter "component resolution") from our own complete data set (diamonds) ( Table 2) as well as from data for the same meteorites taken from the literature (compilation of Schultz and Franke 2004;+ signs). These are compared to the range of possible values produced by GCR.…”

Section: Neon: the Influence Of Solar Cosmic Raysmentioning

confidence: 99%

“…Noble gas and nitrogen measurements on EETA79001, Shergotty, and Zagami reported in the literature. For He, Ne, and Ar data see also the data collection of Schultz and Franke (2004). Conc.…”

Section: Concmentioning

confidence: 99%

Noble gases in mineral separates from three shergottites: Shergotty, Zagami, and EETA79001

Schwenzer¹,

Herrmann²,

Mohapatra

et al. 2007

Meteorit & Planetary Scien

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Abstract-This study provides a complete data set of all five noble gases for bulk samples and mineral separates from three Martian shergottites: Shergotty (bulk, pyroxene, maskelynite), Zagami (bulk, pyroxene, maskelynite), and Elephant Moraine (EET) A79001, lithology A (bulk, pyroxene). We also give a compilation of all noble gas and nitrogen studies performed on these meteorites. Our mean values for cosmic-ray exposure ages from 3 He, 21 Ne, and 38 Ar are 2.48 Myr for Shergotty, 2.73 Myr for Zagami, and 0.65 Myr for EETA79001 lith. A. Serious loss of radiogenic 4 He due to shock is observed. Cosmogenic neon results for bulk samples from 13 Martian meteorites (new data and literature data) are used in addition to the mineral separates of this study in a new approach to explore evidence of solar cosmic-ray effects. While a contribution of this low-energy irradiation is strongly indicated for all of the shergottites, spallation Ne in Chassigny, Allan Hills (ALH) 84001, and the nakhlites is fully explained by galactic cosmic-ray spallation. Implanted Martian atmospheric gases are present in all mineral separates and the thermal release indicates a near-surface siting. We derive an estimate for the 40 Ar/ 36 Ar ratio of the Martian interior component by subtracting from measured Ar in the (K-poor) pyroxenes the (small) radiogenic component as well as the implanted atmospheric component as indicated from 129 Xe * excesses. Unless compromised by the presence of additional components, a high ratio of ~2000 is indicated for Martian interior argon, similar to that in the Martian atmosphere. Since much lower ratios have been inferred for Chassigny and ALH 84001, the result may indicate spatial and/or temporal variations of 40 Ar/ 36 Ar in the Martian mantle.

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Helium, neon, and argon in meteorites: A data collection

Cited by 98 publications

References 3 publications

Noble gases in fossil micrometeorites and meteorites from 470 Myr old sediments from southern Sweden, and new evidence for the L‐chondrite parent body breakup event

Noble gases in fossil micrometeorites and meteorites from 470 Myr old sediments from southern Sweden, and new evidence for the L‐chondrite parent body breakup event

Noble gas constraints on the origin and evolution of Earth’s volatiles

Noble gases in mineral separates from three shergottites: Shergotty, Zagami, and EETA79001

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