Helium, neon, and argon abundances in the solar wind: In vacuo etching of meteoritic iron-nickel

Murer, Christoph; Baur, H.; Signer, P.; Wieler, R.

doi:10.1016/s0016-7037(97)83772-6

Cited by 25 publications

(17 citation statements)

References 23 publications

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“…The solar wind noble gas data obtained from these "targets" are in good agreement with data obtained from in-situ measurements and the Apollo foils (e.g., for He, Ne and Ar [7,34,30]), which gives us confidence to make predictions also for Kr and Xe. Because of the long exposure time of the meteoritic and lunar samples, their analysis is so far the only method to obtain solar wind Kr and Xe abundances as well as the Kr and Xe isotopic composition.…”

Section: Trapped Solar Windsupporting

confidence: 81%

“…Diffusive loss or redistribution of light noble gases within the grains may influence the original solar wind composition. Experiments on mineral separates have shown that the most retentive Fe-Ni grains conserve the true relative abundances of solar He, Ne, Ar [34,30], but FeNi is very rare in lunar samples. Ilmenite, another retentive mineral phase, which is abundant in lunar samples, has lost some of its solar He and Ne, but apparently without altering the isotopic composition of these gases [7].…”

Section: Trapped Solar Windmentioning

confidence: 99%

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Measuring Solar Abundances

Steiger¹,

Vial²,

Bochsler³

et al. 2001

AIP Conference Proceedings

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Abstract. This is the rapporteur paper of Working Group 2 on Measuring Solar Abundances. The working group presented and discussed the different observations and methods for obtaining the elemental and isotopic composition of the Sun, and critically reviewed their results and the accuracies thereof. Furthermore, a few important yet unanswered questions were identified, and the potential of future missions to provide answers was assessed.

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Section: Trapped Solar Windsupporting

confidence: 81%

Section: Trapped Solar Windmentioning

confidence: 99%

Measuring Solar Abundances

Steiger¹,

Vial²,

Bochsler³

et al. 2001

AIP Conference Proceedings

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“…The average composition, energy, and flux of the SW is relatively well characterized from analyses of Al foils exposed on the surface of the Moon during the Apollo missions (Geiss et al 2004), studies of gas-retentive meteoritic Fe-Ni separates (e.g., Murer et al 1997), and lunar soil samples (e.g., Benkert et al 1993;Palma et al 2002), satellite measurements (e.g., Bochsler et al 1986), and more recently by studies of collector materials from the Genesis spacecraft (e.g., Grimberg et al 2006;Hohenberg et al 2006;Meshik et al 2006). SW ions are relatively low in energy (~0.5-2.6 keV/amu).…”

Section: Discussion Solar Gases In Idpsmentioning

confidence: 99%

Noble gas space exposure ages of individual interplanetary dust particles

Kehm

Flynn

Hohenberg

2006

Meteoritics &Amp; Planetary Science

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Abstract-The He, Ne, and Ar compositions of 32 individual interplanetary dust particles (IDPs) were measured using low-blank laser probe gas extraction. These measurements reveal definitive evidence of space exposure. The Ne and Ar isotopic compositions in the IDPs are primarily a mixture between solar wind (SW) and an isotopically heavier component dubbed "fractionated solar" (FS), which could be implantation-fractionated solar wind or a distinct component of the solar corpuscular radiation previously identified as solar energetic particles (SEP). Space exposure ages based on the Ar content of individual IDPs are estimated for a subset of the grains that appear to have escaped significant volatile losses during atmosphere entry. Although model-dependent, most of the particles in this subset have ages that are roughly consistent with origin in the asteroid belt. A short (<1000 years) space exposure age is inferred for one particle, which is suggestive of cometary origin. Among the subset of grains that show some evidence for relatively high atmospheric entry heating, two possess elevated 21 Ne/ 22 Ne ratios generated by extended exposure to solar and galactic cosmic rays. The inferred cosmic ray exposure ages of these particles exceeds 10 7 years, which tends to rule out origin in the asteroid belt. A favorable possibility is that these 21 Ne-rich IDPs previously resided on a relatively stable regolith of an Edgeworth-Kuiper belt or Oort cloud body and were introduced into the inner solar system by cometary activity. These results demonstrate the utility of noble gas measurements in constraining models for the origins of interplanetary dust particles.

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“…The 20 Ne/ 4 He ratio of Q is after Busemann et al (2000), the 3 He/ 4 He ratio of Q is after Wieler et al (1991), the 3 He/ 4 He ratios of SEP and SW are after Benkert et al (1993), the 20 Ne/ 4 He ratio of SW is after Murer et al (1997), and the 20 Ne/ 4 He ratio of SEP is after Ozima and Podosek (2002). The errors are 1σ.…”

Section: Argonmentioning

confidence: 92%

Noble gas isotopes and mineral assemblages of Antarctic micrometeorites collected at the meteorite ice field around the Yamato Mountains

Osawa

Nakamura

Nagao

2003

Meteorit & Planetary Scien

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Noble gas isotopes and mineral assemblages of Antarctic micrometeorites collected at the meteorite ice field around the Yamato MountainsAbstract-From November 1998 to January 1999, the 39th Japanese Antarctic Research Expedition (JARE) conducted a large-scale micrometeorite collection at 3 areas in the meteorite ice field around the Yamato Mountains, Antarctica. The Antarctic micrometeorites (AMMs) collected were ancient cosmic dust particles. This is in contrast with the Dome Fuji AMMs, which were collected previously from fresh snows in 1996 and 1997 and which represent modern micrometeorites. To determine the noble gas concentrations and isotopic compositions of individual AMMs, noble gas analyses were carried out using laser-gas extraction for 35 unmelted Yamato Mountains AMMs and 3 cosmic spherules. X-ray diffraction analyses were performed on 13 AMMs before the noble gas measurement and mineral compositions were determined. AMMs are classified into 4 main mineralogical groups, defined from the heating they suffered during atmospheric entry. Heating temperatures of AMMs, inferred from their mineral compositions, are correlated with 4 He concentrations and reflect the effect of degassing during atmospheric entry. Jarosite, an aqueous alteration product, is detected for 4 AMMs, indicating the aqueous alteration during long-time storage in Antarctic ice. Jarosite-bearing AMMs have relatively low concentrations of 4 He, which is suggestive of loss during the alteration.High 3 He/ 4 He ratios are detected for AMMs with high 20 Ne/ 4 He ratios, showing both cosmogenic 3 He and preferential He loss. SEP (solar energetic particles)-He and Ne, rather than the solar wind (SW), were dominant in AMMs, presumably showing a preferential removal of the more shallowly implanted SW by atmospheric entry heating. The mean 20 Ne/ 22 Ne ratio is 11.27 ± 0.35, which is close to the SEP value of 11.2. Cosmogenic 21 Ne is not detected in any of the particles, which is probably due to the short cosmic ray exposure ages. Ar isotopic compositions are explained by 3-component mixing of air, Q, and SEP-Ar. Ar isotopic compositions can not be explained without significant contributions of Q-Ar. SEP-Ne contributed more than 99% of the total Ne. As for 36 Ar and 38 Ar, the abundance of the Q component is comparable to that of the SEP component. 84 Kr and 132 Xe are dominated by the primordial component, and solar-derived Xe is almost negligible.

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Helium, neon, and argon abundances in the solar wind: In vacuo etching of meteoritic iron-nickel

Cited by 25 publications

References 23 publications

Measuring Solar Abundances

Measuring Solar Abundances

Noble gas space exposure ages of individual interplanetary dust particles

Noble gas isotopes and mineral assemblages of Antarctic micrometeorites collected at the meteorite ice field around the Yamato Mountains

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