The Genesis Discovery Mission: Return of Solar Matter to Earth

Burnett, D. S.; Barraclough, B. L.; Bennett, Richard B.; Neugebauer, M.; Oldham, Lloyd P.; Sasaki, Chester; Sevilla, D.; Smith, Nicholas G.; Stansbery, Eileen K.; Sweetnam, D. N.; Wiens, R. C.

doi:10.1007/978-94-010-0241-7_1

Cited by 50 publications

(42 citation statements)

References 29 publications

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“…An overview of the Genesis Mission is given in [1], and the SW implant is detailed in [2]. However, the salient points to note about the Genesis-flown DoS fragments used here are:…”

Section: The Genesis Sw Samplementioning

confidence: 99%

“…The purpose of the Genesis Mission was to return a sample of SW in order to measure the composition of the minor SW ions accurately and precisely. The SW composition defines the composition of the outer portion of the Sun and, by extension, the composition of the solar nebula from which our solar system formed [1]. The SW is a flux of high-velocity ions consisting primarily of H with a significant amount of He.…”

Section: Introductionmentioning

confidence: 99%

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Understanding heterogeneity in Genesis diamond-like carbon film using SIMS analysis of implants

et al. 2017

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An amorphous diamond-like carbon film deposited on silicon made at Sandia National Laboratory by pulsed laser deposition was one of several solar wind (SW) collectors used by the Genesis Mission (NASA Discovery Class Mission #5). The film was *1 lm thick, amorphous, anhydrous, and had a high ratio of sp 3 -sp 2 bonds ([50%). For 27 months of exposure to space at the first Lagrange point, the collectors were passively irradiated with SW (H fluence *2 9 10 16 ions cm -2 ; He fluence *8 9 10 14 ions cm -2 ). The radiation damage caused by the implanted H ions peaked at 12-14 nm below the surface of the film and that of He about 20-23 nm. To enable quantitative measurement of the SW fluences by secondary ion mass spectroscopy, minor isotopes of Mg ( 25 Mg and 26 Mg) were commercially implanted into flight-spare collectors at 75 keV and a fluence of 1 9 10 14 ions cm -2 . The shapes of analytical depth profiles, the rate at which the profiles were sputtered by a given beam current, and the intensity of ion yields are used to characterize the structure of the material in small areas (*200 9 200 ± 50 lm). Data were consistent with the hypothesis that minor structural changes in the film were induced by SW exposure.

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“…An overview of the Genesis Mission is given in [1], and the SW implant is detailed in [2]. However, the salient points to note about the Genesis-flown DoS fragments used here are:…”

Section: The Genesis Sw Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Understanding heterogeneity in Genesis diamond-like carbon film using SIMS analysis of implants

et al. 2017

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“…Samples containing the Solar Wind (SW), captured by Genesis Mission collectors (http:// genesismission.jpl.nasa.gov/; Burnett et al, 2003;Jurewicz et al, 2003), became available for laboratory analyses in early 2005. However, it took more than 5 years of refining the analytical capabilities for results for of all noble gases to emerge.…”

Section: Introductionmentioning

confidence: 99%

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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“…Solar wind was captured at the Earth-Sun Lagrangian (L1) point using high-purity collectors over 28 months [Burnett et al, 2003]. The Genesis capsule returned to Earth in 2004.…”

Section: Solar Wind Atoms From the Genesis Spacecraftmentioning

confidence: 99%