Solar Wind and Solar System Matter After Mission Genesis

Marti, K.; Bochsler, P.

doi:10.5772/36974

Cited by 2 publications

(2 citation statements)

References 89 publications

(126 reference statements)

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“…WIND MASS [Gloeckler et al, 1995] and SOHO CELIAS MTOF [Hovestadt et al, 1995] have indeed provided great insight into the solar wind isotope composition and have expanded on the initial measurements taken with solar wind collector foils during the Apollo missions on the Moon's surface [Geiss et al, 1972]. The isotope composition of the solar wind is the best proxy that we can currently obtain on the Sun's isotope composition, which in turn is an archive of the element forming processes in the galaxy [Geiss and Reeves, 1972] and of the fractionation processes during the solar system formation [Marti and Bochsler, 2012]. The solar corona and thus the solar wind do not necessarily share an unbiased isotope composition with the Sun's interior [Bochsler, 2001].…”

Section: Solar Wind Isotope Observationmentioning

confidence: 99%

Time‐of‐flight mass spectrographs—From ions to neutral atoms

et al. 2016

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After their introduction to space physics in the mid 1980s time‐of‐flight (TOF) spectrographs have become a main staple in spaceborne mass spectrometry. They have largely replaced magnetic spectrometers, except when extremely high mass resolution is required to identify complex molecules, for example, in the vicinity of comets or in planetary atmospheres. In combination with electrostatic analyzers and often solid state detectors, TOF spectrographs have become key instruments to diagnose space plasma velocity distributions, mass, and ionic charge composition. With a variety of implementation schemes that also include isochronous electric field configurations, TOF spectrographs can respond to diverse science requirements. This includes a wide range in mass resolution to allow the separation of medium heavy isotopes or to simply provide distributions of the major species, such as H, He, and O, to obtain information on source tracers or mass fluxes. With a top‐hat analyzer at the front end, or in combination with deflectors for three‐axis stabilized spacecraft, the distribution function of ions can be obtained with good time resolution. Most recently, the reach of TOF ion mass spectrographs has been extended to include energetic neutral atoms. After selecting the arrival direction with mechanical collimation, followed by conversion to ions, adapted TOF sensors form a new branch of the spectrograph family tree. We review the requirements, challenges, and implementation schemes for ion and neutral atom spectrographs, including potential directions for the future, while largely avoiding overlap with complementary contributions in this special issue.

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Section: Solar Wind Isotope Observationmentioning

confidence: 99%

Time‐of‐flight mass spectrographs—From ions to neutral atoms

et al. 2016

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“…Although rapidly developing, optical observations are still of little value for determining isotopic compositions in the present context, and we have no physical samples of bulk solar material, but rather only of the solar wind. The distinction between ''solar'' and ''solar wind'' (hereafter SW) is significant: Although SW is directly ejected from the solar atmosphere, so that its elemental and isotopic compositions are generally regarded as good proxies for the Sun (see, e.g., Marti and Bochsler [2012] for a recent review), SW is a chemically and isotopically biased sampling, as fractionations arise in acceleration of bulk solar material into the SW. The SW can be sampled and analyzed in direct real-time spacecraft measurements, in artificial targets exposed to SW in space and then returned to Earth in the Genesis mission, and in natural solid planetary materials exposed on airless bodies over geologic time.…”

Section: Introductionmentioning

confidence: 99%

Noble gas isotopic fractionation between solar wind and the Sun, and implications for Genesis solar wind oxygen measurements

Ozima

Suzuki

Yamada

et al. 2012

Meteorit & Planetary Scien

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Abstract-We urge that He is the best case for a meaningful estimation of solar composition without measurement of solar wind (SW) composition; the value of such an estimation is that it may then be compared to the actual measurements, thereby leading to an empirical constraint on the degree of isotopic fractionation arising in SW and thence to how much fractionation may have affected the SW composition of other elements. We take primordial 3 He ⁄ 4 He to be as identified in the so-called Q component identified in meteoritic materials. In the Sun, however, 3 He ⁄ 4 He is higher because of the augmentation of 3 He by D-burning, the nuclear conversion of primordial deuterium. After accounting for the D-converted 3 He, we estimate 3 He ⁄ 4 He in the present Sun (post-D burning He), and then, from the difference between this and the 3 He ⁄ 4 He found in Genesis SW, we estimate the isotopic fractionation between them. Then, from noble gas systematics, we show that Genesis SW noble gases may be related to Q-noble gases by a mass-dependent Rayleigh-type fractionation. We develop a kinetic description of isotopic fractionation of minor components in SW relative to the solar atmosphere, which is consistent with the Rayleigh-type fractionation. This predicts fractionation in the O mass range, which is significantly different from the value used by Heber et al. (2011). The latter value corresponds to the premise that Ca-Al-rich inclusion O is the same as solar O, whence this work does not support that premise.

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Solar Wind and Solar System Matter After Mission Genesis

Cited by 2 publications

References 89 publications

Time‐of‐flight mass spectrographs—From ions to neutral atoms

Time‐of‐flight mass spectrographs—From ions to neutral atoms

Noble gas isotopic fractionation between solar wind and the Sun, and implications for Genesis solar wind oxygen measurements

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