{"type": "FeatureCollection", "features": [{"id": "10.1016/j.epsl.2017.05.033", "type": "Feature", "geometry": null, "properties": {"updated": "2026-05-24T16:16:07Z", "type": "Journal Article", "created": "2017-06-16", "title": "Rubidium isotopic composition of the Earth, meteorites, and the Moon: Evidence for the origin of volatile loss during planetary accretion", "description": "Abstract Understanding the origin of volatile element variations in the inner Solar System has long been a goal of cosmochemistry, but many early studies searching for the fingerprint of volatile loss using stable isotope systems failed to find any resolvable variations. An improved method for the chemical purification of Rb for high-precision isotope ratio measurements by multi-collector inductively-coupled-plasma mass-spectrometry. This method has been used to measure the Rb isotopic composition for a suite of planetary materials, including carbonaceous, ordinary, and enstatite chondrites, as well as achondrites (eucrite, angrite), terrestrial igneous rocks (basalt, andesite, granite), and Apollo lunar samples (mare basalts, alkali suite). Volatile depleted bodies (e.g. HED parent body, thermally metamorphosed meteorites) are enriched in the heavy isotope of Rb by up to several per mil compared to chondrites, suggesting volatile loss by evaporation at the surface of planetesimals. In addition, the Moon is isotopically distinct from the Moon in Rb. The variations in Rb isotope compositions in the volatile-poor samples are attributed to volatile loss from planetesimals during accretion. This suggests that either the Rb (and other volatile elements) were lost during or following the giant impact or by evaporation earlier during the accretion history of Theia.", "keywords": ["volatile depletion", "[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology", "[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry", "13. Climate action", "[SDU.STU.GC] Sciences of the Universe [physics]/Earth Sciences/Geochemistry", "the Moon", "[SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology", "01 natural sciences", "chondrites", "rubidium isotopes", "0105 earth and related environmental sciences"]}, "links": [{"href": "https://doi.org/10.1016/j.epsl.2017.05.033"}, {"rel": "related", "href": "https://repository.soilwise-he.eu/cat/collections/metadata:main/items/Earth%20and%20Planetary%20Science%20Letters", "name": "related record", "description": "related record", "type": "application/json"}, {"rel": "self", "type": "application/geo+json", "title": "10.1016/j.epsl.2017.05.033", "name": "item", "description": "10.1016/j.epsl.2017.05.033", "href": "https://repository.soilwise-he.eu/cat/collections/metadata:main/items/10.1016/j.epsl.2017.05.033"}, {"rel": "collection", "type": "application/json", "title": "Collection", "name": "collection", "description": "Collection", "href": "https://repository.soilwise-he.eu/cat/collections/metadata:main"}], "time": {"date": "2017-09-01T00:00:00Z"}}, {"id": "10.1073/pnas.2023023118", "type": "Feature", "geometry": null, "properties": {"updated": "2026-05-24T16:17:52Z", "type": "Journal Article", "created": "2021-03-15", "title": "Conditions and extent of volatile loss from the Moon during formation of the Procellarum basin", "description": "Significance

The depletion of moderately volatile elements in the lunar interior, compared to the Earth\uffe2\uff80\uff99s interior, is accompanied by enrichment in heavy isotopes for most species. This has been explained by vapor loss from the protolunar disk, incomplete accretion of volatiles, or volatile degassing during crystallization of the lunar magma ocean. Importantly, these hypotheses have assumed that volatile depletion and associated isotope fractionations are relevant to the whole Moon. However, our lunar sample collections are biased, as Apollo and Luna samples come from within or around the anomalous Procellarum KREEP Terrane region on the lunar nearside. Here, we propose that these chemical and isotopic features could have resulted from a large-scale impact event on the nearside early in the Moon\uffe2\uff80\uff99s history.

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Events following the giant impact formation of the Moon are thought to have led to volatile depletion and concurrent mass-dependent fractionation of the isotopes of moderately volatile elements (MVE). The detailed processes and conditions surrounding this episode remain obscured and are not unified by a single model for all volatile elements and compounds. Using available data, including new Zn isotope data for eight lunar samples, we demonstrate that the isotopic fractionation of MVE in the Moon is best expressed by nonideal Rayleigh distillation, approaching the fractionation factor \uffce\uffb1 using the reduced masses of the evaporated isotopologs. With these calculations, a best fit for the data is obtained when the lunar MVE isotope data are normalized to ordinary or enstatite chondrites ( ), rather than a bulk silicate Earth composition. This analysis further indicates that the parent body from which the Moon formed cannot have partitioned S into its core based on S isotope compositions of lunar rocks. The best fit between and modeled nonideal Rayleigh fractionation is defined by a slope that corresponds to a saturation index of 90%\uffc2\uffa0\uffc2\uffb1\uffc2\uffa04%. In contrast, the older Highland suite is defined by a saturation index of 75%\uffc2\uffa0\uffc2\uffb1\uffc2\uffa02%, suggesting that the vapor phase pressure was higher during mare basalt eruptions. This provides the first tangible evidence that the Moon was veiled by a thin atmosphere during mare basalt eruption events spanning at least from 3.8 to 3 billion years ago and implies that MVE isotope fractionation dominantly occurred after the Moon had accreted.

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