Habit and texture studies of lunar and meteoritic materials with a 1 MeV electron microscope
References (25)
Disordered pyroxene in chondrites
Geochim. Cosmochim. Acta
(1968)- et al.
X-ray diffraction study of kamacite from iron meteorites
Geochim. Cosmochim. Acta
(1968) - et al.
High voltage electron microscope studies of fossil nuclear particle tracks in extraterrestrial matter
Earth Planet. Sci. Letters
(1970) La magnetite en plaquette des meteorites carbonées d'Alais, Ivuna et Orgueil
Earth Planet. Sci. Letters
(1967)- et al.
Sur les notions d'habitus et de texture des solides pulvérulents
- et al.
Electron Microscopy of Thin Crystals
(1965) The use of selected area electron diffraction in meteorite mineralogy, in Meteorite Research
(1968)- et al.
High voltage transmission electron microscopy study of lunar surface material
Science
(1970) - et al.
Mineralogical and petrological investigations of lunar samples
Science
(1970) - et al.
Mössbauer effect and high-voltage electron microscopy of pyroxenes in type B samples
Science
(1970)
Lunar clinopyroxenes
Science
Lunar pyroxenes, Microscopie Electronique
Cited by (25)
Surface microstructures of lunar soil returned by Chang'e-5 mission reveal an intermediate stage in space weathering process
2022, Science BulletinCitation Excerpt :The energy resolution of EELS was estimated to be 0.4–0.7 eV from the full width at half maximum of zero-loss peak. Most of the measured grains have sharp edges and typical crystallographic habits rather than the rounded surface of grains from the Apollo and Luna missions [27]. We start with olivine as it is the most sensitive to space weathering among the Moon’s minerals [28–31].
Structural and chemical modifications of oxides and OH generation by space weathering: Electron microscopic/spectroscopic study of hydrogen-ion-irradiated Al<inf>2</inf>O<inf>3</inf>
2021, Geochimica et Cosmochimica ActaCitation Excerpt :The main cause of space weathering is either bombardment of micrometeorites or irradiation of the solar wind. Detailed analyses of damaged textures on the actual regolith grains—brought back directly from airless bodies such as Moon and the asteroid Itokawa—suggest that solar-wind irradiation, ∼95% of which is attributable to hydrogen (H) ions (Reisenfeld et al., 2003, 2007), should be responsible for their characteristic textures (Dran et al., 1970; Christoffersen et al., 1996; Keller and McKay, 1997; Noguchi et al., 2011, 2014; Pieters and Noble, 2016). In addition, damaged rims produced by the solar wind irradiation were also found in crystalline silicates from chondritic porous interplanetary-dust particles (CP-IDPs; Bradley et al., 2014).
Isotopic composition of surface-correlated chromium in Apollo 16 lunar soils
2003, Geochimica et Cosmochimica ActaThe nature and origin of rims on lunar soil grains
1997, Geochimica et Cosmochimica Acta