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Yang Liu
California Institute of Technology
136Publications
28H-index
2,188Citations
Publications 136
Newest
#1William Abbey (California Institute of Technology)H-Index: 6
#2Luther W. Beegle (California Institute of Technology)H-Index: 13
Last.Yang Liu (California Institute of Technology)H-Index: 28
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#1Chi Ma (California Institute of Technology)H-Index: 21
#2Oliver Tschauner (UNLV: University of Nevada, Las Vegas)H-Index: 20
Last.Vitali B. Prakapenka (Argonne National Laboratory)H-Index: 49
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Chenmingite (FeCr_2O_4; IMA 2017-036) is a high-pressure mineral, occurring as micrometer- to submicrometer-sized lamellae within precursor chromite grains along with xieite and Fe,Cr-rich ulvospinel next to shock-induced melt pockets, from the Tissint martian meteorite. The composition of type chenmingite by electron probe analysis shows an empirical formula of (Fe^(2+)_(0.75)Mg_(0.23)Mn_(0.02)) (Cr_(1.60)Al_(0.29)Fe^(3+)_(0.06)Fe^(2+)_(0.04)Ti_(0.02))_(Σ2.01)O_4. The general and end-member for...
#1Chi Ma (California Institute of Technology)H-Index: 21
#2Yang Liu (California Institute of Technology)H-Index: 28
We present the first discovery of a Zn-rich mineral on the pristine surface of orange pyroclastic beads from Apollo sample 74220. This Zn-rich mineral is wide occurring, trigonal or hexagonal in shape, with a normalized composition of ~59 wt% Zn, ~26 wt% O (calculated), ~6 wt% S, ~5 wt% Na, and ~4 wt% Cl. The crystal morphology, homogeneity, and chemistry of individual grains are most consistent with gordaite, a zinc chlorohydroxosulfate mineral, showing an empirical formula of Na_(1.02)Zn_(3.98...
#1James M. D. Day (UCSD: University of California, San Diego)H-Index: 37
#2Kimberly T. Tait (ROM: Royal Ontario Museum)H-Index: 11
Last.Clive R. Neal (ND: University of Notre Dame)H-Index: 38
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Direct analysis of the composition of Mars is possible through delivery of meteorites to Earth. Martian meteorites include ∼165 to 2400 Ma shergottites, originating from depleted to enriched mantle sources, and ∼1340 Ma nakhlites and chassignites, formed by low degree partial melting of a depleted mantle source. To date, no unified model has been proposed to explain the petrogenesis of these distinct rock types, despite their importance for understanding the formation and evolution of Mars. Here...
#1Madison L. Myers (UO: University of Oregon)H-Index: 4
#2Paul J. Wallace (UO: University of Oregon)H-Index: 46
Last.Yang Liu (California Institute of Technology)H-Index: 28
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#1Yang Liu (California Institute of Technology)H-Index: 28
#2Yang Chen (California Institute of Technology)H-Index: 16
Last.Youxue Zhang (UM: University of Michigan)H-Index: 44
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We report volatile concentrations and hydrogen isotope compositions of impact melts and minerals in EETA 79001. We observed chemical changes in pyroxene, maskelynite (or feldspathic glass), and merrillite in contact with or inside impact melts. All pyroxene grains analyzed here are inside or close to impact melt pockets and contain 10–41 ppm H_2O and enriched in D (δD=+1729 to +3707‰), with the highest values found in a grain enclosed in an impact melt pocket. Maskelynite or feldspathic glass co...
#1Hejiu Hui (ND: University of Notre Dame)H-Index: 9
#2Yunbin Guan (California Institute of Technology)H-Index: 29
Last.Gordon R. Osinski (UWO: University of Western Ontario)H-Index: 33
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Knowing the amount and timing of water incorporation into the Moon has fundamental implications for our understanding of how the Earth–Moon system formed. Water has been detected in lunar samples but its abundance, distribution and origin are debated. To address these issues, we report water concentrations and hydrogen isotope ratios obtained by secondary ion mass spectrometry (SIMS) of plagioclase from ferroan anorthosites (FANs), the only available lithology thought to have crystallized direct...
#1C.R. Kuchka (U of A: University of Alberta)H-Index: 1
#2Christopher D. K. Herd (U of A: University of Alberta)H-Index: 24
Last.Yang Liu (California Institute of Technology)H-Index: 28
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We apply an array of in situ analytical techniques, including electron and Raman microscopy, electron and ion probe microanalysis, and laser ablation mass spectrometry to the Tissint martian meteorite in order to find and elucidate a geochemical signature characteristic of low-temperature alteration at or near the martian surface. Tissint contains abundant shock-produced quench-crystallized melt pockets containing water in concentrations ranging from 73 to 1730 ppm; water content is positively c...
#1Francis M. McCubbinH-Index: 32
#2Yang LiuH-Index: 28
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#1Yang Liu (UT: University of Tennessee)H-Index: 28
#2Ioannis Baziotis (UT: University of Tennessee)H-Index: 9
Last.Lawrence A. Taylor (UT: University of Tennessee)H-Index: 60
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The Tissint meteorite is a geochemically depleted, olivine-phyric shergottite. Olivine megacrysts contain 300–600 μm cores with uniform Mg# (~80 ± 1) followed by concentric zones of Fe-enrichment toward the rims. We applied a number of tests to distinguish the relationship of these megacrysts to the host rock. Major and trace element compositions of the Mg-rich core in olivine are in equilibrium with the bulk rock, within uncertainty, and rare earth element abundances of melt inclusions in Mg-ri...
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