The behavior of Li and B in lunar mare basalts during crystallization, shock, and thermal metamorphism: Implications for volatile element contents of martian basalts

2006 ◽  
Vol 91 (10) ◽  
pp. 1553-1564 ◽  
Author(s):  
J. Chaklader ◽  
C.K. Shearer ◽  
L.E. Borg
Keyword(s):  
Volatile Element ◽  
Thermal Metamorphism ◽  
Lunar Mare ◽  
Element Contents ◽  
Mare Basalts

Thermal Metamorphism of Primitive Meteorites—XII. The Enstatite Chondrites Revisited

2005 ◽  
Vol 2 (3) ◽  
pp. 215 ◽  
Author(s):  
Ming-Sheng Wang ◽  
Michael E. Lipschutz
Keyword(s):  
Radiochemical Neutron Activation Analysis ◽  
Parent Material ◽  
Ordinary Chondrites ◽  
Terrestrial Environment ◽  
Volatile Element ◽  
Thermal Metamorphism ◽  
Report Data ◽  
Element Contents ◽  
Type 3 ◽  
Solid Bodies

Environmental Context.The first Solar System material condensed 4.567 billion years ago, rapidly forming planetesimals—solid bodies that might combine to form planets (accretion) or survive as asteroidal meteorites. Earth’s main accretion ended within the next 30 million years, but subsequent high temperatures essentially erased evidence of this history. However, heating in these early episodes produced effects uniquely recorded by 14 volatile trace elements. The volatile element composition of chondritic meteorites, whose parent material formed closest to Earth, may thus provide important information about early planetesimal evolution. Abstract.We report data for 14 trace and ultratrace elements—Au, Co, Sb, Ga, Rb, Ag, Cs, Te, Zn, Cd, Bi, Tl, In (ordered by increasing putative nebular volatility)—in 13 enstatite (E) chondrites recovered from Antarctica and two E inclusions in the Kaidun polymict breccia that fell in 1980. These data, determined by radiochemical neutron activation analysis (RNAA), essentially double the amount of information known for E chondrites, whose parent materials formed closest to the Sun in the chondrite-forming nebular region. We discuss here the data for all 29 samples studied. The meteoritic suite studied here includes both representatives of previously rare types—like high-iron EH3 and EH5 individuals—but also unique individuals and previously unknown low-iron, EL3, chondrites. Prior hypothetical assertions by others are corrected by the new data. Volatile element contents of EL3 and EH3 chondrites are variable, but comparable, like those of type 3 ordinary chondrites (i.e. H3, L3, and LL3). Volatile element contents of EH4 chondrites are at least as high as those of the E3 types, in contrast to the lower contents of H4, L4, and LL4 types. Compositionally, E3,4 chondrites reflect only nebular condensation and/or accretion processes. Volatiles in E5 and E6 chondrites—whether of EH, EL or unique ones—are depleted relative to cosmic (i.e. CI1) or E3,4 chondrite abundances. The evidence indicates that E5,6 chondrites compositionally reflect vaporization and loss of volatiles during open-system, thermal metamorphism of their parent(s); this may have been the terrestrial environment during Earth’s formation from early planetesimals. Compositional differences between Antarctic E5,6 chondrites and contemporary falls probably do not reflect weathering during the long residence of these chondrites in Antarctica. They might reflect differences in the starting compositions and/or metamorphic conditions in the parent(s).

Systematics of Ni and Co in olivine from planetary melt systems; lunar mare basalts

1999 ◽  
Vol 84 (3) ◽  
pp. 392-399 ◽  
Author(s):  
J. J. Papike ◽  
G. W. Fowler ◽  
C. T. Adcock ◽  
C. K. Shearer
Keyword(s):  
Lunar Mare ◽  
Mare Basalts

Lunar Mare Basalts: Conference Summary

Eos ◽  
1976 ◽  
Vol 57 (11) ◽  
pp. 823
Author(s):  
R. B. Merill ◽  
L. A. Haskin ◽  
N. J. Hubbard ◽  
G. E. Lofgren ◽  
J. W. Minear ◽  
...  
Keyword(s):  
Conference Summary ◽  
Lunar Mare ◽  
Mare Basalts

A dynamic origin for the global asymmetry of lunar mare basalts

2000 ◽  
Vol 177 (3-4) ◽  
pp. 131-140 ◽  
Author(s):  
Shijie Zhong ◽  
E.M. Parmentier ◽  
Maria T. Zuber
Keyword(s):  
Lunar Mare ◽  
Mare Basalts

scholarly journals Thickness of Lunar Mare Basalts: New Results Based on Modeling the Degradation of Partially Buried Craters

2019 ◽  
Vol 124 (9) ◽  
pp. 2430-2459 ◽  
Author(s):  
Jun Du ◽  
Wenzhe Fa ◽  
Mark A. Wieczorek ◽  
Minggang Xie ◽  
Yuzhen Cai ◽  
...  
Keyword(s):  
Lunar Mare ◽  
Mare Basalts

scholarly journals Young lunar mare basalts in the Chang'e-5 sample return region, northern Oceanus Procellarum

2021 ◽  
Vol 555 ◽  
pp. 116702
Author(s):  
Yuqi Qian ◽  
Long Xiao ◽  
James W. Head ◽  
Carolyn H. van der Bogert ◽  
Harald Hiesinger ◽  
...  
Keyword(s):  
Sample Return ◽  
Lunar Mare ◽  
Mare Basalts

Lunar mare basalts in the Aristarchus region: Implications for the stratigraphic sequence from Clementine UVVIS data

Icarus ◽  
2014 ◽  
Vol 227 ◽  
pp. 132-151 ◽  
Author(s):  
F. Zhang ◽  
Y.L. Zou ◽  
Y.C. Zheng ◽  
X.H. Fu ◽  
Y.C. Zhu
Keyword(s):  
Stratigraphic Sequence ◽  
Lunar Mare ◽  
Mare Basalts

Lu-Hf and Sm-Nd evolution in lunar mare basalts

1984 ◽  
Vol 89 (S02) ◽  
pp. B459 ◽  
Author(s):  
D. M. Unruh ◽  
P. Stille ◽  
P. J. Patchett ◽  
M. Tatsumoto
Keyword(s):  
Lunar Mare ◽  
Mare Basalts

scholarly journals NanoSIMS and EPMA dating of lunar zirconolite

2021 ◽  
Vol 8 (1) ◽  
Author(s):  
Nian Wang ◽  
Qian Mao ◽  
Ting Zhang ◽  
Jialong Hao ◽  
Yangting Lin
Keyword(s):  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Lunar Meteorite ◽  
Geochemical Study ◽  
Lunar Rocks ◽  
Crater Counting ◽  
Resolution Analysis ◽  
Lunar Mare ◽  
Mare Basalts ◽  
Non Destructive

Abstract Zirconolite is a common Zr-rich accessary mineral in mafic rocks. It is also an ideal U–Pb/Pb–Pb chronometer because it commonly contains high U content (mostly 0.1–10 wt%) and negligible initial Pb. However, zirconolite is usually very small (e.g., ~ 1 μm in width) in lunar rocks, requiring a high spatial resolution analysis. We analyzed a single, large (25 μm × 20 μm) grain of zirconolite in lunar meteorite NWA 4485 using Pb–Pb dating by NanoSIMS and U–Th–Pb dating by EPMA. The resultant U–Th–Pb age is 4540 ± 340 Ma (2σ) with a spatial resolution of 1.3 μm. The Pb–Pb age by NanoSIMS is 4348.5 ± 4.8 Ma (2σ) with a spatial resolution of ~ 2 μm, consistent with the age of 4352 ± 10 Ma and 4344 ± 14 Ma reported in the same meteorite and its paired meteorite NWA 4472. Although U–Th–Pb age is somewhat older, it still includes the NanoSIMS results within the analytical uncertainty. This work demonstrates the potential application of the combined EPMA dating and REE analysis of lunar zirconolite, with the benefits of high spatial resolution, non-destructive, and readily accessibility of the instrument. The precision of the EPMA dating (7.6%, 2σ) can be improved by increasing the counting time for Pb, U and Th. We expect to apply this EPMA technique for a quick and non-destructive age survey and geochemical study of zirconolite grains from the lunar mare basalts newly returned by Chang’E-5 mission which landed on a very young (1.2–2.0 Ga by crater-counting chronology) basalt unit in Procellarum KREEP Terrain.

The age of lunar mare basalts south of the Aristarchus Plateau and effects of secondary craters formed by the Aristarchus event

Icarus ◽  
2018 ◽  
Vol 309 ◽  
pp. 45-60 ◽  
Author(s):  
A.C. Stadermann ◽  
M.R. Zanetti ◽  
B.L. Jolliff ◽  
H. Hiesinger ◽  
C.H. van der Bogert ◽  
...  
Keyword(s):  
Lunar Mare ◽  
Mare Basalts
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