FN Archimer Export Format
PT J
TI A 4,565-My-old andesite from an extinct chondritic protoplanet
BT 
AF Barrat, Jean-Alix
   Chaussidon, Marc
   Yamaguchi, Akira
   Beck, Pierre
   Villeneuve, Johan
   Byrne, David J.
   Broadley, Michael W.
   Marty, Bernard
AS 1:1;2:2;3:3;4:4;5:5;6:5;7:5;8:5;
FF 1:;2:;3:;4:;5:;6:;7:;8:;
C1 Univ Brest, CNRS, IRD, Ifremer, LEMAR, F-29280 Plouzané, France
   Institut de physique du globe de Paris, CNRS, Université de Paris, F-75005 Paris, France
   National Institute of Polar Research, Tachikawa, Tokyo 190-8518, Japan
   CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, F-38400 Saint Martin d'Hères, France
   Université de Lorraine, CNRS, CRPG, F-54000 Nancy, France
C2 UBO, FRANCE
   CNRS, FRANCE
   NIPR, JAPAN
   CNRS, FRANCE
   UNIV LORRAINE, FRANCE
UM LEMAR
IN WOS Cotutelle UMR
   copubli-france
   copubli-univ-france
   copubli-int-hors-europe
IF 12.779
TC 36
UR https://archimer.ifremer.fr/doc/00685/79674/82450.pdf
   https://archimer.ifremer.fr/doc/00685/79674/82451.pdf
LA English
DT Article
DE ;andesitic magmatism;early solar system;planetary differentiation;differentiated meteorites
AB The age of iron meteorites implies that accretion of protoplanets began during the first millions of years of the solar system. Due to the heat generated by 26Al decay, many early protoplanets were fully differentiated with an igneous crust produced during the cooling of a magma ocean and the segregation at depth of a metallic core. The formation and nature of the primordial crust generated during the early stages of melting is poorly understood, due in part to the scarcity of available samples. The newly discovered meteorite Erg Chech 002 (EC 002) originates from one such primitive igneous crust and has an andesite bulk composition. It derives from the partial melting of a noncarbonaceous chondritic reservoir, with no depletion in alkalis relative to the Sun’s photosphere and at a high degree of melting of around 25%. Moreover, EC 002 is, to date, the oldest known piece of an igneous crust with a 26Al-26Mg crystallization age of 4,565.0 million years (My). Partial melting took place at 1,220 °C up to several hundred kyr before, implying an accretion of the EC 002 parent body ca. 4,566 My ago. Protoplanets covered by andesitic crusts were probably frequent. However, no asteroid shares the spectral features of EC 002, indicating that almost all of these bodies have disappeared, either because they went on to form the building blocks of larger bodies or planets or were simply destroyed. 
PY 2021
PD MAR
SO Proceedings Of The National Academy Of Sciences Of The United States Of America
SN 0027-8424
PU Proceedings of the National Academy of Sciences
VL 118
IS 11
UT 000629635100094
DI 10.1073/pnas.2026129118
ID 79674
ER

EF