FN Archimer Export Format PT J TI Volatile element evolution of chondrules through time BT AF MAHAN, Brandon MOYNIER, Frederic SIEBERT, Julien GUEGUEN, Bleuenn AGRANIER, Arnaud PRINGLE, Emily A. BOLLARD, Jean CONNELLY, James N. BIZZARRO, Martin AS 1:1;2:1,2;3:1,2;4:3,4,5;5:3,4;6:1,6;7:7;8:7;9:1,7; FF 1:;2:;3:;4:;5:;6:;7:;8:;9:; C1 Univ Paris Diderot, Sorbonne Paris Cite, CNRS UMR 7154, Inst Phys Globe Paris, F-75238 Paris 05, France. Inst Univ France, F-75005 Paris, France. Univ Bretagne Occidentale, UMR CNRS 6538, Lab Geosci Ocean, F-29280 Plouzane, France. Inst Univ Europeen Mer, F-29280 Plouzane, France. Inst Univ Europeen Mer, UMS CNRS 3113, F-29280 Plouzane, France. Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. C2 UNIV PARIS 07, FRANCE INST UNIV FRANCE, FRANCE UBO, FRANCE UBO, FRANCE UBO, FRANCE UNIV CALIF SAN DIEGO, USA UNIV COPENHAGEN, DENMARK UM LGO IF 9.58 TC 14 UR https://archimer.ifremer.fr/doc/00638/74979/75756.pdf https://archimer.ifremer.fr/doc/00638/74979/75757.pdf LA English DT Article DE ;cosmochemistry;planetary formation;pebble accretion;Solar System evolution;meteorites AB Chondrites and their main components, chondrules, are our guides into the evolution of the Solar System. Investigating the history of chondrules, including their volatile element history and the prevailing conditions of their formation, has implications not only for the understanding of chondrule formation and evolution but for that of larger bodies such as the terrestrial planets. Here we have determined the bulk chemical composition-rare earth, refractory, main group, and volatile element contents-of a suite of chondrules previously dated using the Pb-Pb system. The volatile element contents of chondrules increase with time from similar to 1 My after Solar System formation, likely the result of mixing with a volatile-enriched component during chondrule recycling. Variations in the Mn/Na ratios signify changes in redox conditions over time, suggestive of decoupled oxygen and volatile element fugacities, and indicating a decrease in oxygen fugacity and a relative increase in the fugacities of in-fluxing volatiles with time. Within the context of terrestrial planet formation via pebble accretion, these observations corroborate the early formation of Mars under relatively oxidizing conditions and the protracted growth of Earth under more reducing conditions, and further suggest that water and volatile elements in the inner Solar System may not have arrived pairwise. PY 2018 PD AUG SO Proceedings Of The National Academy Of Sciences Of The United States Of America SN 0027-8424 PU Natl Acad Sciences VL 115 IS 34 UT 000442351000045 BP 8547 EP 8552 DI 10.1073/pnas.1807263115 ID 74979 ER EF