ACCRETION OF WATER IN CARBONACEOUS CHONDRITES: CURRENT EVIDENCE AND IMPLICATIONS FOR THE DELIVERY OF WATER TO EARLY EARTH Josep M. Trigo-Rodríguez1,2, Albert Rimola3, Safoura Tanbakouei1,3, Victoria Cabedo Soto1,3, and Martin Lee4 1 Institute of Space Sciences (CSIC), Campus UAB, Facultat de Ciències, Torre C5-parell-2ª, 08193 Bellaterra, Barcelona, Catalonia, Spain. E-mail:
[email protected] 2 Institut d’Estudis Espacials de Catalunya (IEEC), Edif.. Nexus, c/Gran Capità, 2-4, 08034 Barcelona, Catalonia, Spain 3 Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Catalonia, Spain. E-mail:
[email protected] 4 School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow G12 8QQ, UK. Manuscript Pages: 37 Tables: 2 Figures: 10 Keywords: comet; asteroid; meteoroid; meteorite; minor bodies; primitive; tensile strength Accepted in Space Science Reviews (SPAC-D-18-00036R3, Vol. Ices in the Solar System) DOI: 10.1007/s11214-019-0583-0 Abstract: Protoplanetary disks are dust-rich structures around young stars. The crystalline and amorphous materials contained within these disks are variably thermally processed and accreted to make bodies of a wide range of sizes and compositions, depending on the heliocentric distance of formation. The chondritic meteorites are fragments of relatively small and undifferentiated bodies, and the minerals that they contain carry chemical signatures providing information about the early environment available for planetesimal formation. A current hot topic of debate is the delivery of volatiles to terrestrial planets, understanding that they were built from planetesimals formed under far more reducing conditions than the primordial carbonaceous chondritic bodies.