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Protoplanetary disks are dust-rich structures around young stars. Thecrystalline and amorphous materials contained within these disks are variablythermally processed and accreted to make bodies of a wide range of sizes andcompositions, depending on the heliocentric distance of formation. Thechondritic meteorites are fragments of relatively small and undifferentiatedbodies, and the minerals that they contain carry chemical signatures providinginformation about the early environment available for planetesimal formation. Acurrent hot topic of debate is the delivery of volatiles to terrestrialplanets, understanding that they were built from planetesimals formed under farmore reducing conditions than the primordial carbonaceous chondritic bodies. Inthis review, we describe significant evidence for the accretion of ices andhydrated minerals in the outer protoplanetary disk. In that distant regionhighly porous and fragile carbon and water-rich transitional asteroids formed,being the parent bodies of the carbonaceous chondrites (CCs). CCs areundifferentiated meteorites that never melted but experienced other physicalprocesses including thermal and aqueous alteration. Recent evidence indicatesthat few of them have escaped significant alteration, retaining unique featuresthat can be interpreted as evidence of wet accretion. Some examples ofcarbonaceous chondrite parent body aqueous alteration will be presented.Finally, atomistic interpretations of the first steps leading to water-mediatedalteration during the accretion of CCs are provided and discussed. From thesenew insights into the water retained in CCs we can decipher the pathways ofdelivery of volatiles to the terrestrial planets.

Accretion of water in carbonaceous chondrites: current evidence and implications for the delivery of water to early Earth