Twentieth International Conference on Technology, Knowledge, and Society

Abstract

Planets and planetesimals acquire their chemical composition (i.e volatiles) through ice and gas accretion into a planet formation environment, called protoplanetary disks, around young stars. The composition of planets will depend on the distributions of those volatiles (in icy grain mantles and gas) across the disk, which depend on the disk temperature profiles. If the ices are present as a mixture, “entrapment” of more volatile species in less volatile ice matrices will change the prediction of solid composition, since entrapment now allows hyper-volatiles to be present in solid form closer to the star. Availability of volatiles in solid form closer to the star will change the chemistry of planet core and atmosphere composition. More recently, we showed that in addition to water, the major space molecule, entrapment in carbon dioxide ice may be important for the distribution of volatiles in disks. Furthermore, recent quantitative works which are in publication process, showed that a binary mixture of CO2 or H2O ice matrix for a range of four hyper-volatiles (CO, CH4, N2 and Ar) entrap those volatiles with the same efficiencies, as well as different ice matrices (NH3, CH3OH, C2H6) and multi-components ices. I present the overall entrapment process present and reproduced in planet formation regions and how it is impacting the chemical availability for astrophysical bodies. I correlate this laboratory work with the James Webb Telescope observations.