Click here to download a pdf of the talk I gave at the 235th AAS:
Click below to download a high-resolution pdf (~8 MB) of the poster I presented at the 2019 GRC on Origin of Solar Systems in June 2019:
The animations below are movies of the simulations shown in Fig. 5 of the poster.
Fig. 5a: In the model with local chemistry only, the gas phase CO abundance in the upper regions hardly changes over 3 Myr. In the midplane, CO is processed more efficiently, forming CH3OH in the outer regions and CO2 around/inside the CO snowline. This is consistent with findings of Bosman et al. (2018) and Schwarz et al. (2018).
Fig. 5b: When diffusive tranport of vapor species and small grains is included, the picture changes. CO can be removed from the gas-phase by cycling it to the midplane (where it is chemically processed) and reaction products (like CH3OH) spread through the disk, increasing their abundance away from the midplane.
Fig. 5c: In this model, chemistry is ignored but dust coagulation (i.e., the formation, settling, and radial drift of pebbles) is included. Now, CO becomes depleted because it can be sequestered on large solids in the midplane. Pebbles drifting through the snowline enrich the inner regions in CO gas (consistent with Krijt et al. 2018).
Fig. 5d: In the most complete model presented here, chemistry, pebble formation, and material transport are all included self-consistently. The resulting behavior is a mix of Figs. 5b and 5c. With chemical processing and midplane sequestration both operating, the gas-phase CO abundance between ~50-125 au is reduced dramatically within 3 Myr. As in Fig. 5c, a plume of CO vapor appears inside the snowline, though its strength is reduced.