TY  - GEN
N2  - Protoplanetary discs are the natal environments of planets and contain the building blocks from which planets form. It is therefore of crucial importance to understand how the dust growth and evolution shapes discs and what the implications are for planet formation. At the same time, our observational capabilities have improved in the recent years, providing us with more constraints that need to be considered in our theoretical studies. The goal of this thesis is to determine through numerical simulations how the dust shapes the (thermal) structure of the protoplanetary disc, how the conditions within the disc affect the growth of planets and how the forming planets affect the dust mass itself. We find that opacity models based only on micrometer-sized dust grains might not be a good approximation to simulate the disc's structure, especially for discs with significant viscous heating. There is a trade-off between the pebble isolation mass and the planetary growth timescale, which is important for the modeling of the growth of super-Earths via pebble accretion. 
We also find that the most favorable conditions for giant planet formation are high disc mass, early formation, and a large enough disc, however we conclude that their formation is mainly the outcome of a combination of beneficial factors or lack of adverse ones. Our findings strengthen the hypothesis that planet formation has already happened or is ongoing in Class II discs and we show that the assumption of an optically thin emission significantly underestimates the total dust mass in discs, if a giant planet is present that traps dust exterior to its orbit. We conclude that we should use the ever-increasing and improved observational data to better constrain the protoplanetary disc properties and connect the dots better to the observed exoplanets, based on our more sophisticated theoretical models.
Y1  - 2023///
UR  - https://archiv.ub.uni-heidelberg.de/volltextserver/33319/
ID  - heidok33319
TI  - How dust shapes protoplanetary discs and the implications to planet formation
CY  - Heidelberg
A1  - Savvidou, Sofia
AV  - public
ER  -