mcdust: A 2D Monte Carlo code for dust coagulation in protoplanetary disks

The Solar System and other planetary systems are formed in a disk of gas and dust around the young, forming central star, called a protoplanetary disk.The micron-sized particles collide and grow through several processes to form the planetary architectures as we see them today.The overall gas dynamics, the interaction between the gas and dust, and the collisions between the dust particles leave an imprint on the formation pathways of the planets and, therefore, on life.Recent observations with telescopes such as ALMA (Andrews et al., 2018) show a diversity of dust structures in protoplanetary disks, and it is imperative that we have models that are able to describe the observations and, more generally, to help move forward towards the goal of an end-to-end planet formation theory.We present mcdust, a parallel Monte Carlo code aimed at modelling the evolution of dust in protoplanetary disks to better understand the dust size distributions and dust collisional evolution.