During the first million years of evolution, nascent planetary
\nsystems are embedded in dense disk\u00ad-shaped clouds of gas. These
\ncircumstellar disks are home to a myriad of hydrodynamical processes,
\nwhich bring about turbulence and the emergence of viscous\u00ad-like behavior,
\nenabling accretion of gas onto the protostar. Meanwhile, micron\u00adsize dust
\ngrains embedded in the disk are growing through coagulation onto pebbles
\nand rocks. Turbulence has a positive effect on these small solids,
\nconcentrating them into transient high pressure regions for long enough to
\nachieve gravitational collapse into km\u00ad-sized bodies, forming the first
\nplanetesimals. Giant storm systems in the disk, similar to Jupiter’s Great
\nRed Spot, may exist in quiescent zones of the disk. These are even more
\nprone to collecting solid material, producing the first terrestrial
\nplanets and cores of giant planets. In this talk I will discuss the state
\nof the art and recent advances in the field of planet formation, as well
\nas pressing problems such as the asymmetries observed in ALMA images of
\ncircumstellar disks, and how to interpret them.<\/p>\n","protected":false},"excerpt":{"rendered":"
During the first million years of evolution, nascent planetary systems are embedded in dense disk\u00ad-shaped clouds of gas. These circumstellar disks are home to a myriad of hydrodynamical processes, which bring about turbulence and the emergence of viscous\u00ad-like behavior, enabling accretion of gas onto the protostar. Meanwhile, micron\u00adsize dust grains embedded in the disk are … <\/p>\n