Over the past two decades, large strides have been made in the field of planet formation. Yet
fundamental questions remain. Here we review our state of understanding of five …

Planets form and obtain their compositions in dust-and gas-rich disks around young stars,
and the outcome of this process is intimately linked to the disk chemical properties. The …

The Molecules with ALMA at Planet-forming Scales (MAPS) Large Program provides a
unique opportunity to study the vertical distribution of gas, chemistry, and temperature in the …

Protoplanetary disks are known to possess a variety of substructures in the distribution of
their millimetre-sized grains, predominantly seen as rings and gaps, which are frequently …

The gas-phase CO abundance (relative to hydrogen) in protoplanetary disks decreases by
up to two orders of magnitude from its interstellar medium value of∼ 10− 4, even after …

We explore the dynamical structure of the protoplanetary disks surrounding HD 163296 and
MWC 480 as part of the Molecules with ALMA at Planet-forming Scales (MAPS) large …

The growth of a planetary core by pebble accretion stops at the so-called pebble isolation
mass, when the core generates a pressure bump that traps drifting pebbles outside its orbit …

Detecting planets in the early stages of formation is key to reconstructing the history and
diversity of fully developed planetary systems. The aim of this work is to identify potential …

Context. The specific location from where molecules emit in a protoplanetary disk depends
on the system properties. Therefore, directly constraining the emitting regions radially …

The “Grand Tack” model proposes that the inner Solar System was sculpted by the giant
planets' orbital migration in the gaseous protoplanetary disk. Jupiter first migrated inward …