Proto-planetary discs, the birth environment of planets, are an example of a structure
commonly found in astrophysics, accretion discs. Identifying the mechanism responsible for …

While dust disks around optically visible, Class II protostars are found to be vertically thin,
when and how dust settles to the midplane are unclear. As part of the Atacama Large …

The envelopes and disks that surround protostars reflect the initial conditions of star and
planet formation and govern the assembly of stellar masses. Characterizing these structures …

Protoplanetary disks exhibit a vertical gradient in angular momentum, rendering them
susceptible to the vertical shear instability (VSI). The most important condition for the onset …

The streaming instability (SI) is a leading candidate for planetesimal formation, which can
concentrate solids through two-way aerodynamic interactions with the gas. The resulting …

Abstract We present James Webb Space Telescope imaging from 2 to 21 μm of the edge-on
protoplanetary disk around the embedded young star IRAS04302+ 2247. The structure of …

Context. Understanding the formation of substructures in protoplanetary disks is vital for
gaining insights into dust growth and the process of planet formation. Studying these …

In the theory of protoplanetary disk turbulence, a widely adopted ansatz, or assumption, is
that the turnover frequency of the largest turbulent eddy, Ω L, is the local Keplerian …

The amount of turbulence in protoplanetary discs around young stars is critical for
determining the efficiency, timeline, and outcomes of planet formation. It is also difficult to …

The streaming instability, a promising mechanism to drive planetesimal formation in dusty
protoplanetary discs, relies on aerodynamic drag naturally induced by the background radial …