Turbulence plays a key role in determining what types of planets can form in a disk. We are finally on the verge of measuring this property for the first time using CO spectral lines, but it will only work if we factor in how quickly CO can be depleted.
My name is Protoplanetary Disk Mass. I am important for determining what types of planets can form, where they can form, and how quickly they can form. Signed Protoplanetary Disk Mass.
Characterizing planets through direct imaging is no easy task! But today’s authors offer a work-around formula, which estimates the crucial parameter of planetary mass from protoplanetary disk observations. In this astrobite, we discuss ‘The Theory’ and ‘The Practice’ of their cool equation.
The image of the protoplanetary disk around HL Tau illustrating ring structures triggered a huge “WOW!”. Read on and get convinced by recent observations of TW Hya that ring structures seem to be rule rather than the exception.
The authors of today’s paper show that the locations of the protoplanetary gaps in HL Tau are to be expected from the condensation points of common ices in the disk.