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.
Giant planets take too long to form from large planetesimals. Does including much smaller pebbles fix this problem?
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.
Interstellar space should be littered with debris ejected during the formation of planetary systems—but how much? Engelhardt et al. use solar system surveys and simulations to place an upper limit on the number density of asteroids and comets roaming the Milky Way without a parent star.
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.
In this bite, we talk about observations of substructure in a young circumstellar debris disk. What can the formation of multiple debris dust rings tell us?