Saving Low-mass Planets in Dusty Protoplanetary Disks

He-Feng Hsieh^1,2*, Min-Kai Lin²

¹Institute of Astronomy, National Tsing Hua University, Hsinchu, Taiwan
²Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan

* Presenter:He-Feng Hsieh, email:x.geometric@gmail.com

In standard, gas-dominated disks, low-mass planets undergo rapid inwards migration and are lost to the central star. A key challenge in planet formation theory is, therefore, how to slow down the migrating planets or even reverse their migration directions, so that they could evolve into the present-day observations of planetary systems. Recent researches have found that various dust substructures can develop in dust-laden disks, which could have significant dynamical effects on disk-planet interaction. In this talk, I will present the migration behavior of low-mass planets in dusty protoplanetary disks, obtained from two-fluid two-dimensional hydrodynamic simulations. I will talk about the new stochastic regime applicable to disks with abundant large dust grains, where the planet migration rate and direction becomes chaotic and unpredictable.

Keywords: planet-disk interactions, protoplanetary disks, hydrodynamics