11:00 AM - 1:00 PM
[PAE17-P01] Radiation Hydrodynamics Simulations of Protoplanetary Disks : Dust-deficient Case
Keywords:protoplanetary disk, planet formation, radiation hydrodynamics simulation
We perform radiation hydrodynamics simulations of photoevaporation of protoplanetary disks.
Photoeaporation is a disk dispersal process, which is caused by high-energy radiation.
Photoelectric effect of dust grains by UV radiation is an important process for disk heating, but as a disk evolves, the amount of dust grains decreases.
We run a series of simulations with varying the dust-to-gas mass ratio in a range D=10-1-10-8.
We show that H2 pumping and X-ray heating mainly contribute to the disk heating in case of D<10-3 and photoelectric effect mainly heats the gas in D>10-3 cases.
The mass-loss profile changes significantly with respect to the main heating process.
The outer disk is more efficiently dispersed when photoelectric effect is the main heating source.
Our results suggest that dust-deficient disks are dispersed by photoevaporation from the inner disk region and shapes the disk mass-loss profile.
Photoeaporation is a disk dispersal process, which is caused by high-energy radiation.
Photoelectric effect of dust grains by UV radiation is an important process for disk heating, but as a disk evolves, the amount of dust grains decreases.
We run a series of simulations with varying the dust-to-gas mass ratio in a range D=10-1-10-8.
We show that H2 pumping and X-ray heating mainly contribute to the disk heating in case of D<10-3 and photoelectric effect mainly heats the gas in D>10-3 cases.
The mass-loss profile changes significantly with respect to the main heating process.
The outer disk is more efficiently dispersed when photoelectric effect is the main heating source.
Our results suggest that dust-deficient disks are dispersed by photoevaporation from the inner disk region and shapes the disk mass-loss profile.