hydro

• What we (my Ph.D. student, Shangjia Zhang, and myself) planned:

a. Given 1) a radial intensity profile with gaps/rings, 2) assumed dust size distribution, 3) stellar and disk properties (surface density, H/R, alpha), we can estimate the planet mass.

b. Get the population of potential planets with this method.

• What we have done:

a. Extensive 2-D hydrodynamical simulations with dust particles (ranging over 6 orders of magnitude in size) have been carried out. The simulations are run to 1000 planetary orbits.

b. Making contour plots, and gas and dust surface density profiles.

• What we are working on

a. Generating some fitting formula for the gas surface density for Kees (this week).

b. Calculating the submm intensity profiles along the radial direction. (this and next week)

• What we need from other people: a. the opacity for different sized dust particles. b. the disk radial temperature profile. c. the disk gas surface density profile.