Chemistry and line emission of outer protoplanetary disks
arXiv:astro-ph/0509643 · doi:10.1017/S1743921306007393
Abstract
The structure and chemistry of protoplanetary disks depends strongly on the nature of the central star around which it has formed. The dust temperature is mainly set by the stellar luminosity, while the chemistry of the upper disk layers depends on the amount of intercepted UV and X-ray flux. We will study the differences in chemistry, thermal sturcture and line emission around Herbig Ae/Be, T Tauri stars and low mass M dwarfs. Predictions will be made for future observations with SOFIA and Herschel.
10 pages, 6 figures, to be published in the conferences proceedings of the IAU Symposium 231 on Astrochemistry
Cited by in corpus (5)
- Molecular Hydrogen Emission from Protoplanetary Disks II. Effects of X-ray Irradiation and Dust Evolution
- Line Emission from Gas in Optically Thick Dust Disks around Young Stars
- Radiation thermo-chemical models of protoplanetary disks II. Line diagnostics
- Chemistry and line emission from evolving Herbig Ae disks
- H 21cm emission as a tracer of gas during the evolution from protoplanetary to debris disks