2005/08/01 by Inga Kamp, Cornelis P. Dullemond, Michiel Hogerheijde +1 · 5 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Emission spectrum #Line (geometry) #Planetary system #Protoplanetary disk #Stars #T Tauri star #Thermal #Thermal emission #astro-ph
paper · pdf · doi:10.1017/s1743921306007393
published in Proceedings of the International Astronomical Union 1(S231), 377-386 (Cambridge University Press) · 10 pages, 6 figures, to be published in the conferences proceedings of the IAU Symposium 231 on Astrochemistry
openalex publication_date 2005/08/01 · arxiv created 2005/09/21 · arxiv updated 2015/06/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 discuss here the differences in chemistry, thermal structure 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.