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Chemistry and Line Emission of Outer Protoplanetary Disks

Published online by Cambridge University Press:  21 March 2006

Inga Kamp ,
Cornelis P. Dullemond ,
Michiel Hogerheijde  and
Jesus Emilio Enriquez
Inga Kamp
Affiliation:
Space Telescope Division of ESA, STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA email: kamp@stsci.edu
Cornelis P. Dullemond
Affiliation:
Max-Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Michiel Hogerheijde
Affiliation:
Leiden Observatory, PO Box 9513, NL-3200 RA Leiden, The Netherlands
Jesus Emilio Enriquez
Affiliation:
University of Texas at El Paso, PSCI 210, 500 W. University Ave., El Paso, TX 79968, USA
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Abstract

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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.

Keywords

astrochemistry — planetary systems: protoplanetary disks — radiative transfer — solar system: formation — X-rays: stars — ultraviolet: stars