EPJ Web of Conferences
Volume 102, 2015Summer School “Protoplanetary Disks: Theory and Modeling Meet Observations”
|Number of page(s)||16|
|Published online||23 September 2015|
Gas line observations of disks*
University of Vienna, Department of Astrophysics, Türkenschanzstrasse 17, 1180 Vienna Austria
a e-mail: email@example.com
Published online: 23 September 2015
Gas represents the bulk of the mass content in protoplanetary disks. It is therefore observations of gas that can provide important information of physical structure and chemical evolution of disks. This involves a detailed understanding of the spectroscopic signatures of the gaseous components and the conditions under which their excitation occurs. In the following I provide an introduction to the principles of molecular spectroscopy by discussing the spectral signatures of the most abundant molecular species found in protoplanetary disks. The presentation for each molecule is supplemented by an up-to-date discussion of relevant observations and subsequent constraints on the corresponding physical conditions in protoplanetary disks. A primer to excitation diagrams as a simple but effective tool for accessing the excitation of spectral lines is presented towards the end of the chapter.
© Owned by the authors, published by EDP Sciences, 2015
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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