Observational diagnostics of gas in protoplanetary disks
Abstract
Protoplanetary disks are composed primarily of gas (99% of the mass). Nevertheless, relatively few observational constraints exist for the gas in disks. In this review, I discuss several observational diagnostics in the UV, optical, near-IR, mid-IR, and (sub)-mm wavelengths that have been employed to study the gas in the disks of young stellar objects. I concentrate in diagnostics that probe the inner 20 AU of the disk, the region where planets are expected to form. I discuss the potential and limitations of each gas tracer and present prospects for future research.
Keywords
Cite
@article{arxiv.0911.2271,
title = {Observational diagnostics of gas in protoplanetary disks},
author = {Andres Carmona},
journal= {arXiv preprint arXiv:0911.2271},
year = {2015}
}
Comments
Review written for the proceedings of the conference "Origin and Evolution of Planets 2008", Ascona, Switzerland, June 29 - July 4, 2008. Date manuscript: October 2008. 17 Pages, 6 graphics, 134 references