Molecular Hydrogen Emission from Protoplanetary Disks
Astrophysics
2009-11-11 v1
Abstract
We have modeled self-consistently the density and temperature profiles of gas and dust in protoplanetary disks, taking into account irradiation from a central star. Making use of this physical structure, we have calculated the level populations of molecular hydrogen and the line emission from the disks. As a result, we can reproduce the observed strong line spectra of molecular hydrogen from protoplanetary disks, both in the ultraviolet (UV) and the near-infrared, but only if the central star has a strong UV excess radiation.
Cite
@article{arxiv.astro-ph/0505126,
title = {Molecular Hydrogen Emission from Protoplanetary Disks},
author = {H. Nomura and T. J. Millar},
journal= {arXiv preprint arXiv:astro-ph/0505126},
year = {2009}
}
Comments
19 pages, accepted for publication in Astronomy and Astrophysics