Molecular hydrogen emission from protoplanetary disks

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 di...

Full description

Saved in:
Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2005-08, Vol.438 (3), p.923-938
Main Authors: Nomura, H., Millar, T. J.
Format: Article
Language:English
Subjects:
line: formation
molecular processes
planetary systems: protoplanetary disks
radiative transfer
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary: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.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361:20052809