Molecular hydrogen emission from protoplanetary disks
School of Physics and Astronomy, The University of Manchester, PO Box 88, Manchester M60 1QD, UK e-mail: email@example.com
Accepted: 21 April 2005
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.
Key words: line: formation / molecular processes / radiative transfer / planetary systems: protoplanetary disks
© ESO, 2005