Journal
ASTRONOMY & ASTROPHYSICS
Volume 438, Issue 3, Pages 923-U97Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20052809
Keywords
line : formation; molecular processes; radiative transfer; planetary systems : protoplanetary disks
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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.
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