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arXiv · astro-ph/0505126

Molecular Hydrogen Emission from Protoplanetary Disks

H. Nomura·T. J. Millar
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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.

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H. Nomura, T. J. Millar. 2005-05-06. Molecular Hydrogen Emission from Protoplanetary Disks. https://doi.org/10.1051/0004-6361%3A20052809

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