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Issue A&A
Volume 438, Number 3, August II 2005
Page(s) 923 - 938
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20052809



A&A 438, 923-938 (2005)
DOI: 10.1051/0004-6361:20052809

Molecular hydrogen emission from protoplanetary disks

H. Nomura and T. J. Millar

School of Physics and Astronomy, The University of Manchester, PO Box 88, Manchester M60 1QD, UK
    e-mail: hnomura@kobe-u.ac.jp

(Received 3 February 2005 / Accepted 21 April 2005)

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.


Key words: line: formation -- molecular processes -- radiative transfer -- planetary systems: protoplanetary disks

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