Molecular Hydrogen Emission from Protoplanetary Disks

H. Nomura; TJ Millar

doi:10.1051/0004-6361:20052809

Molecular Hydrogen Emission from Protoplanetary Disks

H. Nomura, TJ Millar

Research output: Contribution to journal › Article › peer-review

122 Citations (Scopus)

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.

Original language	English
Pages (from-to)	923-938
Number of pages	16
Journal	Astronomy and Astrophysics
Volume	438
Issue number	3
DOIs	https://doi.org/10.1051/0004-6361:20052809
Publication status	Published - Aug 2005

ASJC Scopus subject areas

Space and Planetary Science

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title = "Molecular Hydrogen Emission from Protoplanetary Disks",

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.",

author = "H. Nomura and TJ Millar",

year = "2005",

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AU - Nomura, H.

AU - Millar, TJ

PY - 2005/8

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N2 - 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.

AB - 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.

UR - https://www.scopus.com/pages/publications/23744484402

U2 - 10.1051/0004-6361:20052809

DO - 10.1051/0004-6361:20052809

M3 - Article

SN - 0004-6361

VL - 438

SP - 923

EP - 938

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 3

ER -

Molecular Hydrogen Emission from Protoplanetary Disks

Abstract

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