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A hubble space telescope survey of H emission in the circumstellar environments of young stars

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journal contribution
posted on 24.10.2012, 08:57 by K. France, E. Schindhelm, A. Brown, G. J. Herczeg, H. Abgrall, E. Roueff, Richard D. Alexander, E. A. Bergin, J. M. Brown, J. L. Linsky, H. Yang
The formation timescale and final architecture of exoplanetary systems are closely related to the properties of the molecular disks from which they form. Observations of the spatial distribution and lifetime of the molecular gas at planet-forming radii (a < 10 AU) are important for understanding the formation and evolution of exoplanetary systems. Toward this end, we present the largest spectrally resolved survey of H2 emission around low-mass pre-main-sequence stars compiled to date. We use a combination of new and archival far-ultraviolet spectra from the Cosmic Origins Spectrograph and Space Telescope Imaging Spectrograph instruments on the Hubble Space Telescope to sample 34 T Tauri stars (27 actively accreting Classical T Tauri Stars and 7 non-accreting Weak-lined T Tauri Stars) with ages ranging from ~1 to 10 Myr. We observe fluorescent H2 emission, excited by Lyα photons, in 100% of the accreting sources, including all of the transitional disks in our sample (CS Cha, DM Tau, GM Aur, UX Tau A, LkCa 15, HD 135344B, and TW Hya). The spatial distribution of the emitting gas is inferred from spectrally resolved H2 line profiles. Some of the emitting gas is produced in outflowing material, but the majority of H2 emission appears to originate in a rotating disk. For the disk-dominated targets, the H2 emission originates predominately at a lesssim 3 AU. The emission line widths and inner molecular radii are found to be roughly consistent with those measured from mid-IR CO spectra.

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Citation

Astrophysical Journal, 2012, 756 (2), 171

Version

VoR (Version of Record)

Published in

Astrophysical Journal

Publisher

IOP Publishing LTD

issn

0004-637X

eissn

1538-4357

Copyright date

2012

Available date

24/10/2012

Publisher version

http://iopscience.iop.org/article/10.1088/0004-637X/756/2/171/meta

Language

en

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