Shocked Molecular Hydrogen from RNO91

We report the detection of the H2 v=1-0 S(1) line at 2.122um, from RNO91 in the L43 dark cloud, which is known to be a T Tauri star surrounded by a 1700AU disk structure (containing ices) and a weak outflow. The non-detection of the H2 v=2-1 S(1) line at 2.247um suggests shock excitation rather than...

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Bibliographic Details
Published inarXiv.org
Main Authors Nanda Kumar, M S, Anandarao, B G, Davis, C J
Format Paper
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 13.03.1999
Subjects
Emission
Fluorescence
Knots
Mass flow rate
Outflow
T Tauri stars
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Summary:We report the detection of the H2 v=1-0 S(1) line at 2.122um, from RNO91 in the L43 dark cloud, which is known to be a T Tauri star surrounded by a 1700AU disk structure (containing ices) and a weak outflow. The non-detection of the H2 v=2-1 S(1) line at 2.247um suggests shock excitation rather than fluorescence. The emission is extended spatially up to 9arcsec in the north-south direction. The line intensity peak (FWHM 3arcsec) corresponds to the star RNO91 which is embedded in a cocoon of gas and dust. The observed H2 emission from this cocoon may be attributed to embedded Herbig-Haro like knots. The H2 line flux in the central 2"X3"is estimated to be 7X10^{-14} ergs/sec/cm^{2}, which indicates a mass flow rate of 4X10^{-8} M_{sun}/yr. Furthermore, narrow band image taken through H2 1-0 S(1) filter is presented, which reveal a tilted disk and bipolar outflow structure that agrees with earlier observations and models. We show that this disk/outflow system is a unique case.
ISSN:2331-8422