The structure of high-velocity gas in Orion and the possible role of IRc9

Details The structure of high-velocity gas in Orion and the possible role of IRc9 The structure of high-velocity gas in Orion and the possible role of IRc9

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...281..205b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 281, June 1, 1984, p. 205-208.

Astronomy and Astrophysics

Astrophysics

11

Infrared Stars, Interstellar Gas, Molecular Clouds, Orion Nebula, Stellar Winds, Astronomical Models, Gas Flow, Pre-Main Sequence Stars, Spatial Distribution, Stellar Flares, T Tauri Stars, Velocity Distribution

Scientific paper

The spatial and velocity distribution of shocked gas in the Orion molecular cloud has been studied in detail through observations of near-infrared and middle-infrared H2 lines. It is argued that the observed structure requires either an asymmetric outflow or an inhomogeneous ambient molecular cloud, and that the second explanation appears the more likely. It is suggested that mild activity by IRc9, such as a T Tauri type wind or FU Orionis type flare, would be consistent with its apparent nature and could have caused the necessary density structure in the cloud.

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