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. The author suggests that mild activity by IRc 9 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.
|Pages (from-to)||205 - 8|
|State||Published - Jun 1984|
- infrared sources (astronomical)
- interstellar matter
- stellar winds