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Paper: Low Mass Star Formation in the Lynds 1641 Molecular Cloud
Volume: 4, Handbook of Star Forming Regions:
Volume I, The Northern Sky
Page: 621
Authors: Allen, L.E.; Davis, C.J.
Abstract: The Lynds 1641 cloud makes up the bulk of Orion A south of the Orion Nebula Cluster. Although it contains no rich clusters comparable to the ONC, it is forming stars in numerous dense molecular cores found primarily along a ridge of gas that extends the length of the cloud (approximately 2.5 degrees). Optical, X-ray, and infrared surveys have detected hundreds of young, predominantly low-mass stars. Most of the protostars are clustered in small groups or aggregates of N=5–40 members, but the more evolved T Tauri stars appear to be located both in and around these aggregates. L 1641 has thus become a case study for the relative importance of “distributed” vs. “clustered” star formation. Recent results from the Spitzer Space Telescope survey of L 1641 confirms the existence of a significant distributed population, in which 44% of the young stars are in low surface density regions of fewer than 10 stars/pc2. L 1641 is extremely rich in molecular outflows and HH–objects, containing as many as 85 molecular outflows and many HH–shocks. Some of the HH flows are quite spectacular and at least a few comprise pc-scale systems, most notably the HH 303/310 outflow, whose largest lobe extends 6.3 pc from the driving star.
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