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Title:
Low Mass Star Formation in the Lynds 1641 Molecular Cloud
Authors:
Allen, L. E.; Davis, C. J.
Publication:
Handbook of Star Forming Regions, Volume I: The Northern Sky ASP Monograph Publications, Vol. 4. Edited by Bo Reipurth, p.621
Publication Date:
12/2008
Origin:
ASP
Bibliographic Code:
2008hsf1.book..621A

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=3D5--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 fo= r 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/pc^2. 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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