The spatial distribution, age distribution and kinematics of T Tauri stars, both close to and widely distributed around active clouds, are considered using simple models of T Tauri dispersal. Models are compared to observations in and around the nearby cloud complexes, in particular the recent discovery of widely scattered young stars from the ROSAT All-Sky Survey. We suggest the dispersal of T Tauri stars has two major causes: slow isotropic drifting of stars away from long-lived star forming clouds, and star formation in short-lived rapidly moving cloudlets associated with large-scale turbulent motions of molecular cloud complexes. A third mechanism for dispersal, dynamical ejection of high velocity T Tauri stars, appears to be less important. Other implications include: star formation in at least one cloud (Chamaeleon I) has been continuous for star formation efficiencies of clouds may often be 20% or higher; a large fraction of low-mass stars may form in small shoft-lived cloudlets each producing no more than a few stars; and T Tauri kinematics support molecular evidence for large-scale turbulence in molecular clouds. A full presentation of this study appears in Feigelson (1996).
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10 February 1997
The seventh astrophysical conference: Star formation, near and far
14-16 Oct 1996
College Park, Maryland (USA)
Research Article|
February 10 1997
Dispersed T Tauri stars and galactic star formation
Eric D. Feigelson
Eric D. Feigelson
Department of Astronomy & Astrophysics, Pennsylvania State University, University Park, Pennsylvania 16802
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AIP Conf. Proc. 393, 184–188 (1997)
Citation
Eric D. Feigelson; Dispersed T Tauri stars and galactic star formation. AIP Conf. Proc. 10 February 1997; 393 (1): 184–188. https://doi.org/10.1063/1.52743
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