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Turbulence in high latitude molecular clouds

Published online by Cambridge University Press:  01 August 2006

S. N. Shore ,
T. N. LaRosa ,
L. Magnani ,
R. J. Chastain  and
F. Costagliola
S. N. Shore
Affiliation:
Dipartimento di Fisica “Enrico Fermi”, Università di Pisa, Pisa 56127, Italy email: [email protected], [email protected] INFN-Sezione di Pisa
T. N. LaRosa
Affiliation:
Department of Biological and Physical Sciences, Kennesaw State University, Kennesaw, [email protected]
L. Magnani
Affiliation:
Departiment of Physics, University of Georgia, Athens, GAUSA email: [email protected]
R. J. Chastain
Affiliation:
Departiment of Physics, University of Georgia, Athens, GAUSA email: [email protected]
F. Costagliola
Affiliation:
Dipartimento di Fisica “Enrico Fermi”, Università di Pisa, Pisa 56127, Italy email: [email protected], [email protected]
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Abstract

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We summarize a continuing investigation of turbulence in high-latitude translucent molecular clouds. These low mass (~50–100 M), nearby (~100 pc), non-star forming clouds appear to be condensing out of the atomic cirrus. Unlike star-forming clouds the velocity fields in the clouds must be driven by external processes. Our detailed mapping of the clouds MBM 3,16 and 40 indicates that the dynamics in these clouds result from the combination of shear-flow and thermal instabilities, not shocks. These clouds also show coherent structures, non-Gaussian PDFs but no clear velocity-size relation. Lastly, the energetics of these clouds indicate that radiative loss may terminate the cascade before local heating takes place.

Keywords

turbulencehydrodynamicsinstabilitiesISM: kinematics and dynamicsISM: cloudsradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 17 - 23
Copyright
Copyright © International Astronomical Union 2007

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