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Turbulence in high latitude molecular clouds

Published online by Cambridge University Press:  01 August 2006

S. N. Shore
Affiliation:
Dipartimento di Fisica “Enrico Fermi”, Università di Pisa, Pisa 56127, Italy email: shore@df.unipi.it, francesco.costagliola@df.unipi.it INFN-Sezione di Pisa
T. N. LaRosa
Affiliation:
Department of Biological and Physical Sciences, Kennesaw State University, Kennesaw, GAUSAted@avatar.kennesaw.edu
L. Magnani
Affiliation:
Departiment of Physics, University of Georgia, Athens, GAUSA email: loris@physast.uga.edu
R. J. Chastain
Affiliation:
Departiment of Physics, University of Georgia, Athens, GAUSA email: loris@physast.uga.edu
F. Costagliola
Affiliation:
Dipartimento di Fisica “Enrico Fermi”, Università di Pisa, Pisa 56127, Italy email: shore@df.unipi.it, francesco.costagliola@df.unipi.it
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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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

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