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How can vorticity be produced in irrotationally forced flows?

Published online by Cambridge University Press:  08 June 2011

Fabio Del Sordo  and
Axel Brandenburg
Fabio Del Sordo
Affiliation:
NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden; and Department of Astronomy, Stockholm University, SE 10691 Stockholm, Sweden
Axel Brandenburg
Affiliation:
NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden; and Department of Astronomy, Stockholm University, SE 10691 Stockholm, Sweden
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Abstract

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A spherical hydrodynamical expansion flow can be described as the gradient of a potential. In that case no vorticity should be produced, but several additional mechanisms can drive its production. Here we analyze the effects of baroclinicity, rotation and shear in the case of a viscous fluid. Those flows resemble what happens in the interstellar medium. In fact in this astrophysical environment supernovae explosion are the dominant flows and, in a first approximation, they can be seen as spherical. One of the main difference is that in our numerical study we examine only weakly supersonic flows, while supernovae explosions are strongly supersonic.

Keywords

Galaxies: magnetic fields – ISM: bubbles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 373 - 375
Copyright
Copyright © International Astronomical Union 2011

References

Beck, R., Brandenburg, A., Moss, D., Shukurov, A., & Sokoloff, D.ARA&A, 1996, 34, 155Google Scholar
Brandenburg, A. & Del Sordo, F. (in press) 2009 Turbulent diffusion and galactic magnetism Highlights of Astronomy, Vol. 15 de Gouveia Dal Pino, E. CUP, arXiv:0910.0072Google Scholar
Del Sordo, F. & Brandenburg, A. 2010, A&A, submitted, arXiv:1008.5281Google Scholar
Mee, A. J. & Brandenburg, A.MNRAS, 2006, 370, 415CrossRefGoogle Scholar