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Vorticity from irrotationally forced flow

Published online by Cambridge University Press:  12 August 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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In the interstellar medium the turbulence is believed to be forced mostly through supernova explosions. In a first approximation these flows can be written as a gradient of a potential being thus devoid of vorticity. There are several mechanisms that could lead to vorticity generation, like viscosity and baroclinic terms, rotation, shear and magnetic fields, but it is not clear how effective they are, neither is it clear whether the vorticity is essential in determining the turbulent diffusion acting in the ISM. Here we present a study of the role of rotation, shear and baroclinicity in the generation of vorticity in the ISM.

Keywords

Galaxies: magnetic fields – ISM: bubbles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 375 - 376
Copyright
Copyright © International Astronomical Union 2011

References

Beck, R., Brandenburg, A., Moss, D., Shukurov, A., & Sokoloff, D. 1996, ARA&A, 34, 155Google Scholar
Brandenburg, A. & Del Sordo, F. 2009 in Turbulent diffusion and galactic magnetism, ed. Highlights of Astronomy, Vol. 15 (E. de Gouveia Dal Pino), (in press) CUP, arXiv:0910.0072CrossRefGoogle Scholar
Del Sordo, F. & Brandenburg, A. 2010, A&A, submitted, arXiv:1008:5281Google Scholar
Mee, A. J. & Brandenburg, A. 2006, MNRAS, 370, 415CrossRefGoogle Scholar