How can vorticity be produced in irrotationally forced flows?

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...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2010-09, Vol.6 (S274), p.373-375
Main Authors: Sordo, Fabio Del, Brandenburg, Axel
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics
Contributed Papers
Fluid mechanics
Galaxies: magnetic fields
ISM: bubbles
Magnetic fields
Stars & galaxies
Turbulent flow
Citations: Items that this one cites
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Summary: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.
ISSN:1743-9213
1743-9221
1743-9221
DOI:10.1017/S1743921311007307