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3D-Numerical Simulations of Magnetic Field Evolution in the Turbulent Interstellar Gas

Published online by Cambridge University Press:  19 July 2016

K. Otmianowska-Mazur  and
M. Urbanik
K. Otmianowska-Mazur
Affiliation:
Astronomical Observatory of Jagiellonian University, Orla 171, 30-244 Cracow, Poland
M. Urbanik
Affiliation:
Astronomical Observatory of Jagiellonian University, Orla 171, 30-244 Cracow, Poland

Abstract

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A fully three-dimensional kinematic model is applied to simulate the evolution of the magnetic field in a small (120 pc in size) volume of the turbulent interstellar medium (ISM) in the presence of the field diffusion. The turbulent motions arc approximated by a sequence of non-overlapping in time vortices, which have the form of the rotating (with a non-zero hclicity) columns much longer than the parcel size. They moved vertically and at the inclination of ±30° to the galactic plane. The resulting magnetic field structure closely resembles a fragment of a classical twisted flux tube, well-ordered over the whole parcel of the ISM.

Keywords

galaxiesmagnetic fieldsturbulent gasnumerical simulations
Type
9. Magnetohydrodynamic Phenomena in the Interstellar Medium Related to Dynamo Processes
Information
Symposium - International Astronomical Union , Volume 157: The Cosmic Dynamo , 1993 , pp. 405 - 409
Copyright
Copyright © Kluwer 1993 

References

Bayly, B., Childress, S.: 1989, Geophys. Astrophys. Fluid Dyn. 49, 23 CrossRefGoogle Scholar
Otmianowska-Mazur, K., Urbanik, M., Terech, A.: 1992, Geophys. Astrophys. Fluid Dyn. , in press Google Scholar
Ruzmaikin, A. A., Shukurov, A. M., Sokoloff, D. D.: 1988, Magnetic Fields of Galaxies , Astrophysics and Space Science Library, Kluwer Academic Publishers: Dordrecht Google Scholar