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Magnetic field amplification by SN-driven interstellar turbulence

Published online by Cambridge University Press:  20 January 2011

H. Wozniak ,
G. Hensler ,
O. Gressel ,
U. Ziegler  and
D. Elstner
D. Elstner
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
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Abstract

Supernovae are known to be the dominant energy source for driving turbulence in the interstellar medium. Yet, their effect on magnetic field amplification in spiral galaxies is still poorly understood. Analytical models based on the uncorrelated-ensemble approach predicted that any created field will be expelled from the disk before a significant amplification can occur. By means of direct simulations of supernova-driven turbulence, we demonstrate that this is not the case. Accounting for vertical stratification and galactic differential rotation, we find an exponential amplification of the mean field on timescales of 100 Myr. We highlight the importance of rotation in the generation of helicity by showing that a similar mechanism based on Cartesian shear does not lead to a sustained amplification of the mean magnetic field.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 44: JENAM 2008: Grand Challenges in Computational Astrophysics , 2010 , pp. 73 - 76
Copyright
© EAS, EDP Sciences 2011

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References

Références

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