What is it about?
The paper illustrates that even a very symmetric flow of plasma with zero helicity - called the no-cosines flow - can drive a fast dynamo, i.e. that even a simple flow can amplify an initially weak magnetic field.
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Why is it important?
It turns out that in addition to a high growth rate, the dynamo saturates at a level significantly higher than normal turbulent dynamos, namely at exact equipartition, i.e. with a relatively high energy level. Visualization of the magnetic and velocity fields at saturation will help us to understand some of the aspects of the non-linear dynamo problem.
Perspectives
Visualization of magnetic and velocity fields at saturation may help us understand some aspects of non-linear dynamos. This very special dynamo with a highly symmetric flow of plasma with zero helicity drives a fast dynamo and saturates at a level higher than turbulent dynamos, namely at exact equipartition, i.e. with a high energy level.
Dr Bertil F Dorch
Syddansk Universitet
Read the Original
This page is a summary of: On the Saturation of Astrophysical Dynamos: Numerical Experiments with the No-Cosines Flow, Solar Physics, October 2004, Springer Science + Business Media,
DOI: 10.1007/s11207-005-5700-4.
You can read the full text:
Resources
Scholarpedia
Encyclopedia article on the Archontis Dynamo at the Wiki-based publication Scholarpedia.
The role of the Yoshizawa effect in the Archontis dynamo
Paper on the Archontis Dynamo in Monthly Notices of the Royal Astronomical Society (Sur & Brandenburg 2009).
A strong field dynamo in the solar tachocline
Presentation on dynamos by David Galloway, School of Mathematics and Statistics University of Sydney, Australia.
Magnetic activity in late-type giant stars
Numerical MHD simulations of non-linear dynamo action in Betelgeuse
Figure 2 from the paper
Figure 2 incl. description at Figshare
Figure 1 from the paper
Figure 1 incl. description at Figshare.
Figure 5 from the paper
Figure 5 incl. description at Figshare.
Open Access at Springer
Full paper free download
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