University of Cambridge > Talks.cam > DAMTP Astrophysics Seminar > Magnetic buoyancy instabilities in the solar tachocline

Magnetic buoyancy instabilities in the solar tachocline

Add to your list(s) Download to your calendar using vCal

If you have a question about this talk, please contact Dr. Yufeng Lin.

Sunspots are surface manifestations of a large-scale magnetic field that rises to the solar photosphere, under the action of magnetic buoyancy, from deep within the solar interior. It is generally accepted that most of the large-scale magnetic flux that appears at the surface originates from the tachocline, which is a region of strong differential rotation around the base of the solar convection zone. Adopting an idealised model that mimics a local region of the tachocline, I will discuss magnetic buoyancy instabilities in a shear-generated magnetic layer. Recent results suggest that such an instability can only operate in rather restricted regions of parameter space, which would have serious implications for the solar tachocline; I will focus particularly upon the extent to which these results actually constrain the magnetic buoyancy instability in this system. Finally, I will describe some preliminary calculations that suggest that shear-driven magnetic buoyancy may be playing a crucial role in the large-scale solar dynamo (for which there is still no universally accepted model

This talk is part of the DAMTP Astrophysics Seminar series.

Tell a friend about this talk:

This talk is included in these lists:

Note that ex-directory lists are not shown.

 

© 2006-2018 Talks.cam, University of Cambridge. Contact Us | Help and Documentation | Privacy and Publicity