Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...603..785t&link_type=abstract
The Astrophysical Journal, Volume 603, Issue 2, pp. 785-802.
Astronomy and Astrophysics
Astronomy
19
Instabilities, Magnetohydrodynamics: Mhd, Sun: Activity, Sun: Interior, Sun: Magnetic Fields
Scientific paper
The Sun's large-scale magnetic field is believed to be generated deep within the Sun, at the base of the convection zone, in a predominantly stably stratified region of strong radial shear, known as the tachocline. Observations indicate that, owing to magnetic buoyancy, this field rises to the surface to form active regions with systematic properties. Whereas previous investigations of magnetic buoyancy instability have generally assumed a static basic state, here we investigate the role of an aligned shear in modifying this instability. We adopt two complementary approaches. Using the energy principle, we derive sufficient conditions for the stability of a magnetic field in a stratified, compressible shear flow. To investigate the nature of the unstable modes, we have performed a series of numerical calculations; these suggest that the shear has an ``axisymmetrizing'' and stabilizing effect on the magnetic buoyancy instability. We discuss the implications for the instability of the solar magnetic field.
Hughes David W. W.
Tobias Steve M.
No associations
LandOfFree
The Influence of Velocity Shear on Magnetic Buoyancy Instability in the Solar Tachocline does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Influence of Velocity Shear on Magnetic Buoyancy Instability in the Solar Tachocline, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Influence of Velocity Shear on Magnetic Buoyancy Instability in the Solar Tachocline will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1621136