scholarly journals The radial gradient of the near-surface shear layer of the Sun

2014 ◽  
Vol 570 ◽  
pp. L12 ◽  
Author(s):  
A. Barekat ◽  
J. Schou ◽  
L. Gizon
2022 ◽  
Vol 924 (1) ◽  
pp. 19
Author(s):  
H. M. Antia ◽  
Sarbani Basu

Abstract We use helioseismic data obtained over two solar cycles to determine whether there are changes in the near-surface shear layer (NSSL). We examine this by determining the radial gradient of the solar rotation rate. The radial gradient itself shows a solar-cycle dependence, and the changes are more pronounced in the active latitudes than at adjoining higher latitudes; results at the highest latitudes (≳70°) are unreliable. The pattern changes with depth, even within the NSSL. We find that the near-surface shear layer is deeper at lower latitudes than at high latitudes and that the extent of the layer also shows a small solar-cycle-related change.


2011 ◽  
Vol 743 (1) ◽  
pp. 79 ◽  
Author(s):  
Mark S. Miesch ◽  
Bradley W. Hindman

Author(s):  
Benjamin K. Smeltzer ◽  
Yan Li ◽  
Simen Å. Ellingsen

For waves generated by a wave source which is simultaneously moving and oscillating at a constant frequency ω, a resonance is well known to occur at a particular value τres of the nondimensional frequency τ = ωV/g (V: source velocity relative to the surface, g: gravitational acceleration). For quiescent, deep water, it is well known that τres = 1/4. We study the effect on τres from the presence of a shear flow in a layer near the surface, such as may be generated by wind or tidal currents. Assuming the vorticity is constant within the shear layer, we find that the effects on the resonant frequency can be significant even for sources corresponding to moderate shear and relatively long waves, while for stronger shear and shorter waves the effect is stronger. Even for a situation where the resonant waves have wavelengths about 20 times the width of the shear layer, the resonance frequency can change by ∼ 25% for even a moderately strong shear VS/g = 0.3 (S: vorticity in surface shear layer). Intuition for the problem is built by first considering two simpler geometries: uniform current with finite depth, and Couette flow of finite depth.


2011 ◽  
Vol 271 ◽  
pp. 012070 ◽  
Author(s):  
Kyle Augustson ◽  
Mark Rast ◽  
Regner Trampedach ◽  
Juri Toomre

2005 ◽  
Vol 13 ◽  
pp. 431-434
Author(s):  
Deborah A. Haber ◽  
Bradley W. Hindman

AbstractWe report new measurements of the sun’s global meridional circulation within the near-surface shear layer for the years 1996 to 2003. The flows are obtained using the local helioseismic technique of ring analysis applied to MDI Dynamics Program data. The most recent estimates of the solar p-angle correction to this data have been incorporated. Previously published accounts that the solar meridional circulation possesses multiple cells within the northern hemisphere (Haber et al. 2002) are not contradicted by the new findings. We do find, however, that with the inclusion of the p-angle correction, cross-equator flows have been eliminated.


2015 ◽  
Vol 803 (2) ◽  
pp. L17 ◽  
Author(s):  
Benjamin J. Greer ◽  
Bradley W. Hindman ◽  
Nicholas A. Featherstone ◽  
Juri Toomre

2006 ◽  
Vol 2 (S239) ◽  
pp. 457-466 ◽  
Author(s):  
Axel Brandenburg

AbstractThe outer surface layers of the sun show a clear deceleration at low latitudes. This is generally thought to be the result of a strong dominance of vertical turbulent motions associated with strong downdrafts. This strong negative radial shear should not only contribute to amplifying the toroidal field locally and to expelling magnetic helicity, but it may also be responsible for producing a strong prograde pattern speed in the supergranulation layer. Using simulations of rotating stratified convection in cartesian boxes located at low latitudes around the equator it is shown that in the surface layers patterns move in the prograde direction on top of a retrograde mean background flow. These patterns may also be associated with magnetic tracers and even sunspot proper motions that are known to be prograde relative to the much slower surface plasma.


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