Abstract
Material circulation in the solar tachocline mixes the tachocline material with the convection zone, which causes the sound speed in and immediately beneath the tachocline to exceed what one would expect from current standard solar models. Calibration against a helioseismic determination of the sound speed from SOI/MDI data of a sequence of solar models having mixed layers of different thicknesses yields a value of 0.019 R☉ for the mean tachocline thickness Δ, with a formal standard error of about 5%. This value for Δ is somewhat smaller than previous estimates based on measuring shear in the seismically inferred angular velocity, and it has important implications concerning our understanding of the magnetohydrodynamics of the tachocline.
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