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The boundary in the solar interior between the outer convection zone and the inner radiative zone. This boundary arises from the fact that the convection zone rotates faster near the solar equator than it does near the solar poles, while the interior of the sun rotates equally at all latitudes.

[Greek takhos, speed + -cline.]
American Heritage® Dictionary of the English Language, Fifth Edition. Copyright © 2016 by Houghton Mifflin Harcourt Publishing Company. Published by Houghton Mifflin Harcourt Publishing Company. All rights reserved.
References in periodicals archive ?
Power Spectrum Analysis of LMSU (Lomonosov Moscow State University) Nuclear Decay-Rate Data: Further Indication of R-Mode Oscillations in an Inner Solar Tachocline. Astroparticle Physics, 2012, v.
Within the context of the gaseous models, solar magnetic fields are believed to be produced by the action of a powerful solar dynamo [319,320] generated at the base of the convection zone near the tachocline layer, well beneath the solar photosphere [12].
([section]) While a gas can easily be thought to undergo differential rotation, the Sun is characterized by another region: a tachocline layer separates the convection zone from the solid solar core (see [section]6.5).
The tachocline region acts as a shear layer within the Sun.
When considering the tachocline layer, it is important to recall that shear stresses require the presence of a physical plane.