Fig. 1
Cartoon showing the equatorial regions (from 1.6 to 3.0 R⊙) over which the O vi 1032 Å intensity time-series have been analyzed in the solar corona (light gray areas) and the corresponding upper convection zone regions (from 0.90 to 0.99 R⊙) for which the rotation rates have been inferred from helioseismic data (dark gray areas).
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