📝 SummarXiv

Abstract

Radial differential rotation is an important factor in stellar dynamo theory. In the Sun, helioseismology has revealed a near surface shear layer in the upper 5 to 10% of the convection zone. At low to midlatitudes, the rotation velocity gradient decreases sharply near the surface. A depth gradient in rotational velocity was recently detected in the low photosphere using a differential interferometric method on spectroscopic data. Granular structures at different depths in the FeI 630.15 nm line showed a systematic retrograde shift compared to continuum structures, suggesting a height-related decrease in angular velocity, dependent on the assumed granulation coherence time. We use a more direct approach to measure the differential rotational velocity at different photospheric heights. We performed spectroscopic scans of the same granular region in FeI 630.15 nm and CaI 616.2 nm lines and measured displacements of images at different line chords between consecutive scans. These observations require excellent seeing, stable adaptive optics, and scanning times shorter than the granulation lifetime. Adaptive optics stabilizes continuum images but not higher-altitude rotation differences. We used THEMIS and HINODE SOT FeI data to measure formation height differences via perspective shifts observed away from the disk center with the slit radially oriented. Measurements at disk center and $\pm$25{\deg} latitude along the central meridian show a parabolic decrease in rotational velocity with height, reaching about 16% slower rotation at 80 km above the continuum. No significant difference is found between the equator and $\pm$25{\deg} latitudes. The low photosphere is a transition zone between the convective and radiative layers. Our measurements provide new constraints on its dynamical behavior and valuable boundary conditions for numerical simulations of the Sun s upper convection zone.