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Using magnetic field maps acquired by the Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory we measured rotation rates of 864 activeand 322 ephemeral regions observed between 2010 and 2016. We found smallermagnetic tracers to show a tendency to rotate faster as compared to largerones. Thus, ephemeral regions exhibit on average the fastest rotation rate. Wefurther divided active regions into three classes. Class A comprised magneticbipoles obeying Hale's polarity law, Joy's law, and exhibiting more coherentleading polarity in comparison with the following one. The second class Bincluded active regions violating at least one of the aforementioned empiricallaws. The third class U comprised unipolar active regions. We found nosignificant difference between the rotation rates of active regions of classesA and B. In contrast, unipolar active regions exhibited on average lowerrotation rate and narrower distribution of the rotation rate differences.Assuming the rotation rate to indicate the anchoring depth of the magneticstructure within the convection zone, we supposed that active regions ofclasses A and B might be anchored throughout the entire convective envelopewhile unipolar active regions a rooted within a thin layer located either nearthe base of the convection zone or at a shallow near-surface depth.

The rotation rate of solar active and ephemeral regions -- I. Dependence on morphology and peak magnetic flux