Differential Rotation of Individual Sunspots and Pores

Abstract The differential rotation of individual sunspots and pores is analyzed according to Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI) observations processing in the period 01.05.2010 – 31.05.2024. To accurately track sunspots, we processed 5 images for each day. To determine the polarity of the magnetic field, we superimposed the contours of sunspots on observations of magnetic fields at the same time. This made it possible to track the movement of more than 175 thousand individual sunspots and pores. It is found that the rotation rate of individual sunspots and pores differs significantly from the differential rotation of sunspot groups. In particular, solar pores with no penumbra and a characteristic area of S ≈ 10 μhm rotate ≈ 1.7% slower than regular sunspots with penumbra. Perhaps this is due to a change in the rotation rate with depth in the convective zone, namely in the leptocline (0.95R⊙). Sunspots and pores of the leading polarity have rotation rate of ≈ 2.3% faster than trailing polarity spots. This difference is probably due to the movement of the spots when the arches of the magnetic field rise.