Activity of the Star AB Pic with an Exoplanet from the Young Tuc–Hor Association

Based on highly accurate data from the archive of the TESS space mission, we have studied the photometric variability of the K1-type dwarf AB Pic (HD 44627), which is a member of the Tuc–Hor association and possesses a distant giant planet with a mass of 13.5 Jupiter masses. In the interval of its TESS observations 48 flares with an energy in the range $$6.1\times 10^{32}{-}3.4\times 10^{35}$$ erg were detected on the star. We have estimated the stellar rotation period, $$P=3.860\pm 0.020$$ days, and the photometric variability amplitude as well as estimated the spottedness parameter $$A$$ by a standard technique. The spot area on the surface of AB Pic is considerably larger than that on the Sun and varies within the range from 54 000 to 95 000 m.s.h. We suggest that during the interval of its observations the spot area on the stellar surface had cyclic variations with a duration of 233 days, an analog of which may be the so-called Rieger periodicity on the Sun. We have estimated the longer activity cycles of AB Pic based on data from the All Sky Automated Survey archive and revealed possible activity cycles of 258, 1120 days (3.1 years), and 2640 days (7.2 years). The range of possible variations in the CME mass for this star has been estimated.