The rotational and flare activity of the chemically peculiar star B9.5IIIpHgMnSi βScl is studied using data from the archive of the TESS space mission. Rotational modulation of the brightness is clearly visible in the light curve of this star, along with two flares that have a structure typical of flares in stars of a later spectral class, with a sharp rise, a peak, and a damping stage. The constructed power spectrum has a peak corresponding to a rotation period of 1.91±0.09 days. The standard technique for analysis of the flare activity of stars based on observations from the Kepler space telescope and the TESS mission yields the energy of the radiation in the two flares. The energy emitted in the first flare was 3·1036 erg and in the second, 4.5·1035 erg. The values we have found agree with published estimates for the first flare. Arguments in favor of and against the flares taking place on βScl, rather than on a possible companion at an angular separation of 0.641 arcsec, are discussed.
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Translated from Astrofizika, Vol. 62, No. 4, pp. 571-577 (November 2019)
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Savanov, I.S. Activity of the Star bScl Observed by the TESS Space Telescope. Astrophysics 62, 513–517 (2019). https://doi.org/10.1007/s10511-019-09600-8
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DOI: https://doi.org/10.1007/s10511-019-09600-8