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We analyze the light curve of the M5.5 dwarf Proxima Centauri obtained by theTESS in Sectors 11 and 12. In the $\approx 50$ day-long light curve weidentified and analyzed 72 flare events. The flare rate was 1.49 events perday, in total, 7.2% of the data was classified as flaring. The estimated flareenergies were in the order of $10^{30}-10^{32}$ ergs in the TESS passband($\approx4.8\times$ higher in bolometric energies, but in the same order ofmagnitude). Most of the eruptions appeared in groups. Two events showedquasi-periodic oscillations during their decay phase with a time scale of a fewhours, that could be caused by quasiperiodic motions of the emitting plasma oroscillatory reconnection. From the cumulative flare frequency distribution weestimate that superflares with energy output of $10^{33}$ ergs are expected tooccur three times per year, while a magnitude larger events (with $10^{34}$ergs) can occur every second year. This reduces the chances of habitability ofProxima Cen b, although earlier numerical models did not rule out the existenceof liquid water on the planetary surface. We did not find any obvious signs ofplanetary transit in the light curve.

astrophysical journal/the astrophysical journal

Flaring activity of Proxima Centauri from TESS observations:  quasi-periodic oscillations during flare decay and inferences on the  habitability of Proxima b