Proxima Cen flare activity temporal changes

During strong flares the "red asymmetry" appears in the H{alpha} emission line indicating the infall of hot condensed matter into the chromosphere with velocities greater than 100km/s disturbing chromospheric layers. As a result, the strength of the CaII lines anti-correlates with H{alpha} during strong flares. The HeI lines at 4026 and 5876{AA} appear in the strong flares.

The cores of D1 and D2 NaI lines are also seen in emission. During the minimum activity of Proxima Centauri, CaII lines and H{alpha} almost disappear while the blue part of the NaI emission lines is affected by the absorption in the extending and condensing flows. We see different behaviour of emission lines formed in the flare regions and chromosphere.

Chromosphere layers of Proxima Cen are likely heated by the flare events; these layers are cooled in the "non-flare" mode. The self-absorption structures in cores of our emission lines vary with time due to the presence of a complicated system of inward and outward matter flows in the absorbing layers.