  The symbiotic recurrent nova T CrB erupted for the second and last recorded
time in 1946. Following the outburst, the accretion rate onto its WD has
remained rather low with only occasional and minor flaring episodes, until in
late 2014 it entered a "super-active" phase (SAP) that peaked in April 2016:
the flux radiated by Balmer lines increased by two orders of magnitude,
accompanied by the appearance of strong HeI, HeII, and many other emission
lines. Following the sharp maximum, the intensity of the emission lines has
been steadily decreasing, reaching back the pre-SAP levels by mid-2023. The end
of SAP is also confirmed by the drop of $B$-band brightness to pre-SAP
conditions and the simultaneous re-appearance of a large-amplitude flickering.
This suggest that the accretion disk has emptied from the extra material that
has driven the "super active" state and has completed its transfer onto the WD,
setting the stage for a new and probably imminent nova eruption.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena