The Symbiotic Star V694 Mon has Transitioned from the Accreting-only State to the Steady Burning Phase

Abstract I propose that the drastic photometric and spectroscopic changes affecting the symbiotic star V694 Mon since 2018, are due to its transition from the accreting-only state to steady hydrogen-burning on the surface of the white dwarf (WD), closely mimicking the pattern followed by V4368 Sgr. The phase of peak optical brightness and weakest emission lines has probably been reached in early 2024. The high-velocity absorptions powered by jet-ejection and the wild flickering, which dominated the century-long quiescence, should not reappear as long has nuclear burning will hold (timescale of decades). The 3500 L ⊙ burning luminosity suggests a 0.60 M ⊙ mass for the WD.