The symbiotic star V694 Mon has transitioned from the accreting-only state to the steady burning phase

Abstract

We 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, 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 (time-scale of decades). The 3500 Lsun burning luminosity suggests a mass of 0.60 Msun for the WD.

References in corpus (4)

• Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-Novae Supersoft Source
• A Search for Rapid Photometric Variability in Symbiotic Binaries
• Regulation of accretion by its outflow in a symbiotic star: the 2016 outflow fast state of MWC 560
• The 2016 outburst of the unique symbiotic star MWC 560 (= V694 Mon), its long-term BVRI evolution and a marked 331 days periodicity