  We report the optical, UV, and soft X-ray observations of the $2017-2022$
eruptions of the recurrent nova M31N 2008-12a. We infer a steady decrease in
the accretion rate over the years based on the inter-eruption recurrence
period. We find a ``cusp'' feature in the $r'$ and $i'$ band light curves close
to the peak, which could be associated to jets. Spectral modelling indicates a
mass ejection of 10$^{-7}$ to 10$^{-8}$ M$_{\odot}$ during each eruption, and
an enhanced Helium abundance of He/He$_{\odot}$ $\approx$ 3. The super-soft
source (SSS) phase shows significant variability, which is anti-correlated to
the UV emission, indicating a common origin. The variability could be due to
the reformation of the accretion disk. A comparison of the accretion rate with
different models on the $\rm M_{WD}$$-\dot{M}$ plane yields the mass of a CO
WD, powering the ``H-shell flashes'' every $\sim$ 1 year to be $>1.36$
M$_{\odot}$ and growing with time, making M31N 2008-12a a strong candidate for
the single degenerate scenario of Type Ia supernovae progenitor.
