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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 inthe accretion rate over the years based on the inter-eruption recurrenceperiod. We find a ``cusp'' feature in the $r'$ and $i'$ band light curves closeto the peak, which could be associated to jets. Spectral modelling indicates amass ejection of 10$^{-7}$ to 10$^{-8}$ M$_{\odot}$ during each eruption, andan enhanced Helium abundance of He/He$_{\odot}$ $\approx$ 3. The super-softsource (SSS) phase shows significant variability, which is anti-correlated tothe UV emission, indicating a common origin. The variability could be due tothe reformation of the accretion disk. A comparison of the accretion rate withdifferent models on the $\rm M_{WD}$$-\dot{M}$ plane yields the mass of a COWD, 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 forthe single degenerate scenario of Type Ia supernovae progenitor.

Multi-wavelength observations of multiple eruptions of the recurrent nova M31N 2008-12a