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We present a detailed study of the 2017 eruption of the classical novaASASSN-17pf (LMCN 2017-11a), which is located in the Large Magellanic Cloud,including data from AAVSO, ASAS-SN, SALT, SMARTS, SOAR, and the Neil Gehrels\textit{Swift} Observatory. The optical light-curve is characterized bymultiple maxima (flares) on top of a slowly evolving light-curve (with adecline time, $t_2>$ 100 d). The maxima correlate with the appearance of newabsorption line systems in the optical spectra characterized by increasingradial velocities. We suggest that this is evidence of multiple episodes ofmass-ejection with increasing expansion velocities. The line profiles in theoptical spectra indicate very low expansion velocities (FWHM $\sim$ 190 kms$^{-1}$), making this nova one of the slowest expanding ever observed,consistent with the slowly evolving light-curve. The evolution of the colorsand spectral energy distribution show evidence of decreasing temperatures andincreasing effective radii for the pseudo-photosphere during each maximum. Theoptical and infrared light-curves are consistent with dust formation 125 dayspost-discovery. We speculate that novae showing several optical maxima havemultiple mass-ejection episodes leading to shocks that may drive $\gamma$-rayemission and dust formation.

Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a)