  We present spectroscopic and photometric observations of the Type IIP
supernova, SN 2020jfo, in ultraviolet and optical wavelengths. SN 2020jfo
occurred in the spiral galaxy M61 (NGC 4303), with eight observed supernovae in
the past 100 years. SN 2020jfo exhibited a short plateau lasting < 65 d, and
achieved a maximum brightness in V-band of $M_V$ = -17.4 $\pm$ 0.4 mag at about
8.0 $\pm$ 0.5 d since explosion. From the bolometric light curve, we have
estimated the mass of $^{56}$Ni synthesised in the explosion to be 0.033 $\pm$
0.006 $M_\odot$. The observed spectral features are typical for a type IIP
supernova except for shallow H$\alpha$ absorption throughout the evolution and
the presence of stable $^{58}$Ni feature at 7378 \r{A}, in the nebular phase.
Using hydrodynamical modelling in the MESA + STELLA framework, an ejecta mass
of ~ 5 $M_\odot$ is estimated. Models also indicate SN 2020jfo could be the
result of a Red Super Giant progenitor with $M_{ZAMS}$ ~ 12 $M_\odot$.
Bolometric light curve modelling revealed the presence of a secondary radiation
source for initial ~ 20 d, which has been attributed to interaction with a
circumstellar material of mass ~ 0.2 $M_\odot$, which most likely was ejected
due to enhanced mass loss about 20 years prior to the supernova explosion.
