  The presence of companion stars, whether bound or unbound, make correct
identification of the planetary hosting star difficult when a planet has been
detected through a photometrically blended transiting event. We present an
approach that uses a combination of light curve analysis and stellar modeling
to disentangle 8 K2 photometrically blended binary systems that have either a
confirmed or suspected planet to identify the probable host star. The key to
our approach is the use of the mean stellar density, calculated using the
transit geometry, as a discriminator. The approach is strongly dependent on the
difference in magnitude between the stars and the observed transit depth, which
is corrected by the flux ratio between the two stars. While our approach does
not lead to a definitive result for all systems, we were able to determine for
the 8 systems in this case study: two systems where the primary was highly
likely to be the planet hosting star ($>$ 90\% likelihood); three systems where
the primary was likely to be the hosting star ($>$ 55\% likelihood); one system
where the secondary was likely to be the planet hosting star ($>$ 55\%
likelihood); and two systems where we were uncertain which star was the planet
hosting star ($\approx$ 50\% likelihood to be either the primary or the
secondary). Two systems, denoted by their EPIC number, EPIC 201546283 and EPIC
201862715, had confirmed planets, K2-27b and K2-94b respectively, with radii of
$\mathrm{4.0 \pm 0.1}$ and $\mathrm{16.4 \pm 2.9}$ $\mathrm{R_\oplus}$
respectively.
