  KIC~8262223 is an eclipsing binary with a short orbital period ($P=1.61$ d).
The {\it Kepler} light curves are of Algol-type and display deep and partial
eclipses, ellipsoidal variations, and pulsations of Delta Scuti type. We
analyzed the {\it Kepler} photometric data, complemented by phase-resolved
spectra from the R-C Spectrograph on the 4-meter Mayall telescope at Kitt Peak
National Observatory and determined the fundamental parameters of this system.
The low mass and oversized secondary ($M_2=0.20M_{\odot}$, $R_2=1.31R_{\odot}$)
is the remnant of the donor star that transferred most of its mass to the
gainer, and now the primary star. The current primary star is thus not a normal
$\delta$ Scuti star but the result of mass accretion from a lower mass
progenitor. We discuss the possible evolutionary history and demonstrate with
the MESA evolution code that the system can be understood as the result of
non-conservative binary evolution similar to that for the formation of EL CVn
type binaries. The pulsations of the primary star can be explained as radial
and non-radial pressure modes. The equilibrium models from single star
evolutionary tracks can match the observed mass and radius
($M_1=1.94M_{\odot}$, $R_1=1.67R_{\odot}$) but the predicted unstable modes
associated with these models differ somewhat from those observed. This work
presents a preliminary asteroseismic analysis of the abnormal Delta Scuti
pulsators, and we discuss the need for better theoretical understanding of such
pulsating mass gaining stars.
