  We carried out light curve solutions of the ultrashort-period binaries with
MS components observed by $Kepler$. All six targets turned out almost in
thermal contact with contact or slightly overcontact configurations. Two of
them, KID 4921906 and KID 6309193, are not eclipsing but reveal ellipsoidal and
spot variability. One of the components of KID 8108785 exhibits inherent,
quasi-sinusoidal, small-amplitude variability. KID 12055255 turned out a very
rare case of ultrashort-period overcontact binary consisting of two M dwarfs.
Our modeling indicated that the variability of KID 9532219 is due to eclipses
but not to $\delta$ Sct pulsations as it was previously supposed.
