  New multi-color light curves of the very short period K-type eclipsing binary
V1799 Ori were obtained and analyzed with the W-D code. The photometric
solutions reveal that the system is a W-type shallow-contact binary with a mass
ratio of $q=1.335(\pm0.005)$ and a degree of contact about $f = 3.5(\pm1.1)\%$.
In general, the results are in good agreement with which is reported by Samec.
The remarkable O'Connell effects in the light curves are well explained by
employing star spots on the binary surface, which confirms that the system is
active at present. Several new times of light minimum were obtained. All the
available times of light minimum were collected, along with the recalculated
and new obtained. Applying a least-squares method to the constructed O-C
diagram, a new ephemeris was derived for V1799 Ori. The orbital period is found
to show a continuous weak increase at a rate of $1.8(\pm0.6)\times10^{-8}$
days$\cdot$yr$^{-1}$. The extreme-shallow contact, together with the period
increase, suggests that the binary may be at a critical stage predicted by the
TRO theory. \keywords{binaries : close -- binaries : eclipsing -- stars:
individual (V1799 Ori)
