  We present the analysis of optical photometric and spectroscopic observations
of two non-magnetic cataclysmic variables, namely CRTS J080846.2+313106 and
V416 Dra. CRTS J080846.2+313106 has been found to vary with a period of
4.9116$\pm$0.0003 h, which was not found in earlier studies and is
provisionally suggested as the orbital period of the system. In both
long-period systems, the observed dominant signal at second harmonic of the
orbital frequency and the orbital modulation during quiescence are suggestive
of ellipsoidal variation from changing aspects of the secondary, with an
additional contribution from the accretion stream or hotspot. However, during
the outburst, the hotspot itself is overwhelmed by the increased brightness,
which is possibly associated with the accretion disc. The mid-eclipse phase for
V416 Dra occurs earlier and the width of the eclipse is greater during
outbursts compared to quiescence, suggesting an increased accretion disc radius
during outbursts. Furthermore, the investigation of accretion disc eclipse in
V416 Dra implies that a total disc eclipse is possible during quiescence,
whereas the disc seems to be partially obscured during outbursts, which further
signifies that the disc may grow in size as the outburst progresses. Optical
spectra of CRTS J080846.2+313106 and V416 Dra are typical of dwarf novae during
quiescence, and they both show a significant contribution from the M2-4V
secondary. The light curve patterns, orbital periods, and spectra observed in
both systems look remarkably similar, and seem to resemble the characteristics
of U Gem-type dwarf novae.
