  Our aim was to study the light curve periodicity of the solar analogue V352
CMa and in particular show that the presence or absence of periodicity in low
amplitude light curves can be modelled with the Continuous Period Search (CPS)
method. We applied the CPS method to 14 years of V-band photometry of V352 CMa
and obtained estimates for the mean, amplitude, period and minima of the light
curves in the selected datasets. We also applied the Power Spectrum Method
(PSM) to these datasets and compared the performance of this frequently applied
method to that of CPS. We detected signs of a $11.7 \pm 0.5$ year cycle in in
the mean brightness. The long-term average photometric rotation period was
$7.24 \pm 0.22$ days. The lower limit for the differential rotation coefficient
would be $|k| > 0.12$, if the law of solar surface differential rotation were
valid for V352 CMa and the period changes traced this phenomenon. Signs of
stable active longitudes rotating with a period of $7.157 \pm 0.002$ days were
detected from the epochs of the light minima with the Kuiper method. CPS
performed better than the traditional PSM, because the latter always used a
sinusoidal model for the data even when this was clearly not the correct model.
