  In the present paper, we report the photometric and spectroscopic
observations obtained by the 1.88 m telescope at the Kottamia astronomical
observatory of the pulsating star BL Cam. Fourier analysis of the light curves
reveals that the fundamental mode has two harmonics. The O-C method is used to
establish the period changes. So far, the analysis has been very successful in
mapping the pulsation amplitude of the star across the instability strip. By
using the formalism of Eddington and Plakidis (1929), we found significant
results and strong indications of the evolutionary period change. A total of 55
new maximum light timings are reported. New values of (1/P) dP/dt are estimated
using the O-C diagram based on all newly obtained times of maximum light
combined with those taken from the literature, assuming the periods are
decreasing and changing smoothly. To compute the effective temperature and
surface gravity of the star, we performed model atmosphere analysis on its
spectra. The physical parameters of the star are calculated and compared with
the evolutionary models.
