  13\,Tau is a rarely studied bright B9V type star ({\sl V} = 5.68 mag), which
shows a weak and double-peaked H{$\alpha$} emission profile in its spectra. In
this study, we presented high-precision photometric data of 13\,Tau taken by
the {\sl STEREO} satellite between 2007 and 2011, and compared the results to
the spectroscopic findings to shed light on the Be phenomenon in the star. From
the frequency analysis of the five-year data, we detected that 13\,Tau has
exhibited a mono-periodic light variation ($f$ = 1.80487(1) cd$^{-1}$; A $\sim$
2.76(8) mmag). The analysis revealed that frequency and amplitude values of the
seasonal light curves varied from one year to another. From the spectroscopic
data, we figured out that the equivalent widths of the H{$\alpha$} lines also
showed variability, which seemed connected to the changes seen in both
frequency and amplitude.
