  We performed spectroscopic and photometric analyses on the early B-type LP
Ori young stellar object located in the Orion Nebula. The high-resolution
spectra of LP Ori was obtained at the Ankara University Kreiken Observatory in
2023, while all spectra recorded over the past 19 years were extracted from the
ESO and ESPaDOnS archives. In these spectra of LP Ori, there is typically an
emission observed in the core of the Balmer profile. This structure is
accompanied by a $\sim$14-year interval inverse P-Cygni repetition superimposed
on the Balmer profile. Additionally, an emission in the $\lambda$5875 He~I line
is visible in the spectra in the year 2023. When this emission is considered
together with the inverse P-Cygni structures, these observations suggest that
LP Ori is a Herbig Ae/Be star. The abundance pattern of LP Ori is close to
solar with the exception of a slightly rich helium and slightly poor Al
abundance. Additionally, the spectral energy distribution of LP Ori was
constructed to confirm the infrared excess caused by its circumstellar disk.
Furthermore, the photometric analysis performed on the TESS observations of LP
Ori shows significant photometric variability and the frequency analysis
reveals a $\beta$~Cephei star in its forthcoming evolution.
