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We present the results of a spectroscopic and photometric analysis ofHD314884, a slowly pulsating B star (SPB) in a binary system with detected softX-ray emission. We spectrally classify the B star as a B5V-B6V star withT$_{eff}$ = 15,490 $\pm$ 310 K, log $g$ = 3.75 $\pm$ 0.25 dex, and aphotometric period of P$_{0}$ = 0.889521(12) days. A spectroscopic periodsearch reveals an orbital period for the system of P$_{orb}$ = 1.3654(11) days.The discrepancy in the two periods and the identification of a second and thirddistinct frequency in the photometric fourier transform at P$_1$ = 3.1347(56)and P$_2$ = 1.517(28) days provides evidence that HD314884 is a slowlypulsating B star (SPB) with at least three oscillation frequencies. Thesefrequencies appear to originate from higher-order, non-linear tidal pulsations.Using the dynamical parameters obtained from the radial velocity curve, we findthe most probable companion mass to be M$_1$ = $\sim$0.8 M$_{\odot}$ assuming atypical mass for the B star and most probable inclination. We conclude that theX-ray source companion to HD314884 is most likely a coronally active G-typestar or a white dwarf (WD), with no apparent emission lines in the opticalspectrum. The mass probability distribution of the companion star mass spans0.6-2.3 M$_{\odot}$ at 99$\%$ confidence which allows the possibility of aneutron star companion. The X-ray source is unlikely to be a black hole unlessit is of a very low mass or low binary inclination.

HD314884: A Slowly Pulsating B star in a Close Binary