We present the results of a spectroscopic and photometric analysis of HD314884 , a slowly pulsating B star ( SPB ) in a binary system with detected soft X-ray emission .
We spectrally classify the B star as a B5V–B6V star with T _ { eff } = 15,490 \pm 310 K , log g = 3.75 \pm 0.25 dex , and a photometric period of P _ { 0 } = 0.889521 ( 12 ) days .
A spectroscopic period search 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 third distinct 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 slowly pulsating B star ( SPB ) with at least three oscillation frequencies .
These frequencies appear to originate from higher-order , non-linear tidal pulsations .
Using the dynamical parameters obtained from the radial velocity curve , we find the most probable companion mass to be M _ { 1 } = \sim 0.8 M _ { \sun } assuming a typical mass for the B star and most probable inclination .
We conclude that the X-ray source companion to HD314884 is most likely a coronally active G-type star or a white dwarf ( WD ) , with no apparent emission lines in the optical spectrum .
The mass probability distribution of the companion star mass spans 0.6–2.3 M _ { \sun } at 99 \% confidence which allows the possibility of a neutron star companion .
The X-ray source is unlikely to be a black hole unless it is of a very low mass or low binary inclination .