  New photometry, including TESS data, have been combined with recent
spectroscopic observations of the Orion Ib pulsating triple-star system VV Ori.
This yields a revised set of absolute parameters with increased precision. Two
different programs were utilized for the light curve analysis, with results in
predictably close agreement. The agreement promotes confidence in the analysis
procedures. The spectra were analysed using the {\sc FDBinary} program. The
main parameters are as follows: $M_1 = 11.6 \pm 0.14$ and $M_2 = 4.8 \pm 0.06$
(M$_\odot$). We estimate an approximate mass of the wide companion as $M_3 =
2.0 \pm 0.3$ M$_\odot$. Similarly, $R_{1} = 5.11 \pm 0.03$, $R_2 = 2.51 \pm
0.02$, $R_3 = 1.8 \pm 0.1$ (R$_\odot$); $T_{\rm e 1} = 26600 \pm 300$, $T_{\rm
e 2} = 16300 \pm 400$ and $T_{\rm e 3} = 10000 \pm 1000$ (K). The close
binary's orbital separation is $a= 13.91$ (R$_\odot$); its age is $8 \pm 2$
(Myr) and its photometric distance is $396 \pm 7$ pc. The primary's $\beta$ Cep
type oscillations support these properties and confirm our understanding of its
evolutionary status. Examination of the well-defined $\lambda$6678 He I
profiles reveals the primary to have a significantly low projected rotation:
some 80\% of the synchronous value. This can be explained on the basis of the
precession of an unaligned spin axis. This proposal can resolve also observed
variations of the apparent inclination and address other longer-term
irregularities of the system reported in the literature. This topic invites
further observations and follow-up theoretical study of the dynamics of this
intriguing young multiple star.
