  Based on published sources, we have created a kinematic database on 220
massive (>10 solar masses) young Galactic star systems located within <3 kpc of
the Sun. Out of them, approximately 100 objects are spectroscopic binary and
multiple star systems whose components are massive OB stars; the remaining
objects are massive Hipparcos B stars with parallax errors of no more than 10
percent. Based on the entire sample, we have constructed the Galactic rotation
curve, determined the circular rotation velocity of the solar neighborhood
around the Galactic center at Ro=8 kpc, Vo=259+-16 km/s, and obtained the
following spiral density wave parameters: the amplitudes of the radial and
azimuthal velocity perturbations f_R=-10.8+/-1.2 km/s, and f_\theta=7.9+/-1.3
km/s, respectively; the pitch angle for a two-armed spiral pattern i=-6.0+/-0.4
deg., with the wavelength of the spiral density wave near the Sun being
2.6+/-0.2 kpc; and the radial phase of the Sun in the spiral density wave
-120+/-4 deg. We show that such peculiarities of the Gould Belt as the local
expansion of the system, the velocity ellipsoid vertex deviation, and the
significant additional rotation can be explained in terms of the density wave
theory. All these effects decrease noticeably once the influence of the spiral
density wave on the velocities of nearby stars has been taken into account. The
influence of Gould Belt stars on the Galactic parameter estimates has also been
revealed. Eliminating them from the kinematic equations has led to the
following new values of the spiral density wave parameters: f_\theta=2.9+/-2.1
km/s and \chi_\odot=-104+/-6 deg.
