  We present the results of quantitative spectral analyses of ten apparently
normal B-type stars. These stars were found to be young massive B-type stars at
distances of z=2.6 to 7.6 kpc from the galactic plane based on their positions
in the (Teff, log g) diagram, normal abundance patterns and/or large projected
rotational velocities. We discuss formation scenarios (runaway star scenarios
versus a scenario for star formation in the halo) by comparing times-of-flight
and evolutionary time scales. For all stars (except SB 357 and HS 1914+7139)
both the scales are similar, indicating that the stars could have formed in the
galactic disk and been ejected from there soon aftertheir birth. Derived
ejection velocities range from 130 km/s to 440 km/s and may be used to
constrain models for ejection mechanisms. Using new proper motion measurements
we show that PHL 346, which was considered the most likely candidate for a
young B-type star born in the halo, can be explained as a runaway star from the
galactic plane.
