  We analyze a high resolution spectropolarimetric dataset collected for the
He-weak B3p IV star HR 2949. The Zeeman effect is visible in the circularly
polarized component of numerous spectral lines. The longitudinal magnetic field
varies between approximately $-650$ and $+150$ G. The polar strength of the
surface magnetic dipole is calculated to be 2.4$^{+0.3}_{-0.2}$ kG. The star
has strong overabundances of Fe-peak elements, along with extremely strong
overabundances of rare-earth elements; however, He, Al, and S are
underabundant. This implies that HR 2949 is a chemically peculiar star.
Variability is seen in all photospheric lines, likely due to abundance patches
as seen in many Ap/Bp stars. Longitudinal magnetic field variations measured
from different spectral lines yield different results, likely a consequence of
uneven sampling of the photospheric magnetic field by the abundance patches.
Analysis of photometric and spectroscopic data for both HR 2949 and its
companion star, HR 2948, suggests a revision of HR 2949's fundamental
parameters: in particular, it is somewhat larger, hotter, and more luminous
than previously believed. There is no evidence of optical or ultraviolet
emission originating in HR 2949's magnetosphere, despite its moderately strong
magnetic field and relatively rapid rotation; however, when calculated using
theoretical and empirical boundaries on the initial rotational velocity, the
spindown age is compatible with the stellar age. With the extensive phase
coverage presented here, HR 2949 will make an excellent subject for Zeeman
Doppler Imaging.
