  We have observed 15 red giant stars in the relatively massive, metal-poor
globular cluster NGC 4833 using the Magellan Inamori Kyocera Echelle
spectrograph at Magellan. We calculate stellar parameters for each star and
perform a standard abundance analysis to derive abundances of 43 species of 39
elements, including 20 elements heavier than the iron group. We derive <[Fe/H]>
= -2.25 +/- 0.02 from Fe I lines and <[Fe/H> = -2.19 +/- 0.013 from Fe II
lines. We confirm earlier results that found no internal metallicity spread in
NGC 4833, and there are no significant star-to-star abundance dispersions among
any elements in the iron group (19 <= Z <= 30). We recover the usual abundance
variations among the light elements C, N, O, Na, Mg, Al, and possibly Si. The
heavy-element distribution reflects enrichment by r-process nucleosynthesis
([Eu/Fe] = +0.36 +/- 0.03), as found in many other metal-poor globular
clusters. We investigate small star-to-star variations found among the
neutron-capture elements, and we conclude that these are probably not real
variations. Upper limits on the Th abundance, log epsilon (Th/Eu) < -0.47 +/-
0.09, indicate that NGC 4833, like other globular clusters where Th has been
studied, did not experience a so-called "actinide boost."
