  We report results from an X-ray study of the Abell 2111 galaxy cluster using
the Advanced Satellite for Astrophysics and Cosmology ASCA and the ROSAT
Position Sensitive Proportional Counter (PSPC). By correcting for the
energy-dependent point-spread function of the ASCA instruments, we have
examined the temperature structure of the cluster. The cluster's core within 3'
is found to have a temperature of 6.46+-0.87 keV, significantly higher than
3.10+-1.19 keV in the surrounding region of r = 3 - 6'. This radially
decreasing temperature structure can be parameterized by a polytropic index of
$\gamma$ $\simeq$ 1.45. The X-ray morphology of the cluster appears elongated
and clumpy on scales $\le$1'. These results, together with earlier {\it ROSAT}
and optical studies which revealed that the X-ray centroid and ellipticity of
A2111 shift with spatial scale, are consistent with the hypothesis that the
cluster is a dynamically young system. Most likely, the cluster has recently
undergone a merger, which may also be responsible for the high fraction of blue
galaxies observed in the cluster. Alternatively, the temperature structure may
also be due to the gravitational potential of the cluster. We have further
measured the emission weighted abundance of the X-ray-emitting intracluster
medium as 0.25$\pm$0.14 solar. This value is similar to those of nearby
clusters which do not show a large blue galaxy fraction, indicating that star
formation in disk galaxies and subsequent loss to the medium do not drastically
alter the average abundance of a cluster. This is consistent with recent
results which indicate that cluster abundances have remained constant since at
least z ~ 0.3.
