  We analyzed global properties, radial profiles and 2D maps of the metal
abundances and temperature in the cool core cluster of galaxies Hydra A using a
deep XMM-Newton exposure. The best fit among the available spectral models is
provided by a Gaussian distribution of the emission measure (gdem). We can
accurately determine abundances for 7 elements in the cluster core with EPIC
and 3 elements with RGS. The gdem model gives lower Fe abundances than a single
temperature model. The abundance profiles for Fe, Si, S, but also O are
centrally peaked. Combining the Hydra A results with 5 other clusters for which
detailed chemical abundance studies are available, we find a significant
decrease of O with radius, while the increase in the O/Fe ratio with radius is
small within 0.1 r_200. We compare the observed abundance ratios with the
mixing of various supernova type Ia and core-collapse yield models in different
relative amounts. Producing the estimated O, Si and S peaks in Hydra A requires
either an amount of metals ejected by stellar winds 3-8 times higher than
predicted by available models or a remaining peak in the enrichment by
core-collapse supernovae from the protocluster phase. The temperature map shows
cooler gas extending in arm-like structures towards the north and south. These
structures appear to be richer in metals than the ambient medium and spatially
correlated with the large-scale radio lobes. We estimate the mass of cool gas,
which was probably uplifted by buoyant bubbles of relativistic plasma produced
by the AGN, to 1.6-6.1x10^9 M_sun, and the energy associated with this uplift
to 3.3-12.5x10^58 ergs. The best estimate of the mass of Fe uplifted together
with the cool gas is 1.7x10^7 M_sun, 15% of the total mass of Fe in the central
0.5arcmin region.
