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We report on simulations of the formation of the first stars in the Universe,where we identify regions of hot atomic gas (fH2 < 10-6) at densities above10-14 g/cc, heated to temperatures ranging between 3000 and 8000 K. Within thistemperature range atomic hydrogen is unable to cool effectively. We describethe kinetic and thermal characteristics of these regions and investigate theirorigin. We find that these regions, while small in total mass fraction of thecloud, may be dynamically important over the accretion timescale for thecentral clump in the cloud, particularly as a chemical, rather than radiative,mechanism for clearing the polar regions of the accretion disk of material andterminating accretion along these directions. These inherentlythree-dimensional effects stress the need for multi-dimensional calculations ofprotostellar accretion for reliable predictions of the masses of the very firststars.

High-Entropy Polar Regions Around the First Protostars