  We discuss the results of high-resolution (~0.1-0.2 pc) BIMA CO observations
of the central regions of 3 molecular clouds in the far-outer Galaxy (FOG). We
identify clumps and investigate their stability by using the virial theorem,
including terms due to gravity, turbulence, magnetic field, and interclump gas
pressure, and make a comparison with clumps in local clouds (RMC and Orion B
South). While a reasonable combination of these forces can render most clumps
stable, an interesting difference between FOG and local clumps emerges when
comparing only gravity and turbulence. In the FOG these forces are in
equilibrium (virial parameter alpha ~ 1) for clumps down to the lowest masses
found (a few Msol), but for local clumps alpha ~ 1 only for clumps with masses
larger than a few tens of Msol. Thus it appears that in the FOG gravity is the
dominant force down to a much lower mass than in local clouds, implying that
gravitational collapse and star formation may occur more readily even in the
smallest clumps. This might explain the apparently steeper IMF found in the
outer Galaxy.
