discovered in the nebula of a Wolf-Rayet (WR) star for the first time.  At
the measured H2 luminosity of roughly 4 times L(solar), one implication is
that WR stars could contribute a substantial fraction of the total H2 emission
in young starburst galaxies.  The excitation mechanism could be either shocks
from the strong stellar wind, or UV flourescence from the intense stellar
radiation field.  We propose to obtain spectra of the mid-IR H2 transitions
using the SWS grating with the aim of establishing the dominant excitation
mechanism, and combined with nebular lines diagnose the temperature and
density structure and H2 formation rate along the PDR.  With LWS01, we can
also cover the important fine structure CII, OI, and NII lines to establish
the balance of heating and cooling.  SWS06 will further allow us to explore,
for the first time, the crystalline silicate content of the dust in a WR
nebula, and cover the water, CO2, and CO ice or gas phase features that would
occur in the molecular material that partially hides the optical nebula.
This would be the first (and probably only) observations of their kind on a
Pop. I WR nebula with ISO.