  We have used optical echelle spectra along with ROSAT and ASCA X-ray spectra
to test the hypothesis that the southern portion of the N44 X-ray bright region
is the result of a blowout structure. Three pieces of evidence now support this
conclusion. First, the filamentary optical morphology corresponding with the
location of the X-ray bright South Bar suggests the blowout description (Chu et
al 1993). Second, optical echelle spectra show evidence of high velocity (~90
km/sec) gas in the region of the blowout. Third, X-ray spectral fits show a
lower temperature for the South Bar than the main superbubble region of Shell
1. Such a blowout can affect the evolution of the superbubble and explain some
of the discrepancy discussed by Oey & Massey (1995) between the observed shell
diameter and the diameter predicted on the basis of the stellar content and
Weaver et al.'s (1977) pressure-driven bubble model.
