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The Chandra Carina Complex Project (CCCP) has shown that the Carina Nebuladisplays bright, spatially-complex soft diffuse X-ray emission. Here we `sumup' the CCCP diffuse emission work by comparing the global morphology andspectrum of Carina's diffuse X-ray emission to other famous sites of massivestar formation with pronounced diffuse X-ray emission: M17, NGC 3576, NGC 3603,and 30 Doradus. All spectral models require at least two diffuse thermal plasmacomponents to achieve adequate spectral fits, a softer component with kT =0.2--0.6 keV and a harder component with kT = 0.5--0.9 keV. In several casesthese hot plasmas appear to be in a state of non-equilibrium ionization thatmay indicate recent and current strong shocks. A cavity north of the embeddedgiant HII region NGC 3576 is the only region studied here that exhibits harddiffuse X-ray emission; this emission appears to be nonthermal and is likelydue to a recent cavity supernova, as evidenced by a previously-known pulsar andnewly-discovered pulsar wind nebula also seen in this cavity. All of thesetargets exhibit X-ray emission lines that are not well-modeled byvariable-abundance thermal plasmas and that might be attributed to chargeexchange at the shock between the hot, tenuous, X-ray-emitting plasma and cold,dense molecular material; this is likely evidence for dust destruction at themany hot/cold interfaces that characterize massive star-forming regions.

The Integrated Diffuse X-ray Emission of the Carina Nebula Compared to Other Massive Star-forming Regions