High resolution X-ray spectra of very young massive stars opened a new chapter in the diagnostics and understanding of the properties of stellar wind plasmas. Observations of several very young early type stars in the Orion Trapezium demonstrated that the conventional model of shock heated plasmas in stellar winds is not sufficient to explain the observed X-ray spectra. Detailed X-ray line diagnostics revealed extreme temperatures in some of the candidates as well as evidence for high plasma densities. It is also evident from high resolution spectra of more conventional early type stars, that not all show such extreme characteristics. However, the fact that some of the stars show hot and dense components and some do not requires more understanding of the physical processes involved in stellar wind emissions. The Orion Trapezium stars distinguish themselves from all the others by their extreme youth. By comparing the diverse spectral properties of theta Ori A and theta Ori E with those of theta Ori C, we further demonstrate that X-ray spectral properties of very young massive stars are far from understood.
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