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We present some of the salient aspects of the scientific motivation for highresolution soft X-ray spectroscopy of early-type stars with the Line EmissionMapper X-ray Probe. The major strength of {\it LEM} for hot star physics is itslarge effective area, aided by the inherent energy resolution of itsmicrocalorimeter that readily achieves resolving powers of 1000 and obviatesthe need for relatively inefficient dispersive optical elements. This increasedsensitivity enables much fainter and more distant high mass stars to beobserved than are accessible with present-day facilities, greatly increasingthe pool of potential targets. For brighter sources, the sensitivity opens uptime domain studies, wherein sufficient signal can be garnered in short orderand exposure times, probing source variations on ks timescales. We argue thatthese capabilities of {\it LEM} will yield breakthroughs in all types of hotstar systems, from understanding single OB and WR star winds and how they varywith metallicity, to probing the shocks of colliding wind systems and themagnetically channeled winds of magnetic OB stars. {\it LEM} will also studythe energetics of WR star bubbles and feedback from their powerful pre-SNstellar winds.

Addressing Outstanding Problems in the Physics of Massive Stars with the Line Emission Mapper X-ray Probe