Abstract: Hot, luminous, massive stars are strong sources of soft X-ray emission, despite their general lack of surface magnetic fields and the associated dynamo activity and MHD processes that heat a corona and explain the X-ray emission of solar-type stars. Since massive stars' surprising discovery as X-ray sources in the late 1970s, a consensus has emerged that the X-rays are produced in their strong radiation-driven winds. I will show how high-resolution X-ray spectroscopy carried out over the past decade with the Chandra and XMM-Newton satellite observatories has confirmed the basic wind-shock scenario of X-ray production in massive stars and enabled the testing of theoretical models by providing quantitative constraints on the temperature, spatial distribution, and kinematics of the X-ray emitting plasma embedded in the stellar wind. I will also discuss how absorption signatures in the X-ray spectra can be used to measure the mass-loss rates of these winds, and present some initial results that indicate lower mass-loss rates than have been traditionally assumed. When combined with observations in the optical and radio, these X-ray absorption measurements also provide information about the clumping properties of massive star winds.