Hot Stars: Beyond the balmer jump
Review articleOpen access

AbstractWe review the contribution of ultraviolet astronomy to the study of OB stars. UV resonance lines of ions such as C3+, N4+, and Si3+ provide sensitive indicators of mass loss for OB stars. We show how observations of the corresponding P Cygni profiles have tested basic predictions of stellar wind theory— that mass-loss rates should scale with luminosity, that maximum flow velocites should scale with surface escape velocities, and that both should scale with metallicity. We emphasize the rôle that IUE has played in providing an understanding of variability in stellar winds, and conclude with an outline of the likely significance of future observations made below the IUE (and HST) limit of ∼120nm, down to ∼10nm.

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