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We address the inversion problem of deriving the differential emission measure (DEM) distribution D(T) =nenHdV/d log T from the spectrum of an optically thin plasma. In the past we have applied the iterative Withbroe-Sylwester technique and the Polynomial technique to the analysis ofEXOSATspectra of cool stars, but recently we have applied the inversion technique discussed by Craig & Brown (1986) and Press et al. (1992) in the analysis ofEUVEspectra of cool stars. The inversion problem-adoi:10.1017/s0252921100036538 fatcat:u5kqoka4ozfa5myoj4hzldytpi