The pn spectra of WR89 (top) and WR87 (bottom), along with their best-fit spectral models shown as solid lines (see Table 2). While both stars are subject to similar interstellar absorptions (Vázquez & Baume 2001), the spectrum of WR87 is obviously much harder and fainter. A dotted blue line shows the best-fit to WR87 spectra when kT is fixed to 0.6 keV (see text). The color version of this figure is available online.