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Figure 1: The raw spectra of 1.0-M white dwarfs for = 0, 1, and 100.

 
Figure 2: Same as Fig. 1 for 0.5-M white dwarfs.

 
Figure 3: The simulated HEG spectra of accreting white dwarfs with (M/M, ) = (0.5,0), (0.5,1) and (1.0,100). Most of the variations in the continuum are due to variations in the instrument sensitivity. The grating disperses the photons in both the plus and minus directions over several CCD chips. For these simulations, we assume the two spectra have been added. However, the gaps between the chips cause the drops near 0.95, 1.2, 1.7, 2.8, and 8.5 keV. The mirrors are coated with Ir which has strong absorption edges just above 2 keV.

 
Figure 4: Same as Fig. 3 for the MEG. Here, the chip boundaries occur near 0.85, 1.4, and 4.2 keV.

 
Figure 5: The simulated ASCA SIS spectra of accreting white dwarfs with parameters the same as those in Fig. 3 and 4.

 
Figure 6: The simulated MEG spectra in linear scales of photon count and energy. The parameters of the simulations are the same as those in Fig. 3 and 4.

 
Figure 7: The simulated O VII He4 and He5 lines for M = 1.0 M and = 100.

© Copyright Astronomical Society of Australia 1997