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Fig. 3.

image

Extinction-corrected absolute magnitudes (Mg) of AM CVn binaries as a function of orbital period. For known outbursting systems, we plot the quiescent magnitude, and show the magnitude change during outburst as a dotted line. The dashed line is the predicted MV of the accretion disc as originally taken from Nelemans et al. (2004) while the solid line shows the evolution of a 0.65M accreting white dwarf with a high-entropy white dwarf donor, including accretion heating, from Bildsten et al. (2006). Most systems appear somewhat brighter than an isolated white dwarf model during quiescence, and close to the duty-cycle-scaled disc magnitude during outburst.

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