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Debris disks often take the form of eccentric rings with azimuthalasymmetries in surface brightness. Such disks are often described as showing"pericenter glow", an enhancement of the disk brightness in regions nearest thecentral star. At long wavelengths, however, the disk apocenters should appearbrighter than their pericenters: in the long wavelength limit, we find theapocenter/pericenter flux ratio scales as 1+e for disk eccentricity e. Weproduce new models of this "apocenter glow" to explore its causes andwavelength dependence and study its potential as a probe of dust grainproperties. Based on our models, we argue that several far-infrared and(sub)millimeter images of the Fomalhaut and epsilon Eridani debris ringsobtained with Herschel, JCMT, SHARC II, ALMA, and ATCA should be reinterpretedas suggestions or examples of apocenter glow. This reinterpretation yields newconstraints on the disks' dust grain properties and size distributions.

Apocenter glow in eccentric debris disks: implications for Fomalhaut and epsilon Eridani