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We investigate whether varying the dust composition (described by the opticalconstants) can solve a persistent problem in debris disk modeling--theinability to fit the thermal emission without over-predicting the scatteredlight. We model five images of the beta Pictoris disk: two in scattered lightfrom HST/STIS at 0.58 microns and HST/WFC3 at 1.16 microns, and three inthermal emission from Spitzer/MIPS at 24 microns, Herschel/PACS at 70 microns,and ALMA at 870 microns. The WFC3 and MIPS data are published here for thefirst time. We focus our modeling on the outer part of this disk, consisting ofa parent body ring and a halo of small grains. First, we confirm that a modelusing astronomical silicates cannot simultaneously fit the thermal andscattered light data. Next, we use a simple, generic function for the opticalconstants to show that varying the dust composition can improve the fitsubstantially. Finally, we model the dust as a mixture of the most plausibledebris constituents: astronomical silicates, water ice, organic refractorymaterial, and vacuum. We achieve a good fit to all datasets with grainscomposed predominantly of silicates and organics, while ice and vacuum are, atmost, present in small amounts. This composition is similar to one derived fromprevious work on the HR 4796A disk. Our model also fits the thermal SED,scattered light colors, and high-resolution mid-IR data from T-ReCS for thisdisk. Additionally, we show that sub-blowout grains are a necessary componentof the halo.

A Comprehensive Dust Model Applied to the Resolved Beta Pictoris Debris Disk from Optical to Radio Wavelengths