Fig. 4.
From: Revisiting astronomical crystalline forsterite in the UV to near-IR
DUSTY model runs for a spherical shell of dust around a central star of Tstar = 3000 or 30,000 K, and optical depth τ 10 µ m = 0.01 or 0.1, using different options for silicate dust. Insets show behavior of total flux at shorter wavelengths and the dust temperature as a function of radial parameter. The choice whether to use all constructed n,k (“astronomical silicate” from Draine, 2003b), all laboratory n, k (forsterite, this work), or a combination of constructed and laboratory n,k (“astronomical silicate” by Draine, 2003b + forsterite IR by Sogawa et al., 2006, merged by N. Wright) makes a profound difference to modeled Ftot.