“…We used six different thermophysical models for each asteroid, five of which differed only in thermal inertia (P), with values of P equal to 0.0006, 0.002, 0.01, 0.05, and 0.4 cal s −1/2 cm −2 K −1 , corresponding to the values for 1 Ceres, the Moon (and Mercury, Phobos, and Mars), loose pumice, basalt, and iron, respectively (Rees 1990, Betts et al 1995, Chase et al 1976, Ksanfomality et al 1991, Morrison 1976). The final thermophysical model had the same thermal inertia as the iron model, but it had an emissivity ( ) equal to 0.6, rather than 0.9 as with the other model.…”