Predicted values of the Yarkovsky effect and density for asteroid (2100) Ra-Shalom. Bottom panel: Predicted semimajor axis drift da/dt (ordinate) due to the Yarkovsky effect from our model for three different values of the bulk density (2, 2.5, and 3 g cm⁻³; see the labels) are shown by solid curves. The abscissa is the surface thermal inertia in SI units (Jm⁻² s^−0.5 K⁻¹). We assumed the rotation state and shape model from the light-curve inversion in Sect. 2.2 and an effective size of 2.3 km. The grayscale horizontal region shows the value −(2.01 ± 0.43) × 10⁻⁴ auMy⁻¹ from the orbit determination. The vertical dashed line indicates the suggested surface high-thermal inertia of ≃ 1000 Jm⁻² s^−0.5 K⁻¹. Top panel: Model-predicted bulk density to match the observed value of the semimajor axis drift shown by the grayscale region. The solid line in the middle shows the exact correspondence surrounded by a map of the sigma interval of the Yarkovsky drift. A nominal effective size of 2.3 km is used. If this value were higher or lower, the density solution would shift in the direction indicated by the arrows (preserving the ρ_b D value). The analysis of 10 different shape models of (2100) Ra-Shalom reveals a variation of ±10% about the median value used in the figure. Effects of small-scale surface roughness, if important, would shift the solution toward a lower value by typically 10–30% (see Rozitis & Green 2012).