This model was made using MATLAB R2016a on the DEM (digital elevation map) of Io from White et al (2014). Like with many of the colored map based models I've made, there could be many feature artifacts of the colour-level decodification algoritm. The original map is not complete and some parts are very scattered, so I fill the gap using interpolation.
The file's names explained: name_1_x_10_y.stl is 1 : x * 10y. So _1_6_10_7 is 1:600000000 or one in 60 million.
White, O. L., P. M. Schenk, F. Nimmo, and T. Hoogenboom (2014), A new stereo topographic map of Io: Implications for geology from global to local scales, J. Geophys. Res. Planets, 119, doi:10.1002/2013JE004591.
Io is the most proximal to Jupiter of the Galilean moons, and the third of them in size. It is slightly bigger than the Moon. It is the most geologically active object in the Solar System, because is the object most afected by tidal heating. That is heating because the different gravity influence of Jupiter along its orbit, which is maintain eccentric by its resonance with Europa and Ganymede. The heating is so extreme that nearly all the volatiles (water and hydrogen) have scape from the surface.
Orbital period: 1.769 d.
Composition: Silicate rock. Differenciated interior. Iron core
Density: 3.528 g/cm3.
Dimensions: 3660.0 km × 3637.4 km × 3630.6 km.
Model scale: 1:2x107 (18cm) 1:6x107 (6cm)