Visible and near-infrared images of Io from the Galileo spacecraft reveal a
surface more colorful than previously thought. Red, yellow green, white, a
nd black hues decorate the satellite, presumably caused by a varied composi
tion of sulfur compounds and silicates. Almost a third of Io is covered by
red and orange materials, particularly at polar latitudes above +/-30 degre
es. These red regions were scarcely distinguishable in the shorter waveleng
th Voyager observations. Bright red pyroclastic deposits mark the locations
of many hot spots, plumes, and visible surface changes, providing a promin
ent flag of recent volcanic activity. Io's equatorial regions are dominated
by yellow materials, which occupy about 40% of the satellite's surface. Wh
ite and gray materials cover about 27% of Io, primarily in equatorial areas
and in localized deposits at high latitudes. These are identified with mod
erate-to-coarse-grained SO2 as mapped by the NIMS instrument on Galileo (R.
W. Carlson et al, 1997, Geophys, Res. Lett. 24, 2479-2482). Greenish-yello
w materials in small isolated spots on Io's anti-Jupiter hemisphere were re
cently discovered in 3 km/pixel color imaging from orbit 14. Unlike other i
onian terrains, these regions have a negative near-infrared spectral slope,
suggesting contamination by a nonsulfur component. Only about 1.4% of Io's
surface is occupied by dark materials, which display a variety of visible
colors ranging from black to red and green. Most dark spots have a shallow
spectral absorption feature at 0.9 mu m, suggesting magnesium-rich silicate
s rather than black sulfur. Little large-scale alteration in the global col
or and albedo pattern has occurred between the Voyager and Galileo eras; 90
% of the surface appears unchanged despite the vigorous volcanic activity w
hich must have taken place in the intervening 17 years. This suggests that
over a time scale of decades, the bulk of Io's resurfacing is restricted to
a few small but persistently active areas. (C) 1999 Academic Press.