Geology Reference
In-Depth Information
Figure 4.38. This row of small cones in Oceanus Procellarum
intersects the crater Hortensius D and is thought to consist of
volcanic spatter; each cone is less than a fewhundredmeters across
(NASA LO IV H-133).
Figure 4.37. These low-shield volcanoes are about 10 km across
and occur in mare deposits of the Orientale basin; they represent a
style of basaltic volcanism typi
ed by eruptions of low-volume
fluid
lavas (NASA LO IVH-181).
Figure 4.40. A view of the Harbinger Mountains (left+side), viewed
south across the mare plains of Oceanus Procellarum and east of the
crater, Aristarchus (on the right). The numerous sinuous rilles
indicate extensive volcanism in this part of theMoon. Note the 46 km
in diameter crater Prinz that has been partly
flooded by mare basalts
(NASA AS 15
Figure 4.39. The Hyginus Rille is more than 200 km
long and contains a series of rimless craters, some as large as
12 km across. The rille is likely to be a graben, while the
craters are probably of endogenic origin, possibly
analogous to volcanic pit craters formed by collapse (NASA LO
VM-97).
-
2607).
by Pete Schultz suggest that they represent intrusion of
magma along fracture systems generated by the impact
which lifts the
floor units, including central peak structures,
to higher-than-normal elevations (
Fig. 4.42(b)
).
