ASTR 3 Lecture Notes - Lecture 11: Terrestrial Planet
Document Summary
The tectonic plates in other terrestrial planets: moon. It was hit and the magna flowed out to form maria. To have plate tectonics, need internal heat, but moon has cooled since formed: mercury. Mercury has no plate tectonics, but has very heavily craters. Cliffs are evidence for shrinking that followed the cooling of the planet: venus. Continuing geology removing the craters: (cid:28649)(cid:28664)(cid:28673)(cid:28680)(cid:28678) (cid:28663)(cid:28674)(cid:28664)(cid:28678)(cid:28673)"(cid:28679) (cid:28667)(cid:28660)(cid:28681)(cid:28664) erosion like earth, but volcanos are erupting and covering the craters. Shield volcanos are formed from the mantle plumbs. Venus has no plate tectonics or erosions, but it has thick crusts. (cid:28648)(cid:28673)(cid:28671)(cid:28668)(cid:28670)(cid:28664) (cid:28664)(cid:28660)(cid:28677)(cid:28679)(cid:28667)"s volcanos, the volcanos on venus are different: they appear to be episodic (on a periodical basis): mars. The northern hemisphere is smoother than the southern side: the north is being covered up after some of the craters were created. We can say that geologically the northern side is younger than the southern side. Mars is smaller than earth, so it lost heat faster.
