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English: How crater-depth is measured, using the side-view of a typical crater. Depth "A" measures from the surface to the bottom of the crater. Depth "B" measures from the mean height of the rim to the bottom of the crater.
The depth of an impact crater in a solid planet or moon may be measured from the local surface to the bottom of the crater, or from the rim of the crater to the bottom. Crater depth diagram. The diagram above shows the full (side) view of a typical crater. Depth "A" measures from the surface to the bottom of the crater.
The table below is arranged by the continent's percentage of the Earth's land area, and where Asian and Russian structures are grouped together per EID convention. The global distribution of known impact structures apparently shows a surprising asymmetry, [ 37 ] with the small but well-funded European continent having a large percentage of ...
Cross-cutting relationships can be used to determine the relative ages of rock strata and other structures. Explanations: A – folded rock strata cut by a thrust fault; B – large intrusion (cutting through A); C – erosional angular unconformity (cutting off A & B) on which rock strata were deposited; D – volcanic dike (cutting through A, B & C); E – even younger rock strata (overlying ...
A central-peak crater is the most basic form of complex crater. A central-peak crater can have a tightly spaced, ring-like arrangement of peaks, thus be a peak ring crater, though the peak is often single. [3] Central-peak craters can occur in impact craters via meteorites. An Earthly example is Mistastin crater, in Canada. [1]
Unnamed wrinkle ridges north of the lunar crater Flamsteed, Oceanus Procellarum, from Apollo 12 A wrinkle ridge is a type of feature commonly found on lunar maria , or basalt plains. These features are low, sinuous ridges formed on the mare surface that can extend for up to several hundred kilometers.
Shield volcano in Tharsis region on Mars with marked borders, circles represent impact craters counted by crater counting method. Crater counting is a method for estimating the age of a planet's surface based upon the assumptions that when a piece of planetary surface is new, then it has no impact craters; impact craters accumulate after that at a rate that is assumed known.
Valhalla Basin on Jupiter's moon Callisto, taken by Voyager 1. A multi-ringed basin (also a multi-ring impact basin) is not a simple bowl-shaped crater, or a peak ring crater, but one containing multiple concentric topographic rings; [1] a multi-ringed basin could be described as a massive impact crater, surrounded by circular chains of mountains [2] resembling rings on a bull's-eye.