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Chapter 11: Problem 23

What is flake tectonics? Why does Venus exhibit flake tectonics rather than plate tectonics?

Short Answer

Expert verified
Flake tectonics is a geological phenomenon where the lithosphere of a planet breaks into small pieces, or 'flakes', that interact with each other. It differs from plate tectonics, where the lithosphere breaks into larger plates. Venus exhibits flake tectonics instead of plate tectonics due to its more uniform and less fragmentary lithosphere that lacks conditions such as plate boundaries and seafloor spreading zones required for plate tectonics.

Step by step solution

01

Definition of Flake Tectonics

Flake tectonics refers to the geological phenomena where the lithosphere, the rigid outermost shell of a terrestrial planet, breaks into small pieces or 'flakes' that move and interact with each other. This tectonic activity is a significant process in shaping the crust of a planet.
02

Definition of Plate Tectonics

Plate tectonics is another geological phenomenon where the Earth's lithosphere is broken into large pieces or 'plates'. These plates move and interact due to the convective forces in the underlying mantle layer, leading to the creation of tectonic features like mountains, ocean trenches, and volcanoes.
03

Comparison between Flake and Plate Tectonics

The main difference between flake and plate tectonics lies in the size of the pieces that the lithosphere is broken into. In flake tectonics, the lithosphere breaks into many smaller pieces or 'flakes', whereas, in plate tectonics, the lithosphere is broken into larger 'plates'.
04

Tectonics on Venus

On Venus, the tectonic activity is characterized by the lithosphere breaking into smaller pieces, which is indicative of flake tectonics. This is because Venus lacks the conditions necessary for plate tectonics. Specifically, it lacks plate boundaries and seafloor spreading zones. Instead, it has a more uniform and less fragmentary lithosphere that breaks into smaller pieces, exhibiting flake tectonics.

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Most popular questions from this chapter

(a) Suppose you have a telescope with an angular resolution of 1 arcsec. What is the size (in kilometers) of the smallest feature you could have seen on the Martian surface during the opposition of 2005 , when Mars was \(0.464\) AU from Earth? (b) Suppose you had access to the Hubble Space Telescope, which has an angular resolution of \(0.1\) arcsec. What is the size (in kilometers) of the smallest feature you could have seen on Mars with the HST during the 2005 opnosition?

What is the Martian crustal dichotomy? What is the evidence that the southern highlands are older than the northern lowlands?

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