Heat-pipe tectonics is a cooling mode of terrestrial planets and moons in which the main heat transport mechanism in the planet is volcanism through the outer hard shell, also called the lithosphere.[1][2] Heat-pipe tectonics initiates when volcanism becomes the dominant surface heat transfer process.[1] Melted rocks and other more volatile planetary materials are transferred from the mantle to surface via localised vents.[1] Melts cool down and solidify forming layers of cool volcanic materials.[1] Newly erupted materials deposit on top of and bury older layers.[1] The accumulation of volcanic layers on the shell and the corresponding evacuation of materials at depth cause the downward transfer of superficial materials such that the shell materials continuously descend toward the planet's interior.[1]
Heat-pipe tectonics was first introduced based on the observations on Io, one of the moons of Jupiter.[1][2] Io is a rocky body that is internally extremely hot; its heat is produced by tidal flexing associated with its eccentric orbit.[2][3][4][5] It releases internal heat via frequent and extensive volcanic eruptions that transfer melts to the surface.[2][6][7] Its crust is a single thick, dense and cold outer shell made up of layers of volcanic materials, whose rigidity and strength supports the weight of high mountains.[3][2][8]
Observations suggest that similar processes occurred in the early history of other terrestrial planets in the Solar System, i.e. Venus, the Moon, Mars, Mercury and Earth, indicating they may preserve fossil heat-pipe evidence.[9] Every terrestrial body in our Solar System might have had heat-pipe tectonics at some point; heat-pipe tectonics may thus be a universal early cooling mode of terrestrial bodies.[9]
- ^ a b c d e f g Moore, William B.; Webb, A. Alexander G. (2013). "Heat-pipe Earth". Nature. 501 (7468): 501–505. Bibcode:2013Natur.501..501M. doi:10.1038/nature12473. ISSN 0028-0836. PMID 24067709. S2CID 4391599.
- ^ a b c d e O'Reilly, Thomas C.; Davies, Geoffrey F. (1981). "Magma transport of heat on Io: A mechanism allowing a thick lithosphere". Geophysical Research Letters. 8 (4): 313–316. Bibcode:1981GeoRL...8..313O. doi:10.1029/gl008i004p00313. ISSN 0094-8276.
- ^ a b Breuer, D.; Moore, W.B. (2007), "Dynamics and Thermal History of the Terrestrial Planets, the Moon, and Io", Treatise on Geophysics, Elsevier, pp. 299–348, doi:10.1016/b978-044452748-6.00161-9, ISBN 9780444527486
- ^ Tackley, P (2001). "Three-Dimensional Simulations of Mantle Convection in Io". Icarus. 149 (1): 79–93. Bibcode:2001Icar..149...79T. doi:10.1006/icar.2000.6536. ISSN 0019-1035. S2CID 15288576.
- ^ PEALE, S. J.; CASSEN, P.; REYNOLDS, R. T. (1979-03-02). "Melting of Io by Tidal Dissipation". Science. 203 (4383): 892–894. Bibcode:1979Sci...203..892P. doi:10.1126/science.203.4383.892. ISSN 0036-8075. PMID 17771724. S2CID 21271617.
- ^ SMITH, B. A.; SODERBLOM, L. A.; JOHNSON, T. V.; INGERSOLL, A. P.; COLLINS, S. A.; SHOEMAKER, E. M.; HUNT, G. E.; MASURSKY, H.; CARR, M. H.; DAVIES, M. E.; COOK, A. F. (1979-06-01). "The Jupiter System Through the Eyes of Voyager 1". Science. 204 (4396): 951–972. Bibcode:1979Sci...204..951S. doi:10.1126/science.204.4396.951. ISSN 0036-8075. PMID 17800430. S2CID 33147728.
- ^ Carr, M. H.; Masursky, H.; Strom, R. G.; Terrile, R. J. (1979). "Volcanic features of Io". Nature. 280 (5725): 729–733. Bibcode:1979Natur.280..729C. doi:10.1038/280729a0. ISSN 0028-0836.
- ^ McNutt, Marcia (1980-11-10). "Implications of regional gravity for state of stress in the Earth's crust and upper mantle". Journal of Geophysical Research: Solid Earth. 85 (B11): 6377–6396. Bibcode:1980JGR....85.6377M. doi:10.1029/jb085ib11p06377. ISSN 0148-0227.
- ^ a b Moore, William B.; Simon, Justin I.; Webb, A. Alexander G. (2017). "Heat-pipe planets". Earth and Planetary Science Letters. 474: 13–19. Bibcode:2017E&PSL.474...13M. doi:10.1016/j.epsl.2017.06.015. ISSN 0012-821X.
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