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http://onlinelibrary.wiley.com/doi/10.1029/2012JE004237/abstract
[1] The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4) lithospheric stresses. Each of these mechanisms could play a role in compensating topography on Venus, and we distinguish between these mechanisms in part by calculating geoid‐to‐topography …
http://www-geodyn.mit.edu/zubersite/pdfs/jamesetal2013jgr.pdf
[1] The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4) lithospheric stresses. Each of these mechanisms could play a role in compensating topography on Venus, and we distinguish between these mechanisms in part
https://dspace.mit.edu/handle/1721.1/85638
The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support…Cited by: 43
https://www.researchgate.net/publication/258796987_Crustal_thickness_and_support_of_topography_on_Venus
The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4 ...
http://adsabs.harvard.edu/abs/2013JGRE..118..859J
The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support…
http://onlinelibrary.wiley.com/doi/10.1029/2012JE004237/full
Mantle load distribution (in units of kg m − 3 ) for a mean crustal thickness of 15 km and a mantle load depth of 250 km. Warm colors indicate a mass deficit in the mantle and positive buoyancy; cool colors indicate mass excess and negative buoyancy.
https://www.researchgate.net/publication/272040240_The_gravity_field_and_crustal_thickness_of_Venus
The gravity field and crustal thickness of Venus. The gravity and topography of Venus obtained from observations of the Magellan mission, as well as the gravity and topography from our numerical mantle convection model, are discussed in this paper.
https://www.lpi.usra.edu/meetings/lpsc2010/pdf/2663.pdf
GEOID TO TOPOGRAPHY RATIOS ON VENUS AND IMPLICATIONS FOR CRUSTAL THICKNESS. P. B. James 1, M. T. Zuber, and R. J. Phillips2, Department of Earth, Atmospheric and Planetary Sciences, Massa- chusetts Institute of Technology, [email protected] 2Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302.
https://en.wikipedia.org/wiki/Geology_of_Venus
Venus's crust appears to be 70 kilometres (43 mi) thick, and composed of silicate rocks. Venus's mantle is approximately 2,840 kilometres (1,760 mi) thick, its chemical composition is …
https://www.lpi.usra.edu/meetings/lpsc2011/pdf/2456.pdf
maximum thickness of the crust, and the impossibility of negative crustal thickness provides a lower bound. For a reasonable choice of geologic parameters, we can give a plausible upper bound of 24 km for the mean crustal thickness and a lower bound of 11 km. Data: The Magellan mission to Venus …
http://onlinelibrary.wiley.com/doi/10.1029/2012JE004237/abstract
[1] The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4) lithospheric stresses. Each of these mechanisms could play a role in compensating topography on Venus, and we distinguish between these mechanisms in part by calculating geoid‐to‐topography ratios ...
http://www-geodyn.mit.edu/zubersite/pdfs/jamesetal2013jgr.pdf
(1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4) lithospheric stresses. Each of these mechanisms could play a role in compensating topography on Venus, and we distinguish between these mechanisms in part by calculating geoid-to-topography ratios and apparent depths of compensation. By
http://onlinelibrary.wiley.com/doi/10.1029/2012JE004237/full
Abstract [1] The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) d
https://www.researchgate.net/publication/258796987_Crustal_thickness_and_support_of_topography_on_Venus
The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4 ...
http://adsabs.harvard.edu/abs/2013JGRE..118..859J
Abstract The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4) lithospheric stresses.
https://www.lpi.usra.edu/meetings/lpsc2010/pdf/2663.pdf
GEOID TO TOPOGRAPHY RATIOS ON VENUS AND IMPLICATIONS FOR CRUSTAL THICKNESS. P. B. James 1, M. T. Zuber, and R. J. Phillips2, Department of Earth, Atmospheric and Planetary Sciences, Massa- chusetts Institute of Technology, [email protected] 2Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302.
https://www.researchgate.net/publication/272040240_The_gravity_field_and_crustal_thickness_of_Venus
The topography of a terrestrial planet can be supported by several mechanisms: (1) crustal thickness variations, (2) density variations in the crust and mantle, (3) dynamic support, and (4 ...
https://principia-scientific.org/whats-really-going-on-with-venus-two-gas-planets-comparison/
Aug 24, 2017 · (Crustal thickness and support of topography on Venus, 2013) In another paper (one done in 1982), came to a similar conclusion. That the core of Venus…
https://www.lpi.usra.edu/meetings/lpsc2011/pdf/2456.pdf
ed that support of topography comes only from crustal thickness variations and mantle mass anomalies. Given high geoid/topography ratios observed on Venus [10] there is the expectation of dynamic uplift, which we have not yet explicitly considered. Future work will explore the effects of dynamic support on the Venusian crustal thickness model.
https://en.wikipedia.org/wiki/Geology_of_Venus
The surface of Venus is comparatively flat. When 93% of the topography was mapped by Pioneer Venus Orbiter, scientists found that the total distance from the lowest point to the highest point on the entire surface was about 13 kilometres (8.1 mi), about the same as the vertical distance between the Earth's ocean floor and the higher summits of the Himalayas.
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