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The Huygens-Hellas Giant Dike System on Mars: Implications for Late Noachian-Early Hesperian Volcanic Resurfacing and Climatic Evolution.

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The Huygens-Hellas Giant Dike System on Mars: Implications for Late Noachian-Early Hesperian Volcanic Resurfacing and Climatic Evolution. / Wilson, Lionel; Dickson, J.; Head, James W.; Neukum, G.

In: Geology, Vol. 34, No. 4, 01.04.2006, p. 285-288.

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@article{58a6917921734457bf2acabc91888fbc,
title = "The Huygens-Hellas Giant Dike System on Mars: Implications for Late Noachian-Early Hesperian Volcanic Resurfacing and Climatic Evolution.",
abstract = "Two narrow, broadly arcuate, low ridges extend for 600–700 km in western Terra Tyrrhena, Mars, crosscut ancient Noachian terrain, and are associated with Early Hesperian plains, which cover 30% of Mars. Geological relationships suggest that the ridges represent near-surface erosional remnants of subsurface dikes, solidified magma-filled cracks that were responsible for the volcanic emplacement of the plains. Ridge width and geometry are consistent with very high-effusion-rate flood basalt eruptions, emplacement events that would form smooth featureless plains and input significant volcanic gas into the atmosphere. Geological relationships suggest that the ridges were exposed by erosion (fluvial, sublimation, eolian) and partial removal of a regional volatile-rich dust layer.",
keywords = "dike, Noachian, Hesperian, magma, Mars, eruptions",
author = "Lionel Wilson and J. Dickson and Head, {James W.} and G. Neukum",
note = "Wilson provided the mathematical modelling, Head and Dickson (Brown Univ.) the morphometry, and Neukum (Berlin) the spacecraft data. Eroded dyke outcrops on Mars provide partial information on the history of the crust, allowing questions to be formulated for upcoming spacecraft missions. RAE_import_type : Journal article RAE_uoa_type : Earth Systems and Environmental Sciences",
year = "2006",
month = apr
day = "1",
doi = "10.1130/G22163.1",
language = "English",
volume = "34",
pages = "285--288",
journal = "Geology",
issn = "0091-7613",
publisher = "Geological Society of America",
number = "4",

}

RIS

TY - JOUR

T1 - The Huygens-Hellas Giant Dike System on Mars: Implications for Late Noachian-Early Hesperian Volcanic Resurfacing and Climatic Evolution.

AU - Wilson, Lionel

AU - Dickson, J.

AU - Head, James W.

AU - Neukum, G.

N1 - Wilson provided the mathematical modelling, Head and Dickson (Brown Univ.) the morphometry, and Neukum (Berlin) the spacecraft data. Eroded dyke outcrops on Mars provide partial information on the history of the crust, allowing questions to be formulated for upcoming spacecraft missions. RAE_import_type : Journal article RAE_uoa_type : Earth Systems and Environmental Sciences

PY - 2006/4/1

Y1 - 2006/4/1

N2 - Two narrow, broadly arcuate, low ridges extend for 600–700 km in western Terra Tyrrhena, Mars, crosscut ancient Noachian terrain, and are associated with Early Hesperian plains, which cover 30% of Mars. Geological relationships suggest that the ridges represent near-surface erosional remnants of subsurface dikes, solidified magma-filled cracks that were responsible for the volcanic emplacement of the plains. Ridge width and geometry are consistent with very high-effusion-rate flood basalt eruptions, emplacement events that would form smooth featureless plains and input significant volcanic gas into the atmosphere. Geological relationships suggest that the ridges were exposed by erosion (fluvial, sublimation, eolian) and partial removal of a regional volatile-rich dust layer.

AB - Two narrow, broadly arcuate, low ridges extend for 600–700 km in western Terra Tyrrhena, Mars, crosscut ancient Noachian terrain, and are associated with Early Hesperian plains, which cover 30% of Mars. Geological relationships suggest that the ridges represent near-surface erosional remnants of subsurface dikes, solidified magma-filled cracks that were responsible for the volcanic emplacement of the plains. Ridge width and geometry are consistent with very high-effusion-rate flood basalt eruptions, emplacement events that would form smooth featureless plains and input significant volcanic gas into the atmosphere. Geological relationships suggest that the ridges were exposed by erosion (fluvial, sublimation, eolian) and partial removal of a regional volatile-rich dust layer.

KW - dike

KW - Noachian

KW - Hesperian

KW - magma

KW - Mars

KW - eruptions

U2 - 10.1130/G22163.1

DO - 10.1130/G22163.1

M3 - Journal article

VL - 34

SP - 285

EP - 288

JO - Geology

JF - Geology

SN - 0091-7613

IS - 4

ER -