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Is the primordial crust of Mars magnetized?

Arkani-Hamed, Jafar ; Boutin, Daniel

Icarus (New York, N.Y. 1962), 2012-09, Vol.221 (1), p.192-207 [Revista revisada por pares]

Amsterdam: Elsevier Inc

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  • Título:
    Is the primordial crust of Mars magnetized?
  • Autor: Arkani-Hamed, Jafar ; Boutin, Daniel
  • Materias: Astronomy ; Craters ; Crusts ; Earth, ocean, space ; Exact sciences and technology ; Highlands ; Magnetization ; Mars ; Mars surface ; Solar system ; Tempe ; Topography
  • Es parte de: Icarus (New York, N.Y. 1962), 2012-09, Vol.221 (1), p.192-207
  • Notas: ObjectType-Article-1
    SourceType-Scholarly Journals-1
    ObjectType-Feature-2
    content type line 23
  • Descripción: ► Impacts creating craters larger than 200km can demagnetize the entire crust of Mars. ► Craters and QCDS larger than 200km in Tempe Terra have no magnetic signatures. ► The crust underlying the Tempe Terra on Mars is not appreciably magnetized. ► No strong core dynamo existed within the first about 100Myr of Mars history. A meteorite impact capable of creating a 200km diameter crater can demagnetize the entire crust beneath, and produce an appreciable magnetic anomaly at satellite altitudes of ∼400km in case the pre-existing crust is magnetized. In this study we examine the magnetic field over all of the craters and impact-related Quasi-Circular Depressions (QCDs) with diameters larger than 200km that are located on the highlands of Mars, excluding the Tharsis bulge, in order to estimate the mean magnetization of the highland crust. Using the surface topography and the gravity of Mars we first identify those QCDs that are likely produced by impacts. The magnetic map of a given crater or impact-related QCD is derived using the Mars Global Surveyor high-altitude nighttime radial magnetic data. Two extended ancient areas are identified on the highlands, the South Province and the Tempe Terra, which have large number of craters and impact-related QCDs but none of them has an appreciable magnetic signature. The primordial crust of these areas is not magnetized, or is very weakly magnetized at most. We examine some plausible scenarios to explain the weak magnetization of these areas, and conclude that no strong dynamo existed in the first ∼100Myr of Mars’ history when the newly formed primordial crust was cooling below the magnetic blocking temperatures of its minerals.
  • Editor: Amsterdam: Elsevier Inc
  • Idioma: Inglés
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