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Dike intrusion as a possible cause of linear Martian magnetic anomalies

2000; Geological Society of America; Volume: 28; Issue: 5 Linguagem: Inglês

10.1130/0091-7613(2000)28 2.0.co;2

1943-2682

F. Nimmo,

Astro and Planetary Science

Research Article| May 01, 2000 Dike intrusion as a possible cause of linear Martian magnetic anomalies Francis Nimmo Francis Nimmo 1Bullard Laboratories, Department of Earth Sciences, Madingley Road, Cambridge CB3 0EZ, UK Search for other works by this author on: GSW Google Scholar Geology (2000) 28 (5): 391–394. https://doi.org/10.1130/0091-7613(2000)28 2.0.CO;2 Article history received: 30 Aug 1999 rev-recd: 26 Jan 2000 accepted: 04 Feb 2000 first online: 02 Jun 2017 Cite View This Citation Add to Citation Manager Share Icon Share Facebook Twitter LinkedIn MailTo Tools Icon Tools Get Permissions Search Site Citation Francis Nimmo; Dike intrusion as a possible cause of linear Martian magnetic anomalies. Geology 2000;; 28 (5): 391–394. doi: https://doi.org/10.1130/0091-7613(2000)28 2.0.CO;2 Download citation file: Ris (Zotero) Refmanager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentBy SocietyGeology Search Advanced Search Abstract A model in which the ancient, 100–200-km-wide magnetic lineations in the southern hemisphere of Mars are formed by repeated dike intrusion is proposed. On the basis of magnetizations observed at terrestrial mid-ocean ridges, a likely upper bound on the Martian crustal magnetization is about 15 A m−1. This upper bound gives a minimum magnetized layer thickness of 35–60 km. Because the magnetic material is likely to be magnetite, the long-term stability of the anomalies probably requires ilmenite lamellae to have exsolved from the magnetite. This exsolution process provides an upper bound on the cooling time available of 102–105 yr. These bounds can be satisfied if the magnetic anomalies are created by successive intrusion of dikes from 20 to 2000 m wide. Production of a Martian crust 35–60 km thick by rifting requires either mantle potential temperatures in excess of 1430 °C or stretching factors greater than 5. You do not have access to this content, please speak to your institutional administrator if you feel you should have access.