Is the primordial crust of Mars magnetized?

Arkani‐Hamed, J.; Boutin, D.

doi:10.1016/j.icarus.2012.07.030

Cited by 7 publications

(8 citation statements)

References 47 publications

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“…It has been proposed on the basis of the surface distribution of the magnetic anomalies that this magnetization event predated the formation of the Hellas and Argyre basins Lillis et al, 2013), roughly at the end of the Early Noachian (Head et al, 2001). However, the lack of an appreciable magnetization in two ancient areas on the highlands, the South Province and the Tempe Terra, further suggests that no strong dynamo existed in the first $100 My of Mars' history (Arkani-Hamed and Boutin, 2012). However, the lack of an appreciable magnetization in two ancient areas on the highlands, the South Province and the Tempe Terra, further suggests that no strong dynamo existed in the first $100 My of Mars' history (Arkani-Hamed and Boutin, 2012).…”

Section: Marsmentioning

confidence: 99%

“…In the case of the Moon, the lunar magnetic field has been studied indirectly via the natural remanent magnetization of the returned lunar samples and directly with magnetometers carried to the surface and placed in orbit at low altitude above the surface on the Apollo 15 and Apollo 16 subsatellites (see reviews in Dyal et al, 1974;Fuller and Cisowski, 1987). Estimates have been made for the Moon (e.g., Garrick-Bethell et al, 2009;Shea et al, 2012;Tikoo et al, 2012) and Mars (e.g., Arkani-Hamed and Boutin, 2012;Lillis et al, 2008, Mitchell et al, 2007. In the case of Mars, Mars Global Surveyor (MGS) measured the magnetic field of the entire planet (Acuñ a et al, 1998).…”

Section: Magnetic Field Generationmentioning

confidence: 99%

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Dynamics and Thermal History of the Terrestrial Planets, the Moon, and Io

Breuer

Moore

2015

Treatise on Geophysics

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Section: Marsmentioning

confidence: 99%

Section: Magnetic Field Generationmentioning

confidence: 99%

Dynamics and Thermal History of the Terrestrial Planets, the Moon, and Io

Breuer

Moore

2015

Treatise on Geophysics

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“…However, it has been pointed out that the interpretation of the magnetization of volcanic features can be ambiguous [ Lillis et al , ] and the surface age might not be representative for the time of (de)magnetization [ Johnson and Phillips , ]. Also, the dynamo may have started before the primordial crust had formed and cooled [ Stevenson , ], or up to 100 Myr later, as there are large regions with no detectable fields over old terrains [ Arkani‐Hamed and Boutin , ]. Another unresolved question is the location of paleopoles, which contain information about the dynamics of the ancient core dynamo as well as true polar wander.…”

Section: Introductionmentioning

confidence: 99%

“…An asymmetric degree‐one convection pattern in the mantle could also be responsible for the formation of the topographic and magnetic dichotomy, either due to the concentration of melt production in one hemisphere [ Citron and Zhong , ] or due to thermal conditions leading to mineral phase transformations, e.g., the formation of serpentine [ Quesnel et al , ; Chassefière et al , ]. Also, a late start of the dynamo and subsequent localized magnetization by magmatic intrusions has been suggested [ Arkani‐Hamed and Boutin , ], which could have been locally favored by chemical alterations, caused by, e.g., elevated oxygen fugacity and the presence of water in the crust [ Hood et al , ]. Alternatively, the lowlands formation process could have erased any previous magnetization [ Arkani‐Hamed , ].…”

Section: Introductionmentioning

confidence: 99%

A spherical harmonic model of the lithospheric magnetic field of Mars

2014

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Key Points:• SH model up to degree and order 110 of the magnetic lithospheric field of Mars • Several techniques have been used to obtain a stable and wellresolved model • Anomalies over small craters, volcanoes, and isolated anomalies are described Supporting Information:• Readme • Figure S1• Figure S2 • Figure S3 • Figure S4 • Figure S5 • Figure S6 • Figure S7 • Figure S8 • Figure S9 • Table S1 • Table S2 • Table S3 • Table S4 • Table S5 • Table S6 Correspondence to: A. Morschhauser, achim.morschhauser@dlr.de Citation:Morschhauser, A., V. Lesur, and M. Grott (2014) Abstract We present a model of the lithospheric magnetic field of Mars which is based on Mars GlobalSurveyor orbiting satellite data and represented by an expansion of spherical harmonic (SH) functions up to degree and order 110. Several techniques were applied in order to obtain a reliable and well-resolved model of the Martian lithospheric magnetic field: A modified Huber-Norm was used to properly treat data outliers, the mapping phase orbit data was weighted based on an a priori analysis of the data, and static external fields were treated by a joint inversion of external and internal fields. Further, temporal variabilities in the data which lead to unrealistically strong anomalies were considered as noise and handled by additionally minimizing a measure of the horizontal gradient of the vertically down internal field component at surface altitude. Here we use an iteratively reweighted least squares algorithm to approach an absolute measure (L1 norm), allowing for a better representation of strong localized magnetic anomalies as compared to the conventional least squares measure (L2 norm). The resulting model reproduces all known characteristics of the Martian lithospheric field and shows a rich level of detail. It is characterized by a low level of noise and robust when downward continued to the surface. We show how these properties can help to improve the knowledge of the Martian past and present magnetic field by investigating magnetic signatures associated with impacts and volcanoes. Additionally, we present some previously undescribed isolated anomalies, which can be used to determine paleopole positions and magnetization strengths. IntroductionThe Mars Global Surveyor (MGS) spacecraft operated from 1997 to 2006 in Martian orbit and was the first mission to provide magnetic field measurements of Mars at a sufficiently low altitude to reveal the characteristics of the Martian magnetic field. The early mission phases include the aerobraking and science phase orbits (AB/SPO), which are characterized by strongly varying altitudes. At altitudes below 200 km, these early mission phases provide mainly dayside data with sparse global coverage [Acuña et al., 1999]. They are complemented by the later mapping phase orbit (MPO) data, which provide dense global coverage during dayand nighttime at a nearly constant altitude of around 400 km.Earliest results based on AB/SPO data already indicated that Mars does not possess a relevant large-scale magnetic ...

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“…In addition, the Martian mantle mineralogy shows a modest increase in Fe content when compared to the Earth (e.g., Ohtani and Kamaya ; Bertka and Fei ), and the viscosity may be reduced at a given stress by a factor of ~3–5 (Zhao et al. ). A further uncertainty is related to the activation volume, which can vary between 5 × 10 −6 and 20 × 10 −6 m 3 mol −1 (e.g., Karato and Wu ).…”

Section: Interaction Between Volatiles Partial Melting and Mantle Cmentioning

confidence: 99%

Water in the Martian interior—The geodynamical perspective

Breuer

Plesa

Tosi

et al. 2016

Meteorit & Planetary Scien

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Petrological analysis of the Martian meteorites suggests that rheologically significant amounts of water are present in the Martian mantle. A bulk mantle water content of at least a few tens of ppm is thus expected to be present despite the potentially efficient degassing during accretion, magma ocean solidification, and subsequent volcanism. We examine the dynamical consequences of different thermochemical evolution scenarios testing whether they can lead to the formation and preservation of mantle reservoirs, and compare model predictions with available data. First, the simplest scenario of a homogenous mantle that emerges when ignoring density changes caused by the extraction of partial melt is found to be inconsistent with the isotopic evidence for distinct reservoirs provided by the analysis of the Martian meteorites. In a second scenario, reservoirs can form as a result of partial melting that induces a density change in the depleted mantle with respect to its primordial composition. However, efficient mantle mixing prevents these reservoirs from being preserved until present unless they are located in the stagnant lid. Finally, reservoirs could be formed during fractional crystallization of a magma ocean. In this case, however, the mantle would likely end up being stably stratified as a result of the global overturn expected to accompany the fractional crystallization. Depending on the assumed density contrast, little secondary crust would be produced and the lithosphere would be extremely cool and dry, in contrast to observations. In summary, it is very challenging to obtain a self-consistent evolution scenario that satisfies all available constraints. 1960D. Breuer et al.

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Is the primordial crust of Mars magnetized?

Cited by 7 publications

References 47 publications

Dynamics and Thermal History of the Terrestrial Planets, the Moon, and Io

Dynamics and Thermal History of the Terrestrial Planets, the Moon, and Io

A spherical harmonic model of the lithospheric magnetic field of Mars

Water in the Martian interior—The geodynamical perspective

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