On the efficiency of shock magnetization processes

Gattacceca, J.; Berthe, Laurent; Boustie, M.; Vadeboin, F.; Rochette, P.; Rességuier, T. de

doi:10.1016/j.pepi.2007.09.005

Cited by 48 publications

(56 citation statements)

References 24 publications

(15 reference statements)

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“…Nagata 1971;Cisowski and Fuller 1978). A recent experiment shows that SRM possibly has the parallelism and proportionality to the ambient field (Gattacceca et al 2008). In addition to SRM, a shock event may induce piezoremanent magnetization (PRM) in relatively lower pressure and TRM by heating up to blocking temperatures (e.g.…”

Section: Remanence Type and Direction Of The Lunar Crust Magnetizationmentioning

confidence: 97%

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

et al. 2010

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The magnetic field around the Moon has been successfully observed at a nominal altitude of ∼100 km by the lunar magnetometer (LMAG) on the SELENE (Kaguya) spacecraft in a polar orbit since October 29, 2007. The LMAG mission has three main objectives:(1) mapping the magnetic anomaly of the Moon, (2) measuring the electromagnetic and plasma environment around the Moon and (3) estimating the electrical conductivity structure of the Moon. Here we review the instrumentation and calibration of LMAG and report the initial global mapping of the lunar magnetic anomaly at the nominal altitude. We have applied a new de-trending technique of the Bayesian procedure to multiple-orbit datasets observed in the tail lobe and in the lunar wake. Based on the nominal observation of 14 months, global maps of lunar magnetic anomalies are obtained with 95% coverage of the lunar surface. After altitude normalization and interpolation of the magnetic anomaly field by an inverse boundary value problem, we obtained full-coverage maps of the vector magnetic field at 100 km altitude and the radial component distribution on the surface. Relatively strong anomalies are identified in several basin-antipode regions and several near-basin and near-crater regions, while the youngest basin on the Moon, the Orientale basin, has no magnetic anomaly. These features well agree with characteristics of previous maps based on the 220 H. Tsunakawa et al.Lunar Prospector observation. Relatively weak anomalies are distributed over most of the lunar surface. The surface radial-component distribution estimated from the inverse boundary value problem in the present study shows a good correlation with the radial component distribution at 30 km altitude by Lunar Prospector. Thus these weak anomalies over the lunar surface are not artifacts but likely to be originated from the lunar crustal magnetism, suggesting possible existence of an ancient global magnetic field such as a dynamo field of the early Moon. The possibility of the early lunar dynamo and the mechanism of magnetization acquisition will be investigated by a further study using the low-altitude data of the magnetic field by Kaguya.

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Section: Remanence Type and Direction Of The Lunar Crust Magnetizationmentioning

confidence: 97%

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

et al. 2010

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“…First, they can partially or completely erase the pre-shock remanent magnetization (e.g., Cisowski et al 1975;Cisowski and Fuller 1978;Gilder et al 2006;Bezaeva et al 2007). In the presence of an ambient field, they can lead to the acquisition of shock remanent magnetization (e.g., Doell et al 1970;Wasilewski 1973;Pohl et al 1975;Cisowski et al 1975Cisowski et al , 1976Cisowski and Fuller 1978;Pohl and Eckstaller 1981;Gattacceca et al 2008a;). Finally, above 5-10 GPa, shocks (and even quasistatic pressure) can also permanently modify the intrinsic magnetic properties of rocks, including saturation remanent magnetization, coercivity, susceptibility, and anisotropy of susceptibility and remanence (Pohl and Eckstaller 1981;Fig.…”

Section: Shockmentioning

confidence: 99%

“…It is now clear that shock remanent magnetization is usually acquired parallel to the ambient field at the time of shock with an intensity proportional to this ambient field (Pohl et al 1975;Gattacceca et al 2008a), making it a good recorder of the paleomagnetic field at the time of the last major impact. The main remaining difficulty is that the ambient field at the time of impact may be transiently produced (Crawford and Schultz 1988, 1999Srnka 1977;Doell et al 1970) or amplified (Hide 1972;Hood 1987;Hood and Artemieva 2008) by the impact itself, therefore making the interpretation of SRM in meteorites a complex topic.…”

Section: Shockmentioning

confidence: 99%

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

et al. 2009

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The large-scale compositional structures of planets are primarily established during early global differentiation. Advances in analytical geochemistry, the increasing diversity of extraterrestrial samples, and new paleomagnetic data are driving major changes in our understanding of the nature and timing of these early melting processes. In particular, paleomagnetic studies of chondritic and small-body achondritic meteorites have revealed a diversity of magnetic field records. New, more sensitive and highly automated paleomagnetic instrumentation and an improved understanding of meteorite magnetic properties and the effects of shock, weathering, and other secondary processes are permitting primary and secondary magnetization components to be distinguished with increasing confidence. New constraints on the post-accretional histories of meteorite parent bodies now suggest that, contrary to early expectations, few if any meteorites have been definitively shown to retain records of early solar and protoplanetary nebula magnetic fields. However, recent studies of pristine samples coupled with new theoretical insights into the possibility of dynamo generation on small bodies indicate that some meteorites retain records of internally generated fields. These results indicate that some planetesimals formed metallic cores and early dynamos within just a few million years of solar system formation.

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“…In this 1.88 km diameter crater, shocked ejecta blocks exhibit a slightly elevated coercivity. No evidence of shock remanent magnetization (Gattacceca et al 2008), shock demagnetization, or transient, plasma-related processes, such as have been suggested around larger impact structure, was identified.…”

Section: Impactsmentioning

confidence: 84%

Mapping and Interpretation of the Lithospheric Magnetic Field

Purucker

Clark

2010

Geomagnetic Observations and Models

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We review some of the controversial and exciting interpretations of the magnetic field of the earth's lithosphere occurring in the four year period ending with the IAGA meeting in Sopron in 2009. This period corresponds to the end of the Decade of Geopotential Research, an international effort to promote and coordinate a continuous monitoring of geopotential field variability in the near-Earth environment. One of the products of this effort has been the World Digital Magnetic Anomaly Map, the first edition of which was released in 2007. A second, improved, edition is planned for 2011. Interpretations of the lithospheric magnetic field that bear on impacts, tectonics, resource exploration, and lower crustal processes are reviewed. Future interpretations of the lithospheric field will be enhanced through a better understanding of the processes that create, destroy, and alter magnetic minerals, and via routine measurements of the magnetic field gradient. IntroductionThe magnetic field originating in the earth's lithosphere is part of the earth's magnetic field complex, a dynamic system (Friis-Christensen et al. 2009) dominated by the interaction of the earth's magnetic field dynamo with that of the sun's. The lithospheric field M.E. Purucker ( ) Raytheon at Planetary Geodynamics Lab, Goddard Space Flight Center, Code 698, Greenbelt, MD 20771, USA e-mail: michael.e.purucker@nasa.gov is dominated by static (on a human time scale) contributions that typically represents less than 1% of the overall magnitude of the magnetic field complex, and originate from rocks in the crust and locally, the uppermost mantle. Interpretation of the lithospheric magnetic field is used in (1) structural geology and geologic mapping, and extrapolation of surface observations of composition and structure, (2) resource exploration and 3) plate tectonic reconstructions and geodynamics.This article is designed as a review describing recent progress in mapping and interpreting the lithospheric magnetic field, and also includes some highlights from the 2009 IAGA meeting in Sopron, Hungary. Since IAGA meets every four years, we have designed this review to highlight progress in the four year period from 2005 through 2009, although references to earlier important works are not neglected, especially in the area of resource exploration. Several reviews bearing on the mapping and interpretation of the lithospheric magnetic field have appeared between 2005 and 2009. Review articles within books and encyclopedias have included those within the Encyclopedia of Geomagnetism and Paleomagnetism (Gubbins and

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On the efficiency of shock magnetization processes

Abstract: International audienc

Cited by 48 publications

References 24 publications

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

Mapping and Interpretation of the Lithospheric Magnetic Field

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