Pressure demagnetization of the Martian crust: Ground truth from SNC meteorites

Bezaeva, N. S.; Rochette, P.; Gattacceca, J.; Садыков, Р. А.; Trukhin, V. I.

doi:10.1029/2007gl031501

Cited by 28 publications

(33 citation statements)

References 19 publications

(33 reference statements)

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“…For example, the demagnetization radius of the Isidis impact is consistent with an impact energy of ~4 × 10 26 J if the magnetic mineral has a high β value (i.e., is easily demagnetized like multidomain magnetite) [ Borradaile and Jackson , ], whereas it would require ~10 times more energy if the mineral has a much lower value of β , i.e., more difficult to demagnetize, like pseudo‐single domain magnetite [ Bezaeva et al ., ]. To explain the demagnetization at Hellas or Utopia, the multiple large re‐impacting ejecta fragments make interpretation more difficult.…”

Section: Resultsmentioning

confidence: 99%

Demagnetization by basin‐forming impacts on early Mars: Contributions from shock, heat, and excavation

2013

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[1] Large hypervelocity impacts occurred frequently on ancient Mars, leaving many large impact basins visible today. After the planetary dynamo ceased operating, such impacts demagnetized the crust by way of (1) excavation of magnetized material, (2) heating, and (3) shock pressure. We investigate these three demagnetizing processes, both separately and in combination, using hydrocode simulations of large impacts on early Mars at a range of impact energies and using a new parameterization of the shock pressure-demagnetization behavior of candidate Martian minerals. We find that in general, shock pressure demagnetization is more important than thermal demagnetization, except in the combined case of very large impacts (more than~10 26 J) and low Curie temperature minerals such as pyrrhotite. We find that total demagnetized area has a power law dependence on impact energy (with an exponent of 0.6-0.72) and that depending on the magnetic mineral, the demagnetized area resulting for a given impact energy can vary over approximately an order of magnitude. We develop an empirical model that can be used to calculate total demagnetized area for a given impact energy and magnetic mineral (whose pressure-demagnetization properties are known). Once a reliable basin scaling law for ancient Mars (i.e., relating impact energy to final basin topography) is derived, this mineral parameterization and empirical model will allow robust constraints to be placed upon the primary Martian magnetic carrier(s).Citation: Lillis, R. J., S. T. Stewart, and M. Manga (2013), Demagnetization by basin-forming impacts on early Mars: Contributions from shock, heat, and excavation,

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Section: Resultsmentioning

confidence: 99%

Demagnetization by basin‐forming impacts on early Mars: Contributions from shock, heat, and excavation

2013

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“…These experiments have already been partially published 21 and have implications in rock magnetism, geophysics, and planetology. These experiments have already been partially published 21 and have implications in rock magnetism, geophysics, and planetology.…”

Section: Discussionmentioning

confidence: 96%

Nonmagnetic high pressure cell for magnetic remanence measurements up to 1.5 GPa in a superconducting quantum interference device magnetometer

Садыков

Bezaeva

Kharkovskiy

et al. 2008

Review of Scientific Instruments

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We describe here a compact nonmagnetic composite high pressure cell of piston-cylinder type with inner diameter of 6 mm equipped with manganin pressure sensor. This cell was developed for room temperature measurements of magnetic remanence of relatively large rock samples (up to 5.8 mm in diameter and 15 mm long cylinders) under hydrostatic pressure up to 1.5 GPa (the operating pressure limit) in the 2G Enterprises superconducting quantum interference device magnetometer. Its design was focused on minimizing the remanent magnetic moment m(r) of the cell (m(r)=3 x 10(-8) A m(2)) that allowed direct measurements of remanent magnetic moment M(r) under pressure for weakly magnetic materials-rock samples (M(r) epsilon[5 x 10(-7),10(-4)] A m(2)). The inner part of this composite cell is made of hard "Russian alloy" (Ni(57)Cr(40)Al(3)) whereas the envelope of the cell corps is made of less magnetic titanium alloy. This design solution permitted to reduce the total remanent magnetic moment of the whole cell and represents the main device feature. We describe here the choice of materials for pressure cell based on their magnetic and mechanical properties, the choice of the pressure transmitting medium (polyethilsiloxane liquid) providing perfectly hydrostatic conditions for the sample as well as the cell geometry. The cell performance is illustrated by results of pressure demagnetization experiments on rocks and minerals.

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“…Such pressure increases, resulting in a 50 K increase of T M , will result in a farther 5 to 8 km of crust to temporarily pass below the Morin transition (note that we neglect the shock wave temperature increase generated; at 2 GPa this increase is of a few Kelvins only [e.g., Stöffler et al ., ]). This results in an additional demagnetization, with respect to the usually considered pressure demagnetization effect [ Bezaeva et al, , ]. In case this situation occurs in the presence of an ambient field a remagnetization linked to cycling through T M may also occur.…”

Section: Discussionmentioning

confidence: 99%

The effect of hydrostatic pressure up to 1.61 GPa on the Morin transition of hematite‐bearing rocks: Implications for planetary crustal magnetization

Bezaeva

Demory

Rochette

et al. 2015

Geophysical Research Letters

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We present new experimental data on the dependence of the Morin transition temperature (TM) on hydrostatic pressure up to 1.61 GPa, obtained on a well‐characterized multidomain hematite‐bearing sample from a banded iron formation. We used a nonmagnetic high‐pressure cell for pressure application and a Superconducting Quantum Interference Device magnetometer to measure the isothermal remanent magnetization (IRM) under pressure on warming from 243 K to room temperature (T0). IRM imparted at T0 under pressure in 270 mT magnetic field (IRM270mT) is not recovered after a cooling‐warming cycle. Memory effect under pressure was quantified as IRM recovery decrease of 10%/GPa. TM, determined on warming, reaches T0 under hydrostatic pressure 1.38–1.61 GPa. The pressure dependence of TM up to 1.61 GPa is positive and essentially linear with a slope dTM/dP = (25 ± 2) K/GPa. This estimate is more precise than previous ones and allows quantifying the effect of a pressure wave on the upper crust magnetization, with special emphasis on Mars.

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Pressure demagnetization of the Martian crust: Ground truth from SNC meteorites

Cited by 28 publications

References 19 publications

Demagnetization by basin‐forming impacts on early Mars: Contributions from shock, heat, and excavation

Demagnetization by basin‐forming impacts on early Mars: Contributions from shock, heat, and excavation

Nonmagnetic high pressure cell for magnetic remanence measurements up to 1.5 GPa in a superconducting quantum interference device magnetometer

The effect of hydrostatic pressure up to 1.61 GPa on the Morin transition of hematite‐bearing rocks: Implications for planetary crustal magnetization

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