Magmatic intrusions and deglaciation at mid-latitude in the northern plains of Mars

Michaut, Chloé; Baratoux, D.; Thorey, C.

doi:10.1016/j.icarus.2013.04.015

Cited by 14 publications

(15 citation statements)

References 52 publications

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“…Indeed, the crater depth of normal craters increases with increasing diameter and craters in the maria are on average shallower than in the highlands or SPA (Fig. 9) (Pike, 1974(Pike, , 1980Kalynn et al, 2013). Nevertheless, the variability in the degradation state of each crater results in an important variance in the crater depth with diameter with respect to the mean trend.…”

Section: Intrusion Thicknessmentioning

confidence: 96%

“…We consider only complex craters and thus use a minimum crater diameter of 20 km, which is the transitional crater diameter between simple and complex lunar craters (Pike, 1974(Pike, , 1980. We use a maximum crater diameter of 180 km, because for larger craters, the mantle uplift associated with basin formation becomes apparent in the gravity data .…”

Section: Normal and Floor-fractured Crater Populationsmentioning

confidence: 99%

“…Given the observed crater depth, the problem is to estimate the original crater depth before the intrusion formed. In the study of Jozwiak et al (2012), the scaling law which gives the depth d c as a function of the crater diameter D, derived by Pike (1974), was used as an estimate for the initial crater depth. However, this scaling law was calculated using only recent, Erastosthenian, and well preserved craters, and it is generally acknowledged that floorfractured craters are generally older and more degraded than this population.…”

Section: Intrusion Thicknessmentioning

confidence: 99%

“…To characterize the mean trend of normal craters, we make use of a linear least-squares regression in log-log space to obtain a power law relationship of the form d c = A D B (Pike, 1974;Kalynn et al, 2013). We use the same method to characterize the mean dependence of floor-fractured crater depth with crater diameter.…”

Section: Intrusion Thicknessmentioning

confidence: 99%

See 3 more Smart Citations

Gravitational signatures of lunar floor-fractured craters

Thorey

Michaut

Wieczorek

2015

Earth and Planetary Science Letters

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Section: Intrusion Thicknessmentioning

confidence: 96%

Section: Normal and Floor-fractured Crater Populationsmentioning

confidence: 99%

Section: Intrusion Thicknessmentioning

confidence: 99%

Section: Intrusion Thicknessmentioning

confidence: 99%

See 2 more Smart Citations

Gravitational signatures of lunar floor-fractured craters

Thorey

Michaut

Wieczorek

2015

Earth and Planetary Science Letters

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“…In the cases without outflow, the water either drained back to the subsurface, leaving the cracks but not the bulge, or froze, resulting in both the cracks and bulge still being there. Magmatic features such as sills [43] could produce the same morphology and trigger the outflow of groundwater. However, a subsurface aqueous reservoir could explain the extreme high discharges for large outflow channels [41].…”

Section: Discussionmentioning

confidence: 99%

Pressurized groundwater systems in Lunae and Ophir Plana (Mars): Insights from small-scale morphology and experiments

Marra

Hauber

Jong

et al. 2015

GeoResJ

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a b s t r a c tOutflow channels on Mars reveal the past presence of water, possibly released from pressurized groundwater reservoirs. We aim to improve our understanding of such outflow systems in order to better constrain past hydrological conditions on Mars. We investigate the morphology of possible pressurized groundwater outflow systems on Mars and compare them to landscape evolution experiments. These experiments show that incised channels, like the classic outflow channels, form in a last, erosional, stage in morphological development. This is preceded by the formation of sedimentary lobes due to rapid water loss by infiltration. On Mars, we observe similar morphologies related to different stages of groundwater outflow in Lunae and Ophir Plana. In the experiments, pits formed by the pressure of the groundwater, whereas the pits in the source regions of the outflow channels relate to the regional tectonic structure and are not formed by groundwater alone. Faulting, subsidence and collapse likely triggered outflow from a pressurized aquifer. This scenario is consistent with the presence of one or several cryosphere-confined aquifers from the Early Hesperian to at least the middle Amazonian. A pronounced spatial trend of larger and further developed outflow systems at lower elevations suggests that features ranging from small lobes to large outflow channels were sourced from a common aquifer or from aquifers with similar pressures. The required cryosphere indicates a cold climate and enables groundwater outflow even under atmospheric conditions unfavorable for sustained presence of liquid water.

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A model for the dynamics of crater‐centered intrusion: Application to lunar floor‐fractured craters

Thorey

Michaut

2014

JGR Planets

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Lunar floor-fractured craters are a class of craters modified by post-impact mechanisms. They are defined by distinctive shallow floors that are convex or plate-like, sometimes with a wide floor moat bordering the wall region. Radial, concentric, and polygonal floor fractures suggest an endogenous process of modification. Two mechanisms have been proposed to account for such deformations: viscous relaxation and spreading of a magma intrusion at depth below the crater. To test the second assumption and bring more constraints on the intrusion process, we develop a model for the dynamics of magma spreading below an elastic overlying layer with a crater-like topography. As predicted in earlier more qualitative studies, the increase in lithostatic pressure at the crater wall zone prevents the intrusion from spreading laterally, leading to the thickening of the intrusion. Additionally, our model shows that the final crater floor appearance after the uplift, which can be convex or flat, with or without a circular moat bordering the wall zone, depends on the elastic thickness of the layer overlying the intrusion and on the crater size. Our model provides a simple formula to derive the elastic thickness of the overlying layer hence a minimum estimate for the intrusion depth. Finally, our model suggests that crust redistribution by cratering must have controlled magma ascent below most of these craters.

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Magmatic intrusions and deglaciation at mid-latitude in the northern plains of Mars

Cited by 14 publications

References 52 publications

Gravitational signatures of lunar floor-fractured craters

Gravitational signatures of lunar floor-fractured craters

Pressurized groundwater systems in Lunae and Ophir Plana (Mars): Insights from small-scale morphology and experiments

A model for the dynamics of crater‐centered intrusion: Application to lunar floor‐fractured craters

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