Ephemeral liquid water at the surface of the martian North Polar Residual Cap: Results of numerical modelling

Łosiak, A.; Czechowski, Leszek; Velbel, M. A.

doi:10.1016/j.icarus.2015.08.025

Cited by 13 publications

(11 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Indeed, large regions of sulfate-rich material have been detected on and around the modern north polar region of Mars and there is evidence that the material is derived from the polar sediments themselves 27 . It has been shown that even in the polar regions, conditions could be warm enough to melt pure water ice around dark dust grains on steep equatorial facing slopes in the polar region 28 . Our experiments demonstrate that weathering occurs at even much lower temperatures than the 273 K, and therefore if H 2 SO 4 aerosols are present we expect weathering to occur over an even larger area and for longer portions of the day.…”

Section: Discussionmentioning

confidence: 99%

Elevated olivine weathering rates and sulfate formation at cryogenic temperatures on Mars

et al. 2017

View full text Add to dashboard Cite

Large Hesperian-aged (~3.7 Ga) layered deposits of sulfate-rich sediments in the equatorial regions of Mars have been suggested to be evidence for ephemeral playa environments. But early Mars may not have been warm enough to support conditions similar to what occurs in arid environments on Earth. Instead cold, icy environments may have been widespread. Under cryogenic conditions sulfate formation might be blocked, since kinetics of silicate weathering are typically strongly retarded at temperatures well below 0 °C. But cryo-concentration of acidic solutions may counteract the slow kinetics. Here we show that cryo-concentrated acidic brines rapidly chemically weather olivine minerals and form sulfate minerals at temperatures as low as −60 °C. These experimental results demonstrate the viability of sulfate formation under current Martian conditions, even in the polar regions. An ice-hosted sedimentation and weathering model may provide a compelling description of the origin of large Hesperian-aged layered sulfate deposits on Mars.

show abstract

Section: Discussionmentioning

confidence: 99%

Elevated olivine weathering rates and sulfate formation at cryogenic temperatures on Mars

et al. 2017

View full text Add to dashboard Cite

show abstract

“…melting and solidification-see, e.g. Losiak et al 2015). The dependence of k is important in any case if k changes substantially (e.g.…”

Section: The Effects Of Non-linearity Of the Equationmentioning

confidence: 99%

Crustal lithology vs. thermal state and Moho heat flow across the NE part of the European Variscan orogen: a case study from SW Poland

Puziewicz

Czechowski

Grad

et al. 2019

Int J Earth Sci (Geol Rundsch)

Self Cite

View full text Add to dashboard Cite

Geotherms of four crustal profiles across the Variscan orogen in SW Poland have been constructed to better understand the variation in thermal state of the region. Seismic and drilling data as well as rock sequences in exposed parts of the orogen were used for Wilcza Góra (Sudetic Block), Polkowice-Rudna (Middle Odra Horst), Święciechowa (Wolsztyn-Leszno Horst) and Września (Szczecin-Miechów Synclinorium within TESZ) profiles. The palaeoclimate-corrected surface heat flow map and the heat-production calculations based on literature data enabled the construction of geotherms and estimation of Moho heat flow. Exception is the Polkowice-Rudna profile, where the surface heat flow was calculated using temperature measurements in underground copper mines, and K, U and Th contents and density/heat conductivity measurements in rocks drilled in the Middle Odra Horst were used to calculate geotherm. The basaltic lava migration through the lithospheric mantle and its effect on crustal geotherm in Wilcza Góra (area of Cenozoic alkaline volcanism at ca. 30-18 Ma) was shown to increase slightly both current surface and current Moho heat flow (by ca. 4 mW/m 2). The presented approach couples geological and geophysical information and thus differs from standard purely geophysical assessment of lithosphere thermal state. It shows that surface heat flow is enlarged to 84 mW/m 2 by granitic plutons in the upper crust in the Lubin-Polkowice site. Heat flow on the Moho varies from 28 to 34 mW/m 2 in sites located in the Sudetic-/Fore-Sudetic Blocks, Middle Odra Horst and Wolsztyn-Leszno Horst. Locally it may slightly increase because of extraneous heat input by Cenozoic basaltic volcanism, but the values close to 30 mW/m 2 are specific for mantle root of Saxothuringian Zone in SW Poland. Mantle heat flow is 36 mW/m 2 in Września site and supposedly is a manifestation of different nature of lithospheric mantle underlying TESZ.

show abstract

“…is the coefficient of thermal conductivity (it may depend on the temperature, pressure and composition), and Q [W m -3 ] is the heat generation per unit volume. Nonlinear effects are included in the similar way to that used in Czechowski (2014), Puziewicz et al (2012), and Losiak et al (2015). The thickness of considered layer is D=120 km.…”

Section: Equations and Methodsmentioning

confidence: 99%

Isostasy, LAB and some properties of asthenosphere in chosen regions of Poland

Czechowski¹

2019

Preprint

Self Cite

View full text Add to dashboard Cite

We use programs from the package LABWA2015 to determine position of Lithosphere-Asthenosphere Boundary (LAB) and some properties of lower lithosphere in chosen sites in Poland. Seismic, topographic, thermal and petrological data are used together with assumption about isostasy. Moreover we investigate the role of assumption about the steady state temperature distribution. We have found that sometimes this assumption for continental lithosphere can be unjustified but usually does not lead to significant errors. We have found also that in chosen sites, the thermal LAB is in the depth range 85-95 km. The average value of thermal conductivity of mantle is ~4 W m-1 K-1. Just below MOHO, a level of approximate isostatic compensation is found. More precise compensation is found in the asthenosphere at ~110 km but its position is sensitive to the density distribution.

show abstract

Ephemeral liquid water at the surface of the martian North Polar Residual Cap: Results of numerical modelling

Cited by 13 publications

References 61 publications

Elevated olivine weathering rates and sulfate formation at cryogenic temperatures on Mars

Elevated olivine weathering rates and sulfate formation at cryogenic temperatures on Mars

Crustal lithology vs. thermal state and Moho heat flow across the NE part of the European Variscan orogen: a case study from SW Poland

Isostasy, LAB and some properties of asthenosphere in chosen regions of Poland

Contact Info

Product

Resources

About