38 Antarctic Dry Valleys:
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1 38 Antarctic Dry Valleys: 1. The Antarctic environment and the Antarctic Dry Valleys. 2. Cold-based glaciers and their contrast with wet-based glaciers. 3. Microclimate zones in the Antarctic Dry Valleys (ADV) and their implications. 4. Landforms on Earth and Mars: A comparative analysis of analogs. 5. Biological activity in cold-polar deserts. 6. Problems in Antarctic Geoscience and their application to Mars.
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5 The Dry Valleys: A Hyper-Arid Cold Polar Desert
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7 Temperate Wet-Based Glaciers
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9 Cold-Based Glaciers
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14 Antarctic Dry Valleys: Morphological Zonation, Variable Geomorphic Processes, and Implications for Assessing Climate Change on Mars
15 Antarctic Dry Valleys 4000 km 2 ; Mountain topography (2800 m relief). Coldest, driest desert on Earth. Mean annual temperature: -20 o C. Mean annual snowfall (CWV): Min. = <0.6 cm; Max. = 10 cm. Fate of snow: Sublimate or melt. A hyperarid cold polar desert. Topography controls katabatic wind flow: Funneled through valleys, warmed by adiabatic compression. Enhances surface temperatures, increases sublimation rates of ice and snow. Bedrock topography governs local distribution of snow and ice: Biology sparse: ~1 mm Antarctic mite ; microscopic nematodes. Environment very useful for understanding Mars climate change.
16 Antarctic Dry Valleys 4000 km 2 ; Mountain topography (2800 m relief). Coldest and driest desert on Earth. Mean annual temperature: -20 o C. Mean annual snowfall (CWV): Minimum = <0.6 cm; Maximum = 10 cm. Fate of snow: Sublimate or melt. Generally a hyperarid cold polar desert. Topography controls katabatic wind flow: Funneled through valleys, warmed by adiabatic compression. Enhance surface temperatures, increase sublimation rates of ice and snow. Bedrock topography governs local distribution of snow and ice: Biology sparse: ~1 mm-sized Antarctic mite ; microscopic nematodes. Environment very useful for understanding Mars climate change.
17 Antarctic Dry Valleys Hyperarid cold polar desert. But, significant variations within this climate. These variations involve small but important differences: Annual surface temperature (meltwater). Relative humidity. Soil moisture (and type of subsurface ice). We have defined three different microclimate zones within the Antarctic Dry Valleys. These are useful for understanding Mars climate change.
18 Upland frozen zone Microclimate Zones Coastal thaw zone Inland mixed zone
19 Distribution of surface meltwater No traditional active layer No seregation ice Regions with soil moisture < 3% Discontinuous A. L. Ice and sand wedges Soil moisture variable Dynamic Active Layer with segregation ice and wedges Soil moisture ~ 30 to > 50% < -30 C to -35 C Upland Frozen Zone -20 C to -27 C Inland Mixed Zone -14 C Origins of subsurface ice? Coastal Zone
20 Distribution of surface meltwater No traditional active layer No segregation ice soil moisture <3% Discontinuous A. L. sand wedges Soil moisture variable Dynamic active layer with segregation ice and wedges Soil moisture ~30 to >50% -8 C (<-30 C) Upland frozen zone -4 C (-22 C) Inland mixed zone -2 C (-14 C) Coastal thaw zone
21 POLYGONS Upland frozen zone Inland mixed zone Coastal thaw zone Sublimation Sand-wedge Ice wedge
22 A. J. Johnsson and E. M. Kakkinen, Earth Sciences Centre, Gothenburg Sweden
23 Viscous-flow features Upland frozen zone Inland mixed zone Coastal thaw zone Debris-covered glaciers Gelifluction lobes Solifluction lobes
24 Applications to Mars Debris covered glaciers as analogs for viscous flow features on interior of Crater walls Crater wall 248 W/ 36 S M04/ E / 78 S Crater wall 247 W / 38 S M18/00898
25 Mullins Debris-Covered Glacier, Beacon Valley, Antarctica
26 Origin of debris-covered glaciers in upland zone Protective lag of sublimation till
27 Fate of debris-covered glacier ice?
28 Sublimation Polygons
29 POLYGON AGE: in-situ ashfall
30 LU1017/EMS 98 13A/pkt. W J = Grains Ar40/Ar39 Ar38/Ar39 Ar37/Ar39 Ar36/Ar39 Ar39 (moles) % Ar40* Ar40*/Ar39K Age (Ma) Error (Ma) E E E E E E
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33 Applications to Mars Sublimation polygons as an analog for basketball-textured terrain on Mars
34 A. J. Johnsson and E. M. Kakkinen, Earth Sciences Centre, Gothenburg Sweden
35 Applications to Mars Debris covered glaciers as analogs for viscous flow features on interior of Crater walls Crater wall 248 W/ 36 S M04/ E / 78 S Crater wall 247 W / 38 S M18/00898
36 OBLIQUITY VARIATIONS AND CLIMATE CHANGE ON MARS
37 History of Climate Change of Mars: Superposed Geomorphological Climate Indicators
38 Rock Weathering In Antarctica and Mars Antarctica Antarctica Mars Mars
39 Key Issues in Antarctic Dry Valley Geoscience Age of landscapes, surfaces and weathering rates. Modes of rock weathering and soil formation. Stability of microclimate zones; effects of global warming. Debris-covered alpine glaciers: Formation and evolution. Sublimation till: Modes of formation and evolution. Role of sublimation till in inhibiting vapor diffusion, ice loss. Age of ancient ice in subsurface: Oldest ice on Earth? Analysis of ancient climate record in buried ice. Polygon origin and evolution. Implications for Antarctic and global climate change. Provide clues to map changing climate on Mars. Exobiological studies on Earth, application to Mars.
40 Sampling for life detection in extreme environments: Antarctic Dry Valleys Buried ice ancient microbial communities: Paul Falkowski and Kay Bidle, Rutgers. Lipid biomarkers and isotopic ratios from soil profiles: Yongsong Huang, Brown University. Amino Acid Racemization (AAR): Alexander Tsapin (JPL) Molecular biological and Limulus Amebocyte Lyste (LAL) Analyses: Rebecca Gast, WHOI. Ribosomal RNA: Linda Amaral Zettler, MBL.
41 The Dry Valleys: A Hyper-Arid Cold Polar Desert
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