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The Eighth International Conference on Mars

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The Eighth International Conference on Mars July 14-18, 2014 Pasadena, California The Eighth International Conference on Mars Synthesis Presentations and Discussions Chair: Lisa Pratt (Indiana University) Geology: Phil Christensen (Arizona State University) Climate: Rich Zurek (NASA Mars Program Office, JPL/Caltech) Life: Dave Des Marais (Ames Research Center) Future Exploration: Marcello Coradini (European Space Agency) Emergence of Mars System Science Shared Odd Vocabulary: Remnant magnetic field Black Beauty Ultramafic serpentinization Mineral deliquescence Late Noachian icy highlands Transient Hesperian water Perchlorates Gray-scale habitability RSL (do not attempt to say words) Swiss-cheese pit cycle Katabatic jumps in troughs Detached dust layers Rosetta-Stone Images Bibring’s mineral timescale Laskar’s obliquity cycles Pratt, 8th Mars Conference Memorable Quotes . Modern Mars should be much easier to understand than ancient Mars . A balancing act between a variety of processes which can be easily swayed (inclination) . Explanations for present-day Mars are the key to understanding past processes on Mars . Much is known, less is understood . Hopefully, by 9th Mars we will have it all solved Pratt, 8th Mars Conference Reflections on the State of Mars Geology Phil Christensen Mike Kraft Mark Salvatore Arizona State University Kristen Bennett Arizona State University Lonia Friedlander Stony Brook University Rebecca Greenberger Brown University Where We Were in 2008 – MEPAG Goals • A. Determine the nature and evolution of the geologic processes that have created and modified the Martian crust – Determine the formation and modification processes of the major geologic units and surface regolith as reflected in their primary and alteration mineralogies. – Evaluate volcanic, fluvial/lacustrine, hydrothermal, and polar erosion and sedimentation processes. – Constrain the absolute ages of major crustal geologic processes. – Hydrothermal environments. – Evaluate igneous processes and their evolution through time. – Characterize surface-atmosphere interactions on Mars. – Determine the tectonic history and large-scale vertical and horizontal structure of the crust. – Determine the present state, 3-dimensional distribution, and cycling of water on Mars. – Determine the nature of crustal magnetization and its origin. – Evaluate the effect of large-scale impacts on the evolution of the Martian crust. • B. Characterize the structure, composition, dynamics, and evolution of Mars’ interior – Characterize the structure and dynamics of the interior. – Determine the origin and history of the magnetic field. – Determine the chemical and thermal evolution of the planet. Christensen, 8th Mars Conference Advances • Mineralogic diversity and distribution • Knowledge of current water inventory • Real-time observations of modern, dynamic Mars • Climate cycling: Snow, ice, liquid water, dust, CO2, S… • Observations of multiple sites at “field geologist” scale • Potential variations in early volcanic processes • Interior processes connect to surface processes • Growing awareness of the impact of impacts • New techniques, integration of multiple data sets, and cross- disciplinary studies Christensen, 8th Mars Conference Key Questions Overarching question: Time • Water: activity, state, duration…? • Is there a martian rock cycle? And where are we in it? • What is the role of wind? Large impacts? • What is the petrologic context of key mineral detections? • Amorphous materials: How do they form? What do they mean? • Nature of early volcanism – Explosive? Friable ash deposits? • What were the processes of the pre-Noachian? • How does Uniformitarianism apply to Mars? – To what degree do currently active processes explain the past? Christensen, 8th Mars Conference Going Forward • Mineral assemblages: era of mineralogy to era of petrology – Geochemistry, context, and textures – Currently explaining what we can measure » “Lost key” model of mineralogic interpretation » But we’ve only lit up part of the street • We know liquid water interacted with rock – but: • How warm? How wet? How long? How much? How come? Where? • Test competing hypotheses – Fully utilize and integrate data sets • Fill the gap between global and “outcrop” mapping • Appreciate the potential for spatial variability • Global phenomena… regional consequences… local effects • Continue to use geology as ground truth for climate and interior evolution models Christensen, 8th Mars Conference Climate Richard Zurek JPL-Caltech Todd Mooring Princeton University Scott Guzewich GSFC Michael Chaffin University of Colorado Nature of the Early Massive Atmosphere Draw-down of the early, more massive atmosphere: – When did it happen and how fast? – How long was water on/near the surface, &where did it go? • Atmospheric Characterization: – Warm/Wet early Mars is not an option if Solar luminosity was 75% of present value.* Do we really need rain? – Intermittently Warm/Wet may still be in play, but requires exceptional combinations (e.g., maybe trace gases + obliquity extremes). – Cool/Wet looks possible, but lots of details to be worked out. Models appear capable of simulating spatially varying deposition of snow/ice—the question is how does this get turned into liquid and produce the needed compositional alteration? • Looks like the water budget (sources ~ sinks) still has missing components. Need a better understanding of escape processes (go MAVEN!). • Major Progress: At 7th Mars, aqueous minerals indicated water was present (follow the water). Since then, the diversity of minerals detected points to different environmental regimes (T, water, pH, time). Need better spatial/temporal constraints. E.g., was there really more water activity in the late Noachian or has evidence of earlier activity been partially erased? *Vigorously contested during discussion period Zurek, 8th Mars Conference Circulation and Transport Dictated by Astronomical Cycles – Dust and water cycles at different obliquities, eccentricities & seasonal phasing – Changing water, dust, and atmospheric gas inventories • Major Progress: We can now see the record of the polar layered terrains. Radar has revealed the inner structure of the polar caps. In the young (<10 Myr) NPLD there are regular patterns (layer packets) that appear to reflect obliquity cycles. Need to connect cause and effect for the NPLD in a more quantitative way. Need to understand the longer record of the SPLD and put it in context with the north. – Polar troughs: Story seems well in hand—major confirmation of early ideas both qualitatively and semi-quantitatively. • Major Find: CO2 ice buried in the (south) polar caps – Some ideas about how to do this and what it could mean if released back into the atmosphere. Need to pursue and test these ideas. • Major Progress: Buried ice/snow—we know it’s there in some places. How extensive, how deep? Where are the shallow ice boundaries in latitude, south as well as north? • Are there implications here for the Noachian & Hesperian, as well as Amazonian periods? Zurek, 8th Mars Conference Modern Mars: Still Changing Today • Major Progress: Continued observations show a dynamic planet, still changing today, with significant interannual variability (dust storms, CO2 polar ice, etc.) and more: – 8 Mars years of Temperature, column dust and water vapor – RSL (see below) – Seasonal CO2 acting to form/enhance high latitude gullies – Sand dune migration and associated erosion. – Need to extend the observation period • Major Progress: Observations now show the vertical structure of dust, of temperature (tides), and of water vapor and ice. Getting these right is vital to getting the circulation and transport right. Need better vertical resolution near the surface. Need to get independent measurements of T/water and of dust. • Major Course Correction: Clouds (and cloud physics) have to be taken into account. • Major Discovery: RSL suggest generation of liquid water (brines) today over a surprisingly large number of places on Mars. What are these, really? How do we test this hypothesis? Zurek, 8th Mars Conference Tools • GCMs = Global Climate Models – Major Progress: • Vertical/spatial resolution much higher than a decade ago • Transport schemes; interactive processes (e.g., radiatively active dust); photochemical • Parameterizations of key processes: exchanges with surface, cloud physics, photochemistry – More Progress Needed • Better spatial resolution • Better physics • More validation => More observations and different observations (e.g., winds) Gaps • Electrical environment • Photochemical system (TGO will help) – Still issues with oxidation states (and not just of the atmosphere) and basic photochemistry (why is the atmosphere still CO2?) • Instruments Zurek, 8th Mars Conference 8th Intl. Conf. on Mars Life Synthesis Presentation David J. Des Marais Ames Research Center Jennifer Buz Scott Perl California Institute of Technology JPL and USC Caroline Freissenet Marek Slipski Goddard Spaceflight Center University of Colorado Rebecca Mickol Svetlana Shkolyar University of Arkansas Arizona State University solubility demand supply extremes solutes impose costs Des Marais, 8th Mars Conference Important Findings Since 7th Mars • Water – Extensive ancient networks & lakes – precipitation – Aqueous minerals in diverse settings – Transient events affecting abundance throughout history • Ingredients for life – Readily available, even trace nutrients – Local enrichments in key elements (e.g., P, Mn, Zn) – Organics found by SAM • Energy – Ancient wet, sunlit environments were not rare
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