Noachian Life 1

Total Page:16

File Type:pdf, Size:1020Kb

Noachian Life 1 1 Noachian Life An Overview of Prevailing Theories, Studies, & Experiments Surrounding Ancient Martian Life By Mike Morgan 2 The Noachian 3 4 Noachian Climate 5 Northern Plains Arabia Shoreline East of Cydonia Mensae 6 Evaporite in Merdiani Outcrop Burns Cliff of Meridiani Outcrop 7 ALH84001 • Igneous Age of 4.091 + or – 0.030 billion years (Noachian) • Carbonate globules may be microscopic fossils of Martian bacteria. – Shown to have formed at 18 degrees celsius – Morphology is not enough. 8 Tissint Meteorite • Recovered almost immediately after impact as well as a thick fusion crust. – Solidified 400 – 500 MYA – Similar carbonate gobules to ALH84001 – Oxygen and Carbon rich disc-shaped structures typically 20 nm in radius. A Dimmer Solar System • Noachian Solar Luminosity 75% that of Today (Gough, 1981) • Contemporary Average Temperature – 60 degrees C ( Ranges from – 125 degrees C to 20 degrees C) • 100 Times Thinner Atmosphere than Earth – 95% CO2 – 10 Degrees • How do we explain the presence of liquid water with lower solar radiation and what are the subsequent effects on climate? 9 10 11 12 Noachian Mars 13 Evidence of Sulfuric Atmosphere • Modeled using Gusev Crater basalt composition and batch melting model. • Soils from landed missions have sulfate abundances of 3 – 10% – “Flat-lying sedimentary rocks rich in sulfur and contain abundant sulfur salts.” (Squyres et al., 2004) • SNC Meteorites – Contain Sulfur – Negative Isotopic Readings Show Sulfur was produced by Atmospheric Chemical Reactions • (Farquhar et al., 2000) 14 15 16 Impacts of Sulfuric Atmosphere on Habitability • Decreases pH of Ocean waters from deposition – Some estimates as low as a pH of 2 -3 based on 3+ presence of Jarosite: KFe 3(OH)6(SO4)2 • Requires a wet, oxidizing, acid environment • Prevents Deposition of Carbonate • Only last 600 Days, warming effect lasts hundreds of years (Wong, 2004). – Is this Enough for Life to Evolve? – Long-lasting intervals of cold, dry conditions 17 Sulfate-Reducing 0 • 2S + 2H2O + SO2 > 2H2SO4 - - - • H2S + 4OH > SO2 + 6H + 8 e • Bacteria in Siberian Permafrost suggests low-level metabolic activity. • Cells persisted under cold conditions for .5 million years. Extremophile 18 19 ERODED NOACHIAN CRATERS 20 Holden Crater Yellowknife Crater • Curiosity Rover • Once contained Ancient lake that could have supported Martian biosphere founded on chemolithautotrophs. – Low Salinity and sediment- transporting water. – Uses inorganic compounds for energy – Sheepbed Mudstone is believed to be sequestered fine sediments over long periods of time. • Nodules, microbial fossils? • 1500 – millions of years 21 A Promising Crater – Nutrients • Carbon • Hydrogen • Sulfur • Nitrogen • Phosphorous – All found in Gale Crater – Plausible Redox Couples • Sulfur and Iron • Inorganic Volatiles • Higher proportion of reduced sulfur relative to oxidized sulfur points to a plausible redox couple for prokaryotic respiration. 22 Sulfate-Reducing 0 • 2S + 2H2O + SO2 > 2H2SO4 - - - • H2S + 4OH > SO2 + 6H + 8 e 23 24 25 Viking Perchlorate Respiration 26 27 Methanogenic Life • Presence of Methane in Martian Atmosphere reflective of Ancient Noachian Life? • Geologic Processes Trapped Methane Produced by Ancient Methanogenic Life Forms, which becomes slowly released overtime. • Consumes Carbon Dioxide and Respires Methane 28 Future Missions 29 30 ExoMars • Curiosity Spectrometer Detected Carotenoid Molecules – Protects from Radiation – Biosignature of past life? • ExoMars will drill 2 meters deep in Noachian Site – Searching for Biomarkers • Urey Instrument – Mars Organic and Oxidant Detector – Grind up samples of Martian Soil. – Determine Current Habitability of Martian Soil. Proposed Experiments 31 Microbes and Basaltic Glass • Basaltic Glass • Hyaloclastites + subaqueous basalts. • Microbes rapidly colonize along the surface’s fractures and racks that are exposed to water after cooling. – This colonization alters and modifies the surface and produces characteristic granular or tubular biolateration textures. – Silicates can help preserve these markings for geologic time scales. – Terrestrial glass bioalteration can extend as far back as 3.5 billion 32 years ago. • Microbes filter in through cracks within water, feeding off carbon, nitrogen, and phosphorous from the glass. • Overtime becomes locked in by mixture of minerals and respired materials. 33 Detecting Past Life • Lipid Biomakers – 2700 million-year-old Shales from Pilbara Craton, Australia (Brocks, 1999) – Lipid Biomakers were found to be preserved, though limited, in acidic lakes through out the Yilgarn Craton of Australia with pH less than 2 (Johnson, 2008) • Resistant biomakers. 34 Concluding Thoughts • Strong Evidence for a Habitable Climate during Noachian. – Questions about stable habitability can be answered by groundwater. • Did Life Persist for Hundreds of Years or Millions? – Is that Enough for Life to Evolve? 35 Noachian Life? 36 References • Brocks, J. J. "Archean Molecular Fossils and the Early Rise of Eukaryotes." Science285.5430 (1999): 1033-036. Print. • Catling, David. "Atmospheric Evolution of Mars." Encyclopedia of Paleoclimatology and Ancient Environments. Ed. Vivien Gornitz. Dordrecht, Netherlands: Springer, 2009. N. pag. Print. • Clifford, Stephen M., and Timothy J. Parker. "The Evolution of the Martian Hydrosphere: Implications for the Fate of a Primordial Ocean and the Current State of the Northern Plains." Icarus 154 (2001): 40-79. Print. • Farquhar, James et al. "Evidence of Atmospheric Sulphur in the Martian Regolith from Sulphur Isotopes in Meteorites." Nature 404 (2000): 50-52. Print. • Izawa, M. R. M., et al. "Basaltic Glass as a Habitat for Microbial Life: Implications for Astrobiology and Planetary Exploration." Planetary and Space Science 58 (2010): 583-91. Print. • Johnson, Sarah Stewart. Mars in the Late Noachian: Evolution of a Habitable Surface Environment. Diss. Massachusetts Institute of Technology, 2008. N.p.: n.p., n.d. Print. References Con’t • Knoll, Andrew H., Michael Carr, Benton Clark, David J. Des Marais, Jack D. Farmer, Woodward W. Fischer, John P. Grotzinger, Scott M. Mclennan, Michael Malin, Christian Schröder, Steven Squyres, Nicholas J. Tosca, and Thomas Wdowiak. "An Astrobiological Perspective on Meridiani Planum." Earth and Planetary Science Letters 240.1 (2005): 179-89. Print. • Lapen, T. J., M. Righter, A. D. Brandon, V. Debaille, B. L. Beard, J. T. Shafer, and A. H. Peslier. "A Younger Age for ALH84001 and Its Geochemical Link to Shergottite Sources in Mars." Science 328.5976 (2010): 347-51. Print. • Logan, Bruce E. et al. "Kinetics of Perchlorate- and Chlorate-Respiring Bacteria." APPLIED AND ENVIRONMENTAL MICROBIOLOGY 67.6 (2001): 2499-506. Print. • Madden, M. E. Elwood, R. J. Bodnar, and J. D. Rimstidt. "Jarosite as an Indicator of Water-limited Chemical Weathering on Mars." Nature 431.7010 (2004): 821-23. Print. • McKay, David, Everett Gibson, and Kathie Thomas-Keprta. "Possible Evidence for Life in ALH84001." Jet Propulsion Labratory (1999): 1-4. Web. • Squyres, S. W. "The Opportunity Rover's Athena Science Investigation at Meridiani Planum, Mars." Science 306.5702 (2004): 1698-703. Print. “Yet so vain is man, and so blinded by his vanity, that no writer, up to the very end of the nineteenth century, expressed any idea that intelligent life might have developed there far, or indeed at all, beyond its earthly level.” - War of the Worlds .
Recommended publications
  • Mars Express Orbiter Radio Science
    MaRS: Mars Express Orbiter Radio Science M. Pätzold1, F.M. Neubauer1, L. Carone1, A. Hagermann1, C. Stanzel1, B. Häusler2, S. Remus2, J. Selle2, D. Hagl2, D.P. Hinson3, R.A. Simpson3, G.L. Tyler3, S.W. Asmar4, W.I. Axford5, T. Hagfors5, J.-P. Barriot6, J.-C. Cerisier7, T. Imamura8, K.-I. Oyama8, P. Janle9, G. Kirchengast10 & V. Dehant11 1Institut für Geophysik und Meteorologie, Universität zu Köln, D-50923 Köln, Germany Email: [email protected] 2Institut für Raumfahrttechnik, Universität der Bundeswehr München, D-85577 Neubiberg, Germany 3Space, Telecommunication and Radio Science Laboratory, Dept. of Electrical Engineering, Stanford University, Stanford, CA 95305, USA 4Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91009, USA 5Max-Planck-Instuitut für Aeronomie, D-37189 Katlenburg-Lindau, Germany 6Observatoire Midi Pyrenees, F-31401 Toulouse, France 7Centre d’etude des Environnements Terrestre et Planetaires (CETP), F-94107 Saint-Maur, France 8Institute of Space & Astronautical Science (ISAS), Sagamihara, Japan 9Institut für Geowissenschaften, Abteilung Geophysik, Universität zu Kiel, D-24118 Kiel, Germany 10Institut für Meteorologie und Geophysik, Karl-Franzens-Universität Graz, A-8010 Graz, Austria 11Observatoire Royal de Belgique, B-1180 Bruxelles, Belgium The Mars Express Orbiter Radio Science (MaRS) experiment will employ radio occultation to (i) sound the neutral martian atmosphere to derive vertical density, pressure and temperature profiles as functions of height to resolutions better than 100 m, (ii) sound
    [Show full text]
  • Planting and Germination of Sweet Potato, Yam and Radish Plants in the Mars Desert Research Station
    Copyright © 2015 by Olenka Jibaja Valderrama. Published by The Mars Society with permission. Planting and Germination of Sweet Potato, Yam and Radish Plants in the Mars Desert Research Station Olenka Jibaja Valderrama Universidad Católica Santo Toribio de Mogrovejo – Chiclayo, Perú [email protected] Abstract: As part of the future exploration of the universe, manned missions to other planets or satellites near Earth will be needed. One of the main objectives of these missions will be to reach Mars because it is at a relatively close distance to our planet and because both planets have some common characteristics. Since the economic investment of these explorations is quite high, the duration of them must be significant; that’s why the missions should aim to be self-sufficient. The search for food sources for crew members is a key factor to be investigated and even more attention should be on food whose production is possible and sustainable in the environment where the mission arises. This work was involved with the planting and germination of radish, yam and sweet potato plants in the greenhouse of the Mars Desert Research Station (MDRS) and the main objective was to investigate the characteristics of growth and development of these plants in Martian conditions to find out whether its production is possible or not. Orange skin and white skin: two types of sweet potatoes were planted. During rotation, it was discovered that yam grew faster under these conditions than the rest of the tubers, although its development was slower as compared to terrestrial conditions. Radish plants in Mars regolith grew in a similar speed than in the fertile Earth soil, and even faster than in drier soil taken from the desert.
    [Show full text]
  • The Reference Mission of the NASA Mars Exploration Study Team
    NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor Science Applications International Corporation Houston, Texas David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 This publication is available from the NASA Center for AeroSpace Information, 800 Elkridge Landing Road, Linthicum Heights, MD 21090-2934 (301) 621-0390. Foreword Mars has long beckoned to humankind interest in this fellow traveler of the solar from its travels high in the night sky. The system, adding impetus for exploration. ancients assumed this rust-red wanderer was Over the past several years studies the god of war and christened it with the have been conducted on various approaches name we still use today. to exploring Earth’s sister planet Mars. Much Early explorers armed with newly has been learned, and each study brings us invented telescopes discovered that this closer to realizing the goal of sending humans planet exhibited seasonal changes in color, to conduct science on the Red Planet and was subjected to dust storms that encircled explore its mysteries. The approach described the globe, and may have even had channels in this publication represents a culmination of that crisscrossed its surface. these efforts but should not be considered the final solution. It is our intent that this Recent explorers, using robotic document serve as a reference from which we surrogates to extend their reach, have can continuously compare and contrast other discovered that Mars is even more complex new innovative approaches to achieve our and fascinating—a planet peppered with long-term goal.
    [Show full text]
  • Variability of Mars' North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data
    Icarus 144, 382–396 (2000) doi:10.1006/icar.1999.6300, available online at http://www.idealibrary.com on Variability of Mars’ North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data Deborah S. Bass Instrumentation and Space Research Division, Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228-0510 E-mail: [email protected] Kenneth E. Herkenhoff U.S. Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona 86001 and David A. Paige Department of Earth and Space Sciences, University of California, Los Angeles, 405 Hilgard Avenue, Los Angeles, California 90095-1567 Received May 15, 1998; revised November 17, 1999 1. INTRODUCTION Previous studies interpreted differences in ice coverage between Mariner 9 and Viking Orbiter observations of Mars’ north residual Like Earth, Mars has perennial ice caps and an active wa- polar cap as evidence of interannual variability of ice deposition on ter cycle. The Viking Orbiter determined that the surface of the the cap. However,these investigators did not consider the possibility northern residual cap is water ice (Kieffer et al. 1976, Farmer that there could be significant changes in the ice coverage within et al. 1976). At the south residual polar cap, both Mariner 9 the northern residual cap over the course of the summer season. and Viking Orbiter observed carbon dioxide ice throughout the Our more comprehensive analysis of Mariner 9 and Viking Orbiter summer. Many have related observed atmospheric water vapor imaging data shows that the appearance of the residual cap does not abundances to seasonal exchange between reservoirs such as show large-scale variance on an interannual basis.
    [Show full text]
  • MARS DURING the PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- Boratory, University of Arizona
    Fourth Conference on Early Mars 2017 (LPI Contrib. No. 2014) 3078.pdf MARS DURING THE PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- boratory, University of Arizona, Tucson, AZ 85721, [email protected], 2Southwest Research Institute and NASA’s SSERVI-ISET team, 1050 Walnut St., Suite 300, Boulder, CO 80302. Introduction: The surface geology of Mars appar- ing the pre-Noachian was ~10% of that during the ently dates back to the beginning of the Early Noachi- LHB. Consideration of the sawtooth-shaped exponen- an, at ~4.1 Ga, leaving ~400 Myr of Mars’ earliest tially declining impact fluxes both in the aftermath of evolution effectively unconstrained [1]. However, an planet formation and during the Late Heavy Bom- enduring record of the earlier pre-Noachian conditions bardment [5] suggests that the impact flux during persists in geophysical and mineralogical data. We use much of the pre-Noachian was even lower than indi- geophysical evidence, primarily in the form of the cated above. This bombardment history is consistent preservation of the crustal dichotomy boundary, to- with a late heavy bombardment (LHB) of the inner gether with mineralogical evidence in order to infer the Solar System [6] during which HUIA formed, which prevailing surface conditions during the pre-Noachian. followed the planet formation era impacts during The emerging picture is a pre-Noachian Mars that was which the dichotomy formed. less dynamic than Noachian Mars in terms of impacts, Pre-Noachian Tectonism and Volcanism: The geodynamics, and hydrology. crust within each of the southern highlands and north- Pre-Noachian Impacts: We define the pre- ern lowlands is remarkably uniform in thickness, aside Noachian as the time period bounded by two impacts – from regions in which it has been thickened by volcan- the dichotomy-forming impact and the Hellas-forming ism (e.g., Tharsis, Elysium) or thinned by impacts impact.
    [Show full text]
  • Quantitative High-Resolution Reexamination of a Hypothesized
    RESEARCH ARTICLE Quantitative High‐Resolution Reexamination of a 10.1029/2018JE005837 Hypothesized Ocean Shoreline in Cydonia Key Points: • We apply a proposed Mensae on Mars ‐ fi paleoshoreline identi cation toolkit Steven F. Sholes1,2 , David R. Montgomery1, and David C. Catling1,2 to newer high‐resolution data of an exemplar site for paleoshorelines on 1Department of Earth and Space Sciences, University of Washington, Seattle, WA, USA, 2Astrobiology Program, Mars • Any wave‐generated University of Washington, Seattle, WA, USA paleoshorelines should exhibit expressions identifiable in the residual topography from an Abstract Primary support for ancient Martian oceans has relied on qualitative interpretations of idealized slope hypothesized shorelines on relatively low‐resolution images and data. We present a toolkit for • Our analysis of these curvilinear features does not support a quantitatively identifying paleoshorelines using topographic, morphological, and spectroscopic paleoshoreline interpretation and is evaluations. In particular, we apply the validated topographic expression analysis of Hare et al. (2001, more consistent with eroded https://doi.org/10.1029/2001JB000344) for the first time beyond Earth, focusing on a test case of putative lithologies shoreline features along the Arabia level in northeast Cydonia Mensae, as first described by Clifford and Supporting Information: Parker (2001, https://doi.org/10.1006/icar.2001.6671). Our results show these curvilinear features are • Supporting Information S1 inconsistent with a wave‐generated shoreline interpretation. The topographic expression analysis identifies a few potential shoreline terraces along the historically proposed contacts, but these tilt in different directions, do not follow an equipotential surface (even accounting for regional tilting), and are Correspondence to: not laterally continuous.
    [Show full text]
  • Volcanism on Mars
    Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny.
    [Show full text]
  • Mars Science Laboratory: Curiosity Rover Curiosity’S Mission: Was Mars Ever Habitable? Acquires Rock, Soil, and Air Samples for Onboard Analysis
    National Aeronautics and Space Administration Mars Science Laboratory: Curiosity Rover www.nasa.gov Curiosity’s Mission: Was Mars Ever Habitable? acquires rock, soil, and air samples for onboard analysis. Quick Facts Curiosity is about the size of a small car and about as Part of NASA’s Mars Science Laboratory mission, Launch — Nov. 26, 2011 from Cape Canaveral, tall as a basketball player. Its large size allows the rover Curiosity is the largest and most capable rover ever Florida, on an Atlas V-541 to carry an advanced kit of 10 science instruments. sent to Mars. Curiosity’s mission is to answer the Arrival — Aug. 6, 2012 (UTC) Among Curiosity’s tools are 17 cameras, a laser to question: did Mars ever have the right environmental Prime Mission — One Mars year, or about 687 Earth zap rocks, and a drill to collect rock samples. These all conditions to support small life forms called microbes? days (~98 weeks) help in the hunt for special rocks that formed in water Taking the next steps to understand Mars as a possible and/or have signs of organics. The rover also has Main Objectives place for life, Curiosity builds on an earlier “follow the three communications antennas. • Search for organics and determine if this area of Mars was water” strategy that guided Mars missions in NASA’s ever habitable for microbial life Mars Exploration Program. Besides looking for signs of • Characterize the chemical and mineral composition of Ultra-High-Frequency wet climate conditions and for rocks and minerals that ChemCam Antenna rocks and soil formed in water, Curiosity also seeks signs of carbon- Mastcam MMRTG • Study the role of water and changes in the Martian climate over time based molecules called organics.
    [Show full text]
  • Resource Utilization and Site Selection for a Self-Sufficient Martian Outpost
    NASA/TM-98-206538 Resource Utilization and Site Selection for a Self-Sufficient Martian Outpost G. James, Ph.D. G. Chamitoff, Ph.D. D. Barker, M.S., M.A. April 1998 The NASA STI Program Office... in Profile Since its founding, NASA has been dedicated to CONTRACTOR REPORT. Scientific and the advancement of aeronautics and space technical findings by NASA-sponsored science. The NASA Scientific and Technical contractors and grantees. Information (STI) Program Office plays a key part in helping NASA maintain this important CONFERENCE PUBLICATION. Collected role. papers from scientific and technical confer- ences, symposia, seminars, or other meetings The NASA STI Program Office is operated by sponsored or cosponsored by NASA. Langley Research Center, the lead center for NASA's scientific and technical information. SPECIAL PUBLICATION. Scientific, The NASA STI Program Office provides access technical, or historical information from to the NASA STI Database, the largest NASA programs, projects, and mission, often collection of aeronautical and space science STI concerned with subjects having substantial in the word. The Program Office is also public interest. NASA's institutional mechanism for disseminating the results of its research and • TECHNICAL TRANSLATION. development activities. These results are English-language translations of foreign scientific published by NASA in the NASA STI Report and technical material pertinent to NASA's Series, which includes the following report mission. types: Specialized services that complement the STI TECHNICAL PUBLICATION. Reports of Program Office's diverse offerings include completed research or a major significant creating custom thesauri, building customized phase of research that present the results of databases, organizing and publishing research NASA programs and include extensive results.., even providing videos.
    [Show full text]
  • Origin of Fluvial Channels in the Walls of Juventae Chasma: Evidences of Groundwater Sapping? P
    47th Lunar and Planetary Science Conference (2016) 1878.pdf ORIGIN OF FLUVIAL CHANNELS IN THE WALLS OF JUVENTAE CHASMA: EVIDENCES OF GROUNDWATER SAPPING? P. Singh1, R. Sarkar1, I. Ganesh1 and A. Porwal1, 1Geology and Mineral Resources Group, CSRE, Indian Institute of Technology, Bombay, India ([email protected]) Introduction: Juventae Chasma is a deep box- Type IV: This type includes channels emanating from canyon located to the north of Valles Marineris. The gullies between the spurs on the chasma wall (Fig. 1d). main geological units of the chasma are chaotic terrain, They are mainly found in the southern wall of the four mounds of interior layered deposits (ILDs) and an chasma. These channels have shorter lengths ranging outflow channel. The presence of the outflow channel from 1-6 km and at places converge into a single chan- indicates that water played an important role in the nel. geological and geomorphological evolution of the Age determination: We estimated the ages of the chasma. In this paper, we report ground-water sapping geological units containing Type 1 and Type III chan- features from the wall of Juventae Chasma. We also delineate and characterize fluvial channels originating nels using crater size-frequency distributions. The re- from the chasma wall. This study was carried out using sults indicate that Type 1 channels are younger than panchromatic data from the CTX and digital terrain 790+- 200 Ma and Type III channels are younger than models from the HRSC onboard the MRO and MEX 620+-300 Ma. Type II and IV were left out because of respectively.
    [Show full text]
  • Propagation Dynamics of Spatio-Temporal Wave Packets
    PROPAGATION DYNAMICS OF SPATIO-TEMPORAL WAVE PACKETS Thesis Submitted to The School of Engineering of the UNIVERSITY OF DAYTON In Partial Fulfillment of the Requirements for The Degree of Master of Science in Electro-Optics By Qian Cao UNIVERSITY OF DAYTON Dayton, Ohio August, 2014 PROPAGATION DYNAMICS OF SPATIO-TEMPORAL WAVE PACKETS Name: Cao, Qian APPROVED BY: Andy Chong, Ph.D. Joseph Haus, Ph.D. Advisor Committee Chairman Committee Member Assistant Professor, Department of Professor, Electro-Optics Graduate Physics Engineering Program Partha Banerjee, Ph.D. Committee Member Professor, Electro-Optics Graduate Engineering Program John G. Weber, Ph.D. Eddy M. Rojas, Ph.D., M.A., P.E. Associate Dean Dean, School of Engineering School of Engineering ii c Copyright by Qian Cao All rights reserved 2014 ABSTRACT PROPAGATION DYNAMICS OF SPATIO-TEMPORAL WAVE PACKETS Name: Cao, Qian University of Dayton Advisor: Dr. Andy Chong We measured the three-dimensional (3D) propagation dynamics of the Airy-Bessel wave packet, inculding its intensity and phase evolution. Its non-diffraction and non-dispersive features were verified. Meanwhile, we built a spatial light modulator (SLM) based wave packet shaping system to generate other types of wave packets such as Airy-Airy-Airy and dual-Airy-Airy-rings. These wave packets were also measured in 3D. The abrupt 3D autofocusing effect was observed on dual-Airy- Airy-rings. iii To my family, my advisor and committee members and the time in University of Dayton. iv ACKNOWLEDGMENTS First of all, I want to express my thank to my advisor, Prof. Andy Chong. Although the time when I became his student it was the second year of his professor career, he taught and guided me in the world of science in such an experienced way.
    [Show full text]
  • Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°.
    [Show full text]