DOCSLIB.ORG

Constraints on Mars's Recent Equatorial Wind Regimes from Interior Layered Deposits and Comparison with General Circulation Model Results E

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Constraints on Mars's Recent Equatorial Wind Regimes from Interior Layered Deposits and Comparison with General Circulation Model Results E Constraints on Mars's recent equatorial wind regimes from interior layered deposits and comparison with general circulation model results E. Sefton-Nash1 , N. A. Teanby 2, C. Newman3 , R. A. Clancy 2, M. I. Richardson3 1. Department of Earth and Space Sciences, University of California Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095, USA. [email protected] 2. School of Earth Sciences, University of Bristol, Queen’s Road, Bristol, UK, BS8 1RJ. 3. Ashima Research, 600 S. Lake Ave., Pasadena, CA 91106, USA. Introduction Aeolis Gale Crater (west) Candor Chasma In some sites yardangs showed a 1 1 1 10 10 10 A B distinctive teardrop shape (e.g. Aeolian features on Mars are transient on a range of timescales. 2 2 2 Figure 3B), allowing inference of a 0 0 0 100 Ma 10 100 Ma 10 100 Ma 10 unique wind direction. In other The orientations of features such as dunes and yardangs are controlled by the prevailing −1 −1 −1 sites, yardangs with more elongate 10 10 Ma 10 10 10 Ma wind regime over thier respective intervals of formation. No. Craters/km No. Craters/km 10 Ma No. Craters/km and parallel topography allowed 10 ka 10 ka 10 ka −2 −2 −2 10 10 10 inference only of a 180° ambigu- 1 Ma 1 Ma 1 Ma Statistical analysis of the orientations of young features allows probing of Mars's recent 100 ka 100 ka 100 ka 5 10 20 40 60 100 150 5 10 20 40 60 100 150 1 2 5 10 20 40 60 100150 ous trend line (e.g. Figure 3A). wind regime and comparison with wind elds predicted by general circulation models Diameter (m) Diameter (m) Diameter (m) (GCMs). Gordii Dorsum Danielson Crater Iani Chaos Dune orientation was determined 1 1 1 by measurement of the trend line We collect statistical distributions of transverse dune trends and yardang azimuths at nine 10 10 10 parallel to the mean azimuth of 2 2 2 sites on Mars (Figure 1), and compare measured feature orientations to those predicted 0 0 0 10 10 10 each dune crest (Figure 3C). Dune from interpretation of time-integrated wind vectors from the MarsWRF GCM [1, 7]. 100 Ma 100 Ma 100 Ma slip-face normals were perpen- −1 −1 −1 10 10 Ma 10 10 Ma 10 10 Ma No. Craters/km No. Craters/km No. Craters/km dicular to this, but for transverse We focus on features atop interior layered deposits because their young surface ages [2] 10 ka 10 ka 10 ka −2 −2 −2 dunes wind direction remains 180° 10 10 10 and erodible nature makes them applicable to determination of Mars's modern wind 1 Ma 1 Ma 1 Ma C D 100 ka 100 ka 100 ka ambiguous. regime. 5 10 20 40 60 100 150 5 10 20 40 60 100 150 5 10 20 40 60 100 150 Diameter (m) Diameter (m) Diameter (m) 90 20000 Figure 2: Crater size-frequency distributions on ILDs compared to model surface-age isochrons of [5]. 60 15000 We determine eective resurfacing age, and therefore maximum aeolian feature age, for ILDs at each site using small crater populations observed in HiRISE images. 30 Gordii Dorsum 10000 (North & South) Danielson Crater ArabiaArabia TerraTerra Gordii Dorsum (North(South)) Six sites harboured sucient crater populations (e.g. Figure 3E) to enable dating: Aeolis, Candor E Gale Crater Iani Chaos Candor Chasma tion (m) 0 (East & West) GaleGaleAeolis Aeolis CraterCrater (West(East)) Candor Chasma a Chasma, Danielson Crater, Gale Crater (east), Gordii Dorsum (south) and Iani Chaos. v Latitude 5000 Iani Chaos −30 MOLA ele Isochrons in Figure 2 are for model surface ages based on [5], which represents a renement and 0 synthesis of crater-dating techniques. This includes a correction applied to account for the loss of small ( D < 20 m ) bolides in Mars's atmosphere [6]. Error bars represent a factor of two either side of −60 Figure 3: A) Yardang with 180° ambiguous inferred wind −5000 the measured crater density, as suggested by [4]. Uncertainties are greatest if only small (D < 100m) direction B) Yardang with unique inferred wind direction craters are used [5] and we therefore interpret our crater statistics to give order of magnitude resur- (blue bars in Figure 4, except for Danielson crater, in −90 0 60 120 180 240 300 360 facing age estimates, rather than constrained model ages. which all yardang orientations are duplicated in the op- Longitude posite sense.). C) Transverse dune crests (red bars in Figure 1: Location of sites selected for this study. Base map is MOLA 32ppd topography [3]. In general, aeolian features on ILDs at these sites are younger than 0.1-10Ma. Figure 4). D) Aeolian feature population in one HiRISE image. E) Small crater population. Results (Figure 4) Aeolis Arabia Terra Candor Chasma Danielson Crater Gale Crater (east) Gale Crater (west) Gordii Dorsum (south) Gordii Dorsum (north) Iani Chaos 0 0 0 0 0 0 0 Dunes 330 30 330 30 330 30 330 30 330 30 330 30 330 30 Dune trend predicted by maximizing gross-bedform normal transport (GBNT) 300 60 300 60 300 60 300 60 300 60 300 60 300 60 Primary maximum: -2 Weighted by Fryberger (1979) ux with threshold = 0 Nm 30% 15 20% 15% 30% 30% 20% 15% -2 10 20 10 10 20 20 10 15 10 Weighted by Fryberger (1979) ux with threshold = 0.008 Nm No dunes counted. 5 5 10 10 5 5 270 90 270 90 270 90 270 90 270 90 270 90 No dunes counted. 270 90 -2 Weighted by Fryberger (1979) ux with threshold = 0.016 Nm Secondary maximum of signicant magnitude (Iani Chaos only): -2 Weighted by Fryberger (1979) ux with threshold = 0.008 Nm 240 120 240 120 240 120 240 120 240 120 240 120 240 120 -2 Weighted by Fryberger (1979) ux with threshold = 0.016 Nm 210 150 210 150 210 150 210 150 210 150 210 150 210 150 180 180 180 180 180 180 180 0 0 0 1 0 0 0 0 0 0 330 30 330 30 330 30 330 30 330 1 30 330 1 30 330 30 330 30 330 30 1 1 300 60 300 60 300 60 300 60 300 60 300 60 300 60 300 60 300 60 Yardangs 1 1 1 40% 30% 15% 20 30 20 10 6 8 10% 30 40% 30 40 50% 20 30% 30 40% 8 10% 1 Maximum MarsWRF vector frequency 10 10 5 2 4 10 20 10 20 10 10 20 2 4 6 270 90 270 90 270 90 270 90 270 90 270 90 270 90 270 90 270 90 2 Secondary vector frequency maximum 1 240 2 120 240 120 240 120 240 120 240 120 240 120 240 120 240 120 2402 120 2 210 150 210 150 210 150 210 150 210 2 150 210 150 210 150 210 150 210 150 180 180 180 180 180 180 180 180 180 0 0 0 0 0 0 0 0 0 330 30 330 30 330 30 330 30 330 30 330 30 330 30 330 30 330 30 Normalized frequency of MarsWRF wind vector orientation: 300 60 300 60 300 60 300 60 300 60 300 60 300 60 300 60 300 60 Unweighted Weighted by vector mean stress, u* 1 1 1 1 1 1 1 1 1 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 0.5 Weighted by Fryberger (1979) ux 270 90 270 90 270 90 270 90 270 90 270 90 270 90 270 90 270 90 -2 Weighted by Fryberger (1979) ux with 0.008 Nm threshold Weighted by Fryberger (1979) ux with 0.016 Nm-2 threshold 240 120 240 120 240 120 240 120 240 120 240 120 240 120 240 120 240 120 5 Weighted by u* ux with 0.008 Nm-2 threshold 210 150 210 150 210 150 210 150 210 150 210 150 210 150 210 150 210 150 180 180 180 180 180 180 180 180 180 10 6 8 8 2 4 4 8 6 Gross bedform-normal transport (GBNT) 2 4 6 6 2 −2 GBNT with a stress threshold of 0.008 Nm 4 2 2 4 4 2 2 2 2 Relative Gross Bedform- Normal Transport 0 0 0 0 0 0 0 0 0 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 0 30 60 90 120 150 180 Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) Bedform Azimuth ( °) GCM sampling & prediction of feature orientation Conclusions References In 4 out of 7 sites, dune orientations are predicted within ~10° by the MarsWRF GCM [1] Richardson, M. I. et al. (2007) J. Geophys. Res. 112 (E9). At each site we sampled the MarsWRF GCM [1,7] for each minute of a Mars year, by maximizing gross bedform-normal transport. Locations that do not match often [2] Warner, N. H. et al. (2011) J. Geophys. Res. Plan. 116 (E06003), 1-29. giving a total of 963360 wind vectors, spread uniformly throughout the year.
Load more

Recommended publications
  • Performance and Contributions of the Green Industry to Utah's Economy
    Utah State University DigitalCommons@USU All Graduate Plan B and other Reports Graduate Studies 5-2021 Performance and Contributions of the Green Industry to Utah's Economy Lara Gale Utah State University Follow this and additional works at: https://digitalcommons.usu.edu/gradreports Part of the Regional Economics Commons Recommended Citation Gale, Lara, "Performance and Contributions of the Green Industry to Utah's Economy" (2021). All Graduate Plan B and other Reports. 1551. https://digitalcommons.usu.edu/gradreports/1551 This Report is brought to you for free and open access by the Graduate Studies at DigitalCommons@USU. It has been accepted for inclusion in All Graduate Plan B and other Reports by an authorized administrator of DigitalCommons@USU. For more information, please contact [email protected]. PERFORMANCE AND CONTRIBUTIONS OF THE GREEN INDUSTRY TO UTAH’S ECONOMY by Lara Gale A research paper submitted in the partial fulfillment of the requirements for the degree of MASTER OF SCIENCE in Applied Economics Approved: ____________________________ ______________________________ Man Keun Kim, Ph.D. Ruby Ward, Ph.D. Major Professor Committee Member ____________________________ Larry Rupp, Ph.D. Committee Member UTAH STATE UNIVERSITY Logan, Utah 2021 ii ABSTRACT PERFORMANCE AND CONTRIBUTIONS OF THE GREEN INDUSTRY TO UTAH’S ECONOMY by Lara Gale, MS in Applied Economics Utah State University, 2021 Major Professor: Dr. Man Keun Kim Department: Applied Economics Landscaping and nursery enterprises, commonly known as green industry enterprises, can be found everywhere in Utah, and are necessary to create both aesthetic appeal and human well-being in the built environment. In order to understand the impact that events such as economic shocks or policy changes may have on the green industry, the baseline performance and contribution of the industry must be specified for comparison following these shocks.
    [Show full text]
  • “Mining” Water Ice on Mars an Assessment of ISRU Options in Support of Future Human Missions
    National Aeronautics and Space Administration “Mining” Water Ice on Mars An Assessment of ISRU Options in Support of Future Human Missions Stephen Hoffman, Alida Andrews, Kevin Watts July 2016 Agenda • Introduction • What kind of water ice are we talking about • Options for accessing the water ice • Drilling Options • “Mining” Options • EMC scenario and requirements • Recommendations and future work Acknowledgement • The authors of this report learned much during the process of researching the technologies and operations associated with drilling into icy deposits and extract water from those deposits. We would like to acknowledge the support and advice provided by the following individuals and their organizations: – Brian Glass, PhD, NASA Ames Research Center – Robert Haehnel, PhD, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory – Patrick Haggerty, National Science Foundation/Geosciences/Polar Programs – Jennifer Mercer, PhD, National Science Foundation/Geosciences/Polar Programs – Frank Rack, PhD, University of Nebraska-Lincoln – Jason Weale, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory Mining Water Ice on Mars INTRODUCTION Background • Addendum to M-WIP study, addressing one of the areas not fully covered in this report: accessing and mining water ice if it is present in certain glacier-like forms – The M-WIP report is available at http://mepag.nasa.gov/reports.cfm • The First Landing Site/Exploration Zone Workshop for Human Missions to Mars (October 2015) set the target
    [Show full text]
  • Pacing Early Mars Fluvial Activity at Aeolis Dorsa: Implications for Mars
    1 Pacing Early Mars fluvial activity at Aeolis Dorsa: Implications for Mars 2 Science Laboratory observations at Gale Crater and Aeolis Mons 3 4 Edwin S. Kitea ([email protected]), Antoine Lucasa, Caleb I. Fassettb 5 a Caltech, Division of Geological and Planetary Sciences, Pasadena, CA 91125 6 b Mount Holyoke College, Department of Astronomy, South Hadley, MA 01075 7 8 Abstract: The impactor flux early in Mars history was much higher than today, so sedimentary 9 sequences include many buried craters. In combination with models for the impactor flux, 10 observations of the number of buried craters can constrain sedimentation rates. Using the 11 frequency of crater-river interactions, we find net sedimentation rate ≲20-300 μm/yr at Aeolis 12 Dorsa. This sets a lower bound of 1-15 Myr on the total interval spanned by fluvial activity 13 around the Noachian-Hesperian transition. We predict that Gale Crater’s mound (Aeolis Mons) 14 took at least 10-100 Myr to accumulate, which is testable by the Mars Science Laboratory. 15 16 1. Introduction. 17 On Mars, many craters are embedded within sedimentary sequences, leading to the 18 recognition that the planet’s geological history is recorded in “cratered volumes”, rather than 19 just cratered surfaces (Edgett and Malin, 2002). For a given impact flux, the density of craters 20 interbedded within a geologic unit is inversely proportional to the deposition rate of that 21 geologic unit (Smith et al. 2008). To use embedded-crater statistics to constrain deposition 22 rate, it is necessary to distinguish the population of interbedded craters from a (usually much 23 more numerous) population of craters formed during and after exhumation.
    [Show full text]
  • FROM WET PLANET to RED PLANET Current and Future Exploration Is Shaping Our Understanding of How the Climate of Mars Changed
    FROM WET PLANET TO RED PLANET Current and future exploration is shaping our understanding of how the climate of Mars changed. Joel Davis deciphers the planet’s ancient, drying climate 14 DECEMBER 2020 | WWW.GEOLSOC.ORG.UK/GEOSCIENTIST WWW.GEOLSOC.ORG.UK/GEOSCIENTIST | DECEMBER 2020 | 15 FEATURE GEOSCIENTIST t has been an exciting year for Mars exploration. 2020 saw three spacecraft launches to the Red Planet, each by diff erent space agencies—NASA, the Chinese INational Space Administration, and the United Arab Emirates (UAE) Space Agency. NASA’s latest rover, Perseverance, is the fi rst step in a decade-long campaign for the eventual return of samples from Mars, which has the potential to truly transform our understanding of the still scientifi cally elusive Red Planet. On this side of the Atlantic, UK, European and Russian scientists are also getting ready for the launch of the European Space Agency (ESA) and Roscosmos Rosalind Franklin rover mission in 2022. The last 20 years have been a golden era for Mars exploration, with ever increasing amounts of data being returned from a variety of landed and orbital spacecraft. Such data help planetary geologists like me to unravel the complicated yet fascinating history of our celestial neighbour. As planetary geologists, we can apply our understanding of Earth to decipher the geological history of Mars, which is key to guiding future exploration. But why is planetary exploration so focused on Mars in particular? Until recently, the mantra of Mars exploration has been to follow the water, which has played an important role in shaping the surface of Mars.
    [Show full text]
  • CURRICULUM VITAE Bradley J
    CURRICULUM VITAE Bradley J. Thomson Assistant Professor Department of Earth & Planetary Sciences Phone: 865.974.2699 University of Tennessee Fax: 865.974.2368 1621 Cumberland Ave., Room 602 Email: [email protected] Knoxville, TN 37996-1410 Website: https://lunatic.utk.edu EDUCATION Ph.D. Geological Sciences, Brown University, 2006 Dissertation title: Recognizing impact glass on Mars using surface texture, mechanical properties, and mid-infrared spectroscopic properties Advisor: Peter H. SchultZ M.Sc. Geological Sciences, Brown University, 2001 Thesis title: Utopia Basin, Mars: Origin and evolution of basin internal structure Advisor: James W. Head III B.S. Harvey Mudd College, 1999, Geology major at Pomona College Thesis title: Thickness of basalts in Mare Imbrium Advisor: Eric B. Grosfils PROFESSIONAL EXPERIENCE Assistant Professor, Department of Earth and Planetary Sciences (EPS), University of Tennessee, Knoxville TN, 2020–present Research Associate Professor, Department of Earth and Planetary Sciences (EPS), University of Tennessee, Knoxville TN, 2016–2020 Senior Research Scientist, Boston University Center for Remote Sensing, 2011–2016 Co-Investigator, Mini-RF radar on the Lunar Reconnaissance Orbiter, 2009–present Co-Investigator, Mini-SAR radar on Chandrayaan-1, 2008–2009 Senior Staff Scientist, JHU Applied Physics Lab, 2008–2011 NASA Postdoctoral Program Fellow, Jet Propulsion Lab, 2006–2008 Science Theme Lead for mass wasting processes HiRISE camera on Mars Reconnaissance Orbiter, 2007–2010 Postdoctoral Fellow, Lunar and Planetary
    [Show full text]
  • Origin and Evolution of the Peace Vallis Fan System That Drains Into the Curiosity Landing Area, Gale Crater
    44th Lunar and Planetary Science Conference (2013) 1607.pdf ORIGIN AND EVOLUTION OF THE PEACE VALLIS FAN SYSTEM THAT DRAINS INTO THE CURIOSITY LANDING AREA, GALE CRATER. M. C. Palucis1, W. E. Dietrich1, A. Hayes1,2, R.M.E. Wil- liams3, F. Calef4, D.Y. Sumner5, S. Gupta6, C. Hardgrove7, and the MSL Science Team, 1Department of Earth and Planetary Science, University of California, Berkeley, CA, [email protected] and [email protected], 2Department of Astronomy, Cornell University, Ithaca, NY, [email protected], 3Planetary Science Institute, Tucson, AZ, [email protected], 4Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, [email protected], 5Department of Geology, University of California, Davis, Davis, CA, [email protected], 6Department of Earth Science, Imperial College, London, UK, [email protected], 7Malin Space Science Systems, San Diego, CA, [email protected] Introduction: Alluvial fans are depositional land- forms consisting of unconsolidated, water-transported sediment, whose fan shape is the result of sediment deposition downstream of an upland sediment point source. Three mechanisms have been identified, on Earth, for sediment deposition on a fan: avulsing river channels, sheet flows, and debris flows [e.g. 1-3]. Elu- cidating the dominant transport mechanism is im- portant for predicting water sources and volumes to the fan, estimating minimum timescales for fan formation, and understanding the regional climate at the time of fan building. This is especially relevant at Gale Crater (5.3oS 137.7oE), which contains a large alluvial fan, Peace Vallis fan, within the vicinity of the Bradbury Figure 1: HiRISE image of Peace Vallis Fan with smoothed 5-m landing site of the Mars Science Laboratory (MSL) contours.
    [Show full text]
  • Workshop Schedule
    Learn to Live Green. IT PAYS. Workshop Schedule TRADITIONAL YARD 9:00-9:20 Water Wise & Native Plants and Their Uses (New Horizons Nursery) Faye Rutishauser 9:30-9:50 Drip Irrigation Demonstration (The Gardening Coach) Kathlyn Collins 10:00-10:20 Fundamentals of Ecological Gardening (Mountain Bear Inc) Fred Montague 10:30-10:50 The Many Uses of Ornamental Grass (Growing Empire) Ruth McAngus 11:00-11:20 Benefits of Using a Geothermal System for Your Home (Comfort Tech) Becky Robbins 11:30-11:50 Fundamentals of Ecological Gardening (Mountain Bear Inc) Fred Montague 12:00-12:20 Drip Irrigation Demonstration (The Gardening Coach) Kathlyn Collins 12:30-12:50 Green Building is Better Building (G-Build) Brett Moyer 1:00-1:20 Socially Responsible Trading & Investing in the new economy (Locals Have More Fun) Brian Kahn 1:30-1:50 Water Wise & Native Plants and Their Uses (New Horizons Nursery) Faye Rutishauser 2:00-2:20 Brick paver installation techniques using recycled products (O’Brien Landscaping & Construction) Kevin O’Brien NORTH GATHERING AREA – JVWCD STAFF 9:00 Garden Tour 10:00 Garden Tour 11:00 Garden Tour 12:00 Garden Tour 1:00 Garden Tour NORTH GATHERING AREA 9:00 - 9:20 Water conservation for your system (Sprinkler World) Gig Bunnell 9:30 - 9:50 Water Management and Rebates (Innovative Management Solutions) Phil Fabry 10:00 -10:20 Sustainable Marketplace (Re-Direct Guide) Lara Gale 10:30 -10:50 Water Management and Rebates (Innovative Management Solutions) Phil Fabry 11:00 -11:20 Solar Electric Technology 101 (Wind Springs Energy) Mark Price 11:30 -11:50 Rebates For Attic Insulation Upgrade (Energy Savers Insulation) Jeff Dimond 12:00 -12:20 Enhancing Vegetation With Trace Mineral Supplementation (Int’l Institutue for Health & Wellness) Dr.
    [Show full text]
  • A Noachian/Hesperian Hiatus and Erosive Reactivation of Martian Valley Networks
    Lunar and Planetary Science XXXVI (2005) 2221.pdf A NOACHIAN/HESPERIAN HIATUS AND EROSIVE REACTIVATION OF MARTIAN VALLEY NETWORKS. R. P. Irwin III1,2, T. A. Maxwell1, A. D. Howard2, R. A. Craddock1, and J. M. Moore3, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, MRC 315, 6th St. and Inde- pendence Ave. SW, Washington DC 20013-7012, [email protected], [email protected], [email protected]. 2Dept. of Environmental Sciences, P.O. Box 400123, University of Virginia, Charlottesville, VA 22904, [email protected]. 3NASA Ames Research Center, MS 245-3 Moffett Field, CA 94035-1000, [email protected]. Introduction: Despite new evidence for persistent rary in degraded craters of the southern equatorial lati- flow and sedimentation on early Mars [1−3], it remains tudes. All of these deposits likely formed during the unclear whether valley networks were active over long last stage of valley network activity, which appears to geologic timescales (105−108 yr), or if flows were per- have declined rapidly. sistent only during multiple discrete episodes [4] of Gale crater: Gale crater is an important strati- moderate (≈104 yr) to short (<10 yr) duration [5]. Un- graphic marker between discrete episodes of valley derstanding the long-term stability/variability of valley network activity. Gale retains most of the characteris- network hydrology would provide an important control tics of a fresh impact crater [15]: a rough ejecta blan- on paleoclimate and groundwater models. Here we ket, raised rim, hummocky interior walls, secondary describe geologic evidence for a hiatus in highland crater chains, and a (partially buried) central peak valley network activity while the fretted terrain (Figure 2).
    [Show full text]
  • Comment on Liquid Water and Life on Mars
    obiolog str y & f A O u o l t a r e n Chandra Wickramasinghe, Astrobiol Outreach 2015, 3:5 a r c u h o J Journal of Astrobiology & Outreach DOI: 10.4172/2332-2519.1000e111 ISSN: 2332-2519 Editorial Open Access Comment on Liquid Water and Life on Mars Chandra Wickramasinghe N*,1,2,3 1Buckingham Centre for Astrobiology (BCAB), Buckingham University, UK 2Institute for the Study of Panspermia and Astroeconomics, Gifu, Japan 3University of Peradeniya, Peradeniya, Sri Lanka *Corresponding author: Wickramasinghe NC, Buckingham Centre for Astrobiology (BCAB), Buckingham University, UK, Tel: +44-777-838-9243; E-mail: [email protected] Rec date: October 01, 2015; Acc date: October 05, 2015; Pub date: October 07, 2015 Copyright: © 2015 Chandra Wickramasinghe N, et al. This is an open-access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited. Editorial but it was quickly rejected on grounds of alleged uncertainties of interpretation, as well as the lack of organic molecules detectable at the The announcement this week of the detection of liquid water on landing site. A year later, in1977, a major dust storm enveloped the Mars has come close on 4 decades after the arrival of the first Viking planet and H. Abadi and the present writer reported evidence of landers at the red planet in 1976 [1]. The temperatures at the two absorption properties of the Martian dust that was consistent with the original landing sites of the Viking spacecraft in 1976 ranged between a presence of aromatic hydrocarbons [3].
    [Show full text]
  • A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars
    minerals Review A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars Joanna Clark 1,* , Brad Sutter 2, P. Douglas Archer Jr. 2, Douglas Ming 3, Elizabeth Rampe 3, Amy McAdam 4, Rafael Navarro-González 5,† , Jennifer Eigenbrode 4 , Daniel Glavin 4 , Maria-Paz Zorzano 6,7 , Javier Martin-Torres 7,8, Richard Morris 3, Valerie Tu 2, S. J. Ralston 2 and Paul Mahaffy 4 1 GeoControls Systems Inc—Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA 2 Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (B.S.); [email protected] (P.D.A.J.); [email protected] (V.T.); [email protected] (S.J.R.) 3 NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (D.M.); [email protected] (E.R.); [email protected] (R.M.) 4 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; [email protected] (A.M.); [email protected] (J.E.); [email protected] (D.G.); [email protected] (P.M.) 5 Institito de Ciencias Nucleares, Universidad Nacional Autonoma de Mexico, Mexico City 04510, Mexico; [email protected] 6 Centro de Astrobiología (INTA-CSIC), Torrejon de Ardoz, 28850 Madrid, Spain; [email protected] 7 Department of Planetary Sciences, School of Geosciences, University of Aberdeen, Aberdeen AB24 3FX, UK; [email protected] 8 Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, 18100 Granada, Spain Citation: Clark, J.; Sutter, B.; Archer, * Correspondence: [email protected] P.D., Jr.; Ming, D.; Rampe, E.; † Deceased 28 January 2021.
    [Show full text]
  • Connecting the Dots
    Image by Bettymaya Foott CONNECTING THE DOTS FY2020 ANNUAL ACCOUNTING COMMUNITY DEVELOPMENT OFFICE REGIONAL PLANNING PROGRAM FROM OUR LEADERSHIP In these uncertain times planning is Our third and final principle is that more important than ever. I’d like community development must be to share our three guiding principles viewed holistically. The true value we with you to introduce this report strive to provide is in connecting the and emphasize the importance of dots, whether that be people, places, planning for all seasons. It may seem tools, guides or resources — making counterintuitive but as one of our connections is what planning is really three principles states, planning is a about. process. It is in this process that we connect the dots that bring people The Community Development Office together to form a true community. (CDO) is thrilled to work with the Community Impact Board (CIB) and Another of our principles is that each the Associations of Governments community is self-determined. As (AOGs) regional planners. With the planners we are here to provide the goal to help our local communities’ resources each community needs to use their valuable and scarce develop in the manner they see fit resources, including amazing people, based on the changing circumstances to build their community their way. of their respective communities. Working with our regional planners On behalf of all the planners we thank we are better able to know our you for your service and for your communities. To build relationships support of planning in rural Utah. that help us learn the needs of each Together we are making a difference community and how to best serve in creating a viable and resilient place those individual needs.
    [Show full text]
  • Exploring Geomorphic Processes and Martian Gale Crater Topography on Mars Using CTX and Hirise Express Image Dataset” by Pavan Kumar Et Al
    Discussions Earth Syst. Sci. Data Discuss., Earth System https://doi.org/10.5194/essd-2019-4-AC1, 2019 Science ESSDD © Author(s) 2019. This work is distributed under the Creative Commons Attribution 4.0 License. Open Access Data Interactive comment Interactive comment on “Exploring Geomorphic Processes and Martian Gale Crater Topography on Mars using CTX and HiRISE Express Image Dataset” by Pavan Kumar et al. Pavan Kumar et al. [email protected] Received and published: 4 March 2019 Doubt of anonymous author of mail regarding the novelty and originality of the manuscript: The study provides the first analysis of the distribution of craters with displaying MLE morphologies. The study finds that MLE craters concentrate along the dichotomy Printer-friendly version boundary and in areas displaying channels such as those near Elysium and Tharsis. Anonymous author says that most of the findings in the paper seems a duplicate ver- Discussion paper sion of the paper by Anderson and Bell (2010): C1 The location of geomorphological features of an area will be the same but in case of Mars it is necessary to find out the mode of origin. Various authors presented their ESSDD views and reviews towards the same features in different way since the origin of the Gale Crater formation cannot be changed but its evidence can be explained in different ways. Single layer ejecta (SLE) is the most common ejecta morphology over the entire Interactive Martian surface. Martian impact craters display a variety of ejecta and interior features comment differing from those seen on dry and atmosphere free bodies like the moon.
    [Show full text]