Curiosity Assesses Conditions Favorable for Life
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Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Widespread Excess Ice in Arcadia Planitia, Mars
Widespread Excess Ice in Arcadia Planitia, Mars Ali M. Bramson1, Shane Byrne1, Nathaniel E. Putzig2, Sarah Sutton1, Jeffrey J. Plaut3, T. Charles Brothers4 and John W. Holt4 Corresponding author: A. M. Bramson, Lunar and Planetary Laboratory, University of Arizona, Kuiper Space Science Building, 1629 E. University Blvd. Tucson, AZ, 85721, USA. ([email protected]) Affiliations: 1Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA. 2Southwest Research Institute, Boulder, Colorado, USA. 3Jet Propulsion Laboratory, Pasadena, California, USA. 4Institute for Geophysics, University of Texas at Austin, Austin, Texas, USA. Accepted for publication July 18, 2015 in Geophysical Research Letters. An edited version of this paper was published by AGU on August 26, 2015. Copyright 2015 American Geophysical Union. Citation: Bramson, A. M., S. Byrne, N. E. Putzig, S. Sutton, J. J. Plaut, T. C. Brothers, and J. W. Holt (2015), Widespread excess ice in Arcadia Planitia, Mars, Geophys. Res. Lett., 42, doi:10.1002/2015GL064844. Key points: • Terraced craters: abundant in Arcadia Planitia, indicate subsurface layering • A widespread subsurface interface is also detected by SHARAD • Combining data sets yields dielectric constants consistent with decameters of excess water ice Abstract: The distribution of subsurface water ice on Mars is a key constraint on past climate, while the volumetric concentration of buried ice (pore-filling versus excess) provides information about the process that led to its deposition. We investigate the subsurface of Arcadia Planitia by measuring the depth of terraces in simple impact craters and mapping a widespread subsurface reflection in radar sounding data. Assuming that the contrast in material strengths responsible for the terracing is the same dielectric interface that causes the radar reflection, we can combine these data to estimate the dielectric constant of the overlying material. -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J. -
CHLA 2017 Annual Report
Children’s Hospital Los Angeles Annual Report 2017 About Us The mission of Children’s Hospital Los Angeles is to create hope and build healthier futures. Founded in 1901, CHLA is the top-ranked children’s hospital in California and among the top 10 in the nation, according to the prestigious U.S. News & World Report Honor Roll of children’s hospitals for 2017-18. The hospital is home to The Saban Research Institute and is one of the few freestanding pediatric hospitals where scientific inquiry is combined with clinical care devoted exclusively to children. Children’s Hospital Los Angeles is a premier teaching hospital and has been affiliated with the Keck School of Medicine of the University of Southern California since 1932. Table of Contents 2 4 6 8 A Message From the Year in Review Patient Care: Education: President and CEO ‘Unprecedented’ The Next Generation 10 12 14 16 Research: Legislative Action: Innovation: The Jimmy Figures of Speech Protecting the The CHLA Kimmel Effect Vulnerable Health Network 18 20 21 81 Donors Transforming Children’s Miracle CHLA Honor Roll Financial Summary Care: The Steven & Network Hospitals of Donors Alexandra Cohen Honor Roll of Friends Foundation 82 83 84 85 Statistical Report Community Board of Trustees Hospital Leadership Benefit Impact Annual Report 2017 | 1 This year, we continued to shine. 2 | A Message From the President and CEO A Message From the President and CEO Every year at Children’s Hospital Los Angeles is by turning attention to the hospital’s patients, and characterized by extraordinary enthusiasm directed leveraging our skills in the arena of national advocacy. -
Seasonal Melting and the Formation of Sedimentary Rocks on Mars, with Predictions for the Gale Crater Mound
Seasonal melting and the formation of sedimentary rocks on Mars, with predictions for the Gale Crater mound Edwin S. Kite a, Itay Halevy b, Melinda A. Kahre c, Michael J. Wolff d, and Michael Manga e;f aDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA bCenter for Planetary Sciences, Weizmann Institute of Science, P.O. Box 26, Rehovot 76100, Israel cNASA Ames Research Center, Mountain View, California 94035, USA dSpace Science Institute, 4750 Walnut Street, Suite 205, Boulder, Colorado, USA eDepartment of Earth and Planetary Science, University of California Berkeley, Berkeley, California 94720, USA f Center for Integrative Planetary Science, University of California Berkeley, Berkeley, California 94720, USA arXiv:1205.6226v1 [astro-ph.EP] 28 May 2012 1 Number of pages: 60 2 Number of tables: 1 3 Number of figures: 19 Preprint submitted to Icarus 20 September 2018 4 Proposed Running Head: 5 Seasonal melting and sedimentary rocks on Mars 6 Please send Editorial Correspondence to: 7 8 Edwin S. Kite 9 Caltech, MC 150-21 10 Geological and Planetary Sciences 11 1200 E California Boulevard 12 Pasadena, CA 91125, USA. 13 14 Email: [email protected] 15 Phone: (510) 717-5205 16 2 17 ABSTRACT 18 A model for the formation and distribution of sedimentary rocks on Mars 19 is proposed. The rate{limiting step is supply of liquid water from seasonal 2 20 melting of snow or ice. The model is run for a O(10 ) mbar pure CO2 atmo- 21 sphere, dusty snow, and solar luminosity reduced by 23%. -
→ Space for Europe European Space Agency
number 149 | February 2012 bulletin → space for europe European Space Agency The European Space Agency was formed out of, and took over the rights and The ESA headquarters are in Paris. obligations of, the two earlier European space organisations – the European Space Research Organisation (ESRO) and the European Launcher Development The major establishments of ESA are: Organisation (ELDO). The Member States are Austria, Belgium, Czech Republic, Denmark, Finland, France, Germany, Greece, Ireland, Italy, Luxembourg, the ESTEC, Noordwijk, Netherlands. Netherlands, Norway, Portugal, Romania, Spain, Sweden, Switzerland and the United Kingdom. Canada is a Cooperating State. ESOC, Darmstadt, Germany. In the words of its Convention: the purpose of the Agency shall be to provide for ESRIN, Frascati, Italy. and to promote, for exclusively peaceful purposes, cooperation among European States in space research and technology and their space applications, with a view ESAC, Madrid, Spain. to their being used for scientific purposes and for operational space applications systems: Chairman of the Council: D. Williams → by elaborating and implementing a long-term European space policy, by Director General: J.-J. Dordain recommending space objectives to the Member States, and by concerting the policies of the Member States with respect to other national and international organisations and institutions; → by elaborating and implementing activities and programmes in the space field; → by coordinating the European space programme and national programmes, and by integrating the latter progressively and as completely as possible into the European space programme, in particular as regards the development of applications satellites; → by elaborating and implementing the industrial policy appropriate to its programme and by recommending a coherent industrial policy to the Member States. -
Are We Martians? Looking for Indicators of Past Life on Mars with the Missions of the European Space Agency
CESAR Scientific Challenge Are we Martians? Looking for indicators of past life on Mars with the missions of the European Space Agency Teacher's Guide 1 Are we Martians? CESAR Scientific Challenge Table of contents: Didactics 5 Phase 0 18 Phase 1 20 Activity 1: Refresh concepts 21 Activity 2: Getting familiar with coordinates 21 Activity 2.1: Identify coordinates on an Earth map 21 Activity 2.2: The Martian zero meridian 24 Activity 2.3: Identify coordinates on a Martian map 25 Activity 2.4: A model of Mars 27 Activity 3: The origin of life 28 Activity 3.1: What is life? 28 Activity 3.2: Traces of extraterrestrial life 29 Activity 3.2.1: Read the following article 30 Activity 3.2.2: Read about Rosalind Franklin and ExoMars 2022 30 Activity 3.3: Experiment for DNA extraction 31 Activity 4: Habitable zones 31 Activity 4.1: Habitable zone of our star 31 Activity 4.2: Study the habitable zones of different stars 34 Activity 4.3: Past, present and future of water on Mars 37 Activity 4.4: Extremophiles 39 Activity 5: What do you know about Mars? 40 Activity 6: Scientific knowledge from Mars’ surface 41 Activity 6.1: Geology of Mars 41 Activity 6.2: Atmosphere of Mars 44 Activity 7: Mars exploration by European Space Agency 45 Activity 7.1: Major Milestones of the European Space Agency on Mars 50 Activity 8: Check what you have learnt so far 52 2 Are we Martians? CESAR Scientific Challenge Phase 2 53 Activity 9: Ask for a videocall with the CESAR Team if needed 54 Phase 3 56 Activity 10: Prepare the Mars landing 57 Activity 10.1: Get used to Google Mars. -
Robotics and Automation for “Icebreaker” B.J
ROBOTICS AND AUTOMATION FOR “ICEBREAKER” B.J. Glass (1), G. Paulsen(2), A. Dave (1), C. McKay(1) (1) NASA Ames Research Center, Moffett Field, CA 94035 USA; Email: [email protected] (2) Honeybee Robotics, Pasadena, CA 91103 USA; Email: [email protected] ABSTRACT components that will penetrate below the ground, and place these inside a biobarrier. To prevent The proposed “Icebreaker” mission is a return to spores from traveling onto the drill auger/bit via the Mars polar latitudes first visited by the Phoenix sample transfer, there must be an air gap between mission in 2007-08. Exploring and interrogating the sterilized drill and a less-sterilized robotic the shallow subsurface of Mars from the surface sample delivery subsystem that could contact the will require some form of excavation and “dirty” spacecraft instruments (which will not be penetration, with drilling being the most mature heat sterilized to Viking standards). approach. A series of 0.5-5m automated rotary and rotary-percussive drills developed over the past Since 2006, NASA has developed a Discovery- decade by NASA Ames and Honeybee Robotics class mission concept, called "Icebreaker" (Fig. 1), provide a capability that could fly on a Mars which is a Lockheed-Martin (Phoenix-derived) surface mission within the next decade. Surface Mars polar lander with life and organics detection robotics have been integrated for sample transfer to instruments and a 1m sampling drill [4]. The deck instruments, and the Icebreaker sample Icebreaker science payload has since 2010 also acquisition system has been tested successfully in been the baseline science payload for developing a Mars chambers and analog field sites to depths joint NASA-commercial Mars astrobiology between 1-3m. -
Flight Opportunities Newsletter July 2020
ISSUE: 34 | July 2020 In this issue: • Recent Flights: Aeroseismometer Technologies Tested on Raven Balloons • Opportunities: New NASA Lunar Tech Funding Opportunity for U.S. Universities; NASA Advances Roadmap Toward Solicitation for Lunar Surface Investigations • News: Watch Jim Reuter’s Webinar for AIAA • Team Spotlight: Meet the Newest Member of Our Technology Team, Gregory Peters • Upcoming Events: Learn About NASA’s New PACE Initiative at the SmallSat Conference Enjoy! The Flight Opportunities team Recent Flights Aeroseismometer Technologies Tested on Recent Balloon Flights Future detection of seismic activity on Venus is the goal of four aeroseismometers—three from Sandia National Laboratory and one from NASA’s Jet Propulsion Laboratory (JPL)—flight tested on balloons from Raven Aerostar earlier this month. The instruments were rigged to Raven’s Cyclone balloon systems, which flew at approximately 20 km altitude and 30 km horizontal range from ground chemical explosions to test seismic detection efficacy. Flight Opportunities supported this Sandia-led aeroseismometer test as part of a Venus balloon-based seismology effort led by JPL. The recent flight tests will help Sandia and JPL scientists advance the state of the art for the use of aeroseismometers for potential future infrasound investigations on Venus as well as other planetary bodies. Such studies could reveal whether these planets exhibit similar seismic shifts to the earthquakes we experience on our home planet, and also may uncover valuable information about their interior structures. In a flight test over Lemitar, Flight Opportunities New Mexico, a balloon Campaign Manager from Raven Aerostar Paul De León provides carries technology remote support from from Sandia National his home office for Laboratory and NASA’s Sandia National Jet Propulsion Laboratory Laboratory and Raven that could be used to aid Aerostar during the seismology studies on aeroseismometer flight Venus and other planets. -
X-Band Transmission Evolution Towards DVB-S2
X-band transmission evolution towards DVB-S2 for Small Satellites Miguel Angel Fernandez, Anis Latiri, Gabrielle Michaud – SYRLINKS Clément Dudal, Jean-Luc Issler – CNES SSC 2016 – LOGAN | August 10, 2016 Outline About Syrlinks Flight proven X-band transmitter DVB-S2 implementation High Data Rate Transmitter evolutions SYRLINKS – CNES Small Satellite Conference 2016 2 About Syrlinks Flight Proven X-band Transmitter DVB-S2 Implementation High Data Rate Transmitter Evolutions SYRLINKS – CNES Small Satellite Conference 2016 3 About Syrlinks… . Advanced and cost-effective radio-communication manufacturer . Focuses on advanced, compact, & high reliable radios, for harsh environments . Designs, develops of communication systems in radio navigation & geolocation . Partnership with CNES and ESA since 1997 (Rosetta) * * PARIS . 200 cumulated years in orbit, with 100% reliability RENNES . Pioneer in the use of qualified active COTS . Large space portfolio for LEO missions up to 10 years in orbit, especially based on CLASS 3 ECC-Q-ST-60C design SYRLINKS – CNES Small Satellite Conference 2016 4 2014: EWC30 & 29 CLASS 3 ECSS-Q- Some Milestones… ST-60-C Radios 2012: G-SPHERE-S 2013: EWC27 & 31 GNSS Receiver Nano Radios 2010: EWC22/24/28 2010: EWC20 X Band HDR TM L Band Transmitter 2011: GREAT2 (ESA) GaN Reliability And Technology Transfer initiative 1997: EWC15 2004-2013: EWC15 S Band “ISL” S Band TT&C MYRIADE: CNES/ AIRBUS D&S/ TAS MYRIADE Evolutions ADS/CNES/TAS platform 2004: Rosetta/Philae. Demeter, Essaim (4), PROBA-V: 2013 2013: SARAL Microscope: -
High Temperature Mechanisms M High Temperature Mechanisms a R E Y
S 6 th h o I n r t t e C r o n u a r t i s o e n a o l n P E l a x n t r e e t High Temperature Mechanisms m High Temperature Mechanisms a r e y E P n A Breakthrough Development r o v b i r e o n W m o e r n k t s s h T o p e , c h A n Jerri Ji t l o a l n o t g a Honeybee Robotics Spacecraft Mechanisms Corporation i , e G s e New York, NY o r g i a 0 6 / 2 2 1 0 - 2 0 2 8 Page 1 Overview S • Introduction 6 th h o I n r t t e C • High Temperature Mechanisms r o n u a r t i s o e – High Temperature Switched Reluctance Motor n a o l n P E l – High Temperature Drill a x n t r e e t m – High Temperature Brushless DC Motor & Resolver a r e y E P n r o v b • Summary & Conclusions i r e o n W m o e r n k t s s h T o p e , c h A n t l o a l n o t g a i , e G s e o r g i a 0 6 / 2 2 1 0 - 2 0 2 8 Page 2 Introduction • The extreme high temperature /high pressure environments on S 6 th h o I Venus are unique compare with other NASA Solar System n r t t e C r o exploration mission, environment condition is 460C, 90 bar, 97% n u a r t i s CO2 at the Venus surface, sulphuric acid clouds at 50 km o e n a o l n P • No exist off-the-shelf motors or known R&D prototype motors are E l a x n t r capable of operating under Venus surface conditions for any e e t m a r e appreciable amount of time y E P n r o v • Two types of high temperature motor have been developed by b i r e o n W Honeybee Robotics: m o e r n k t s – HT Switched Reluctance Motor s h T o p e , • Completed Phase I & II study (2.5 years) c h A n t l o a l n • Final prototype was used to actuate a high temperature drill o t g a i , e G – HT DC Brushless Motor and Resolver s e o r • Completed 6 month study (Phase I) g i a • Next generation BLDC motor along with high temperate 0 sample acquisition scoop and high temperature joint are 6 / 2 2 1 0 under development in Phase II study - 2 0 2 8 Page 3 Switched Reluctance Motor • The switched reluctance motor is a direct current, brushless electric S 6 th motor.