2020 Mars Base Camp Youth Guide
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Planetary Science Division Status Report
Planetary Science Division Status Report Jim Green NASA, Planetary Science Division January 26, 2017 Astronomy and Astrophysics Advisory CommiBee Outline • Planetary Science ObjecFves • Missions and Events Overview • Flight Programs: – Discovery – New FronFers – Mars Programs – Outer Planets • Planetary Defense AcFviFes • R&A Overview • Educaon and Outreach AcFviFes • PSD Budget Overview New Horizons exploresPlanetary Science Pluto and the Kuiper Belt Ascertain the content, origin, and evoluFon of the Solar System and the potenFal for life elsewhere! 01/08/2016 As the highest resolution images continue to beam back from New Horizons, the mission is onto exploring Kuiper Belt Objects with the Long Range Reconnaissance Imager (LORRI) camera from unique viewing angles not visible from Earth. New Horizons is also beginning maneuvers to be able to swing close by a Kuiper Belt Object in the next year. Giant IcebergsObjecve 1.5.1 (water blocks) floatingObjecve 1.5.2 in glaciers of Objecve 1.5.3 Objecve 1.5.4 Objecve 1.5.5 hydrogen, mDemonstrate ethane, and other frozenDemonstrate progress gasses on the Demonstrate Sublimation pitsDemonstrate from the surface ofDemonstrate progress Pluto, potentially surface of Pluto.progress in in exploring and progress in showing a geologicallyprogress in improving active surface.in idenFfying and advancing the observing the objects exploring and understanding of the characterizing objects The Newunderstanding of Horizons missionin the Solar System to and the finding locaons origin and evoluFon in the Solar System explorationhow the chemical of Pluto wereunderstand how they voted the where life could of life on Earth to that pose threats to and physical formed and evolve have existed or guide the search for Earth or offer People’sprocesses in the Choice for Breakthrough of thecould exist today life elsewhere resources for human Year forSolar System 2015 by Science Magazine as exploraon operate, interact well as theand evolve top story of 2015 by Discover Magazine. -
Design of Low-Altitude Martian Orbits Using Frequency Analysis A
Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noullez, K. Tsiganis To cite this version: A. Noullez, K. Tsiganis. Design of Low-Altitude Martian Orbits using Frequency Analysis. Advances in Space Research, Elsevier, 2021, 67, pp.477-495. 10.1016/j.asr.2020.10.032. hal-03007909 HAL Id: hal-03007909 https://hal.archives-ouvertes.fr/hal-03007909 Submitted on 16 Nov 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noulleza,∗, K. Tsiganisb aUniversit´eC^oted'Azur, Observatoire de la C^oted'Azur, CNRS, Laboratoire Lagrange, bd. de l'Observatoire, C.S. 34229, 06304 Nice Cedex 4, France bSection of Astrophysics Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, GR 541 24 Thessaloniki, Greece Abstract Nearly-circular Frozen Orbits (FOs) around axisymmetric bodies | or, quasi-circular Periodic Orbits (POs) around non-axisymmetric bodies | are of primary concern in the design of low-altitude survey missions. Here, we study very low-altitude orbits (down to 50 km) in a high-degree and order model of the Martian gravity field. We apply Prony's Frequency Analysis (FA) to characterize the time variation of their orbital elements by computing accurate quasi-periodic decompositions of the eccentricity and inclination vectors. -
The Journey to Mars: How Donna Shirley Broke Barriers for Women in Space Engineering
The Journey to Mars: How Donna Shirley Broke Barriers for Women in Space Engineering Laurel Mossman, Kate Schein, and Amelia Peoples Senior Division Group Documentary Word Count: 499 Our group chose the topic, Donna Shirley and her Mars rover, because of our connections and our interest level in not only science but strong, determined women. One of our group member’s mothers worked for a man under Ms. Shirley when she was developing the Mars rover. This provided us with a connection to Ms. Shirley, which then gave us the amazing opportunity to interview her. In addition, our group is interested in the philosophy of equality and we have continuously created documentaries that revolve around this idea. Every member of our group is a female, so we understand the struggles and discrimination that women face in an everyday setting and wanted to share the story of a female that faced these struggles but overcame them. Thus after conducting a great amount of research, we fell in love with Donna Shirley’s story. Lastly, it was an added benefit that Ms. Shirley is from Oklahoma, making her story important to our state. All of these components made this topic extremely appealing to us. We conducted our research using online articles, Donna Shirley’s autobiography, “Managing Martians”, news coverage from the launch day, and our interview with Donna Shirley. We started our research process by reading Shirley’s autobiography. This gave us insight into her college life, her time working at the Jet Propulsion Laboratory, and what it was like being in charge of such a barrier-breaking mission. -
A Future Mars Environment for Science and Exploration
Planetary Science Vision 2050 Workshop 2017 (LPI Contrib. No. 1989) 8250.pdf A FUTURE MARS ENVIRONMENT FOR SCIENCE AND EXPLORATION. J. L. Green1, J. Hol- lingsworth2, D. Brain3, V. Airapetian4, A. Glocer4, A. Pulkkinen4, C. Dong5 and R. Bamford6 (1NASA HQ, 2ARC, 3U of Colorado, 4GSFC, 5Princeton University, 6Rutherford Appleton Laboratory) Introduction: Today, Mars is an arid and cold world of existing simulation tools that reproduce the physics with a very thin atmosphere that has significant frozen of the processes that model today’s Martian climate. A and underground water resources. The thin atmosphere series of simulations can be used to assess how best to both prevents liquid water from residing permanently largely stop the solar wind stripping of the Martian on its surface and makes it difficult to land missions atmosphere and allow the atmosphere to come to a new since it is not thick enough to completely facilitate a equilibrium. soft landing. In its past, under the influence of a signif- Models hosted at the Coordinated Community icant greenhouse effect, Mars may have had a signifi- Modeling Center (CCMC) are used to simulate a mag- cant water ocean covering perhaps 30% of the northern netic shield, and an artificial magnetosphere, for Mars hemisphere. When Mars lost its protective magneto- by generating a magnetic dipole field at the Mars L1 sphere, three or more billion years ago, the solar wind Lagrange point within an average solar wind environ- was allowed to directly ravish its atmosphere.[1] The ment. The magnetic field will be increased until the lack of a magnetic field, its relatively small mass, and resulting magnetotail of the artificial magnetosphere its atmospheric photochemistry, all would have con- encompasses the entire planet as shown in Figure 1. -
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. -
Kevin Gill ‘11G
InSight: RIVIER ACADEMIC JOURNAL, VOLUME 14, NUMBER 1, FALL 2018 EXPLORING THE UNIVERSE: Meet Kevin Gill ‘11G Michelle Marrone (From Rivier Today, Fall 2018) From the comfort of his lab chair in sunny, southern California, Kevin Gill ’11G has a view into outer space. As a Science Data Software Engineer at NASA’s Jet Propulsion Laboratory (JPL), he spends his time planning and designing technology in support of environmental science and space exploration, as well as data visualization and planetary imaging. His recent work not only produced the first-ever close views of Saturn, but also contributed to NASA’s team winning an Emmy Award. Kevin earned his M.S. in Computer Science at Rivier and has been designing software to render the unique images he gathers ever since. He used an algorithm he developed during his program at Rivier to generate hypothetical images portraying Mars as a vibrant planet with oceans, an oxygen-rich atmosphere, and a green biosphere. The images went viral and within a week his work was featured on major media networks—Discovery News, Fox News, Universe Today, and the Huffington Post. His work captured NASA’s attention and paved the way for his career move. “Rivier taught me many of the algorithms and development practices I still use today at NASA,” says Kevin. “In fact, I can trace the lineage of code currently running on NASA systems directly to my final master’s project at the University.” The systems and tools he develops support a range of scientists specializing in the areas of climate, oceanography, asteroids, planetary science, and others. -
Laser Retroreflectors for Insight and an International Mars Geophysical Network (MGN)
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1492.pdf Laser Retroreflectors for InSight and an International Mars Geophysical Network (MGN). S. Dell’Agnello1, G.O. Delle Monache1, L. Porcelli1,2, M. Tibuzzi1, L. Salvatori1, C. Mondaini1, M. Muccino1, L. Ioppi1, O. Luongo1, M. Petrassi1, G. Bianco1,3, R. Vittori1,4, W.B. Banerdt5, J.F. Grinblat5, C. Benedetto3, F. Pasquali3, R. Mugnuolo3, D.C. Gruel5, J.L.Vago6 and P. Baglioni6. 1Istituto Nazionale di Fisica Nucleare–Laboratori Nazionali di Frascati (INFN–LNF), Via E. Fermi 40, 00044, Frascati, Italy ([email protected]); 2Dipartimento di Fisica, Università della Calabria (UniCal), Via P. Bucci, 87036, Arcavacata di Rende, Italy; 3Agenzia Spaziale Italiana– Centro di Geodesia Spaziale “Giuseppe Colombo” (ASI–CGS), Località, Terlecchia 75100, Matera, Italy; 4Italian Air Force, Rome, Italy, ASI and Embassy of Italy in Washington DC; 5NASA–Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA 91109, USA; 6ESA–ESTEC, Noordwijk, The Netherlands. Abstract. There are laser retroreflectors on the Moon, of the INFN-ASI Affiliation-Association to NASA- but there were no laser retroreflectors on Mars until the SSERVI sservi.nasa.gov) is shown in the figure below. NASA InSight mission [1][2] landed and started oper- ating successfully on the surface of the red planet on Nov. 26, 2018. The ESA ExoMars Schiaparelli mis- sion, which unfortunately failed Mars landing in 2016, was carrying a laser retroreflector like InSight [3]. These instruments are positioned by measuring the time-of-flight of short laser pulses, the so-called “laser ranging” technique (for details on satellite/lunar laser ranging and altimetry see https://ilrs.gsfc.nasa.gov). -
UNITED STATES DISTRICT COURT NORTHERN DISTRICT of INDIANA SOUTH BEND DIVISION in Re FEDEX GROUND PACKAGE SYSTEM, INC., EMPLOYMEN
USDC IN/ND case 3:05-md-00527-RLM-MGG document 3279 filed 03/22/19 page 1 of 354 UNITED STATES DISTRICT COURT NORTHERN DISTRICT OF INDIANA SOUTH BEND DIVISION ) Case No. 3:05-MD-527 RLM In re FEDEX GROUND PACKAGE ) (MDL 1700) SYSTEM, INC., EMPLOYMENT ) PRACTICES LITIGATION ) ) ) THIS DOCUMENT RELATES TO: ) ) Carlene Craig, et. al. v. FedEx Case No. 3:05-cv-530 RLM ) Ground Package Systems, Inc., ) ) PROPOSED FINAL APPROVAL ORDER This matter came before the Court for hearing on March 11, 2019, to consider final approval of the proposed ERISA Class Action Settlement reached by and between Plaintiffs Leo Rittenhouse, Jeff Bramlage, Lawrence Liable, Kent Whistler, Mike Moore, Keith Berry, Matthew Cook, Heidi Law, Sylvia O’Brien, Neal Bergkamp, and Dominic Lupo1 (collectively, “the Named Plaintiffs”), on behalf of themselves and the Certified Class, and Defendant FedEx Ground Package System, Inc. (“FXG”) (collectively, “the Parties”), the terms of which Settlement are set forth in the Class Action Settlement Agreement (the “Settlement Agreement”) attached as Exhibit A to the Joint Declaration of Co-Lead Counsel in support of Preliminary Approval of the Kansas Class Action 1 Carlene Craig withdrew as a Named Plaintiff on November 29, 2006. See MDL Doc. No. 409. Named Plaintiffs Ronald Perry and Alan Pacheco are not movants for final approval and filed an objection [MDL Doc. Nos. 3251/3261]. USDC IN/ND case 3:05-md-00527-RLM-MGG document 3279 filed 03/22/19 page 2 of 354 Settlement [MDL Doc. No. 3154-1]. Also before the Court is ERISA Plaintiffs’ Unopposed Motion for Attorney’s Fees and for Payment of Service Awards to the Named Plaintiffs, filed with the Court on October 19, 2018 [MDL Doc. -
Long-Range Rovers for Mars Exploration and Sample Return
2001-01-2138 Long-Range Rovers for Mars Exploration and Sample Return Joe C. Parrish NASA Headquarters ABSTRACT This paper discusses long-range rovers to be flown as part of NASA’s newly reformulated Mars Exploration Program (MEP). These rovers are currently scheduled for launch first in 2007 as part of a joint science and technology mission, and then again in 2011 as part of a planned Mars Sample Return (MSR) mission. These rovers are characterized by substantially longer range capability than their predecessors in the 1997 Mars Pathfinder and 2003 Mars Exploration Rover (MER) missions. Topics addressed in this paper include the rover mission objectives, key design features, and Figure 1: Rover Size Comparison (Mars Pathfinder, Mars Exploration technologies. Rover, ’07 Smart Lander/Mobile Laboratory) INTRODUCTION NASA is leading a multinational program to explore above, below, and on the surface of Mars. A new The first of these rovers, the Smart Lander/Mobile architecture for the Mars Exploration Program has Laboratory (SLML) is scheduled for launch in 2007. The recently been announced [1], and it incorporates a current program baseline is to use this mission as a joint number of missions through the rest of this decade and science and technology mission that will contribute into the next. Among those missions are ambitious plans directly toward sample return missions planned for the to land rovers on the surface of Mars, with several turn of the decade. These sample return missions may purposes: (1) perform scientific explorations of the involve a rover of almost identical architecture to the surface; (2) demonstrate critical technologies for 2007 rover, except for the need to cache samples and collection, caching, and return of samples to Earth; (3) support their delivery into orbit for subsequent return to evaluate the suitability of the planet for potential manned Earth. -
A La Torre Aaker Aalbers Aaldert Aarmour Aaron
A LA TORRE ABDIE ABLEMAN ABRAMOWITCH AAKER ABE ABLES ABRAMOWITZ AALBERS ABEE ABLETSON ABRAMOWSKY AALDERT ABEEL ABLETT ABRAMS AARMOUR ABEELS ABLEY ABRAMSEN AARON ABEKE ABLI ABRAMSKI AARONS ABEKEN ABLITT ABRAMSON AARONSON ABEKING ABLOTT ABRAMZON AASEN ABEL ABNER ABRASHKIN ABAD ABELA ABNETT ABRELL ABADAM ABELE ABNEY ABREU ABADIE ABELER ABORDEAN ABREY ABALOS ABELES ABORDENE ABRIANI ABARCA ABELI ABOT ABRIL ABATE ABELIN ABOTS ABRLI ABB ABELL ABOTSON ABRUZZO ABBA ABELLA ABOTT ABSALOM ABBARCROMBIE ABELLE ABOTTS ABSALON ABBAS ABELLS ABOTTSON ABSHALON ABBAT ABELMAN ABRAHAM ABSHER ABBATE ABELS ABRAHAMER ABSHIRE ABBATIELLO ABELSON ABRAHAMI ABSOLEM ABBATT ABEMA ABRAHAMIAN ABSOLOM ABBAY ABEN ABRAHAMOF ABSOLON ABBAYE ABENDROTH ABRAHAMOFF ABSON ABBAYS ABER ABRAHAMOV ABSTON ABBDIE ABERCROMBIE ABRAHAMOVITZ ABT ABBE ABERCROMBY ABRAHAMOWICZ ABTS ABBEKE ABERCRUMBIE ABRAHAMS ABURN ABBEL ABERCRUMBY ABRAHAMS ABY ABBELD ABERCRUMMY ABRAHAMSEN ABYRCRUMBIE ABBELL ABERDEAN ABRAHAMSOHN ABYRCRUMBY ABBELLS ABERDEEN ABRAHAMSON AC ABBELS ABERDEIN ABRAHAMSSON ACASTER ABBEMA ABERDENE ABRAHAMY ACCA ABBEN ABERG ABRAHM ACCARDI ABBERCROMBIE ABERLE ABRAHMOV ACCARDO ABBERCROMMIE ABERLI ABRAHMOVICI ACE ABBERCRUMBIE ABERLIN ABRAHMS ACERO ABBERDENE ABERNATHY ABRAHMSON ACESTER ABBERDINE ABERNETHY ABRAM ACETO ABBERLEY ABERT ABRAMCHIK ACEVEDO ABBETT ABEYTA ABRAMCIK ACEVES ABBEY ABHERCROMBIE ABRAMI ACHARD ABBIE ABHIRCROMBIE ABRAMIN ACHENBACH ABBING ABIRCOMBIE ABRAMINO ACHENSON ABBIRCROMBIE ABIRCROMBIE ABRAMO ACHERSON ABBIRCROMBY ABIRCROMBY ABRAMOF ACHESON ABBIRCRUMMY ABIRCROMMBIE ABRAMOFF -
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. -
“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