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Mars 2020 Radiological Contingency Planning
National Aeronautics and Space Administration Mars 2020 Radiological Contingency Planning NASA plans to launch the Mars 2020 rover, produce the rover’s onboard power and to Perseverance, in summer 2020 on a mission warm its internal systems during the frigid to seek signs of habitable conditions in Mars’ Martian night. ancient past and search for signs of past microbial life. The mission will lift off from Cape NASA prepares contingency response plans Canaveral Air Force Station in Florida aboard a for every launch that it conducts. Ensuring the United Launch Alliance Atlas V launch vehicle safety of launch-site workers and the public in between mid-July and August 2020. the communities surrounding the launch area is the primary consideration in this planning. The Mars 2020 rover design is based on NASA’s Curiosity rover, which landed on Mars in 2012 This contingency planning task takes on an and greatly increased our knowledge of the added dimension when the payload being Red Planet. The Mars 2020 rover is equipped launched into space contains nuclear material. to study its landing site in detail and collect and The primary goal of radiological contingency store the most promising samples of rock and planning is to enable an efficient response in soil on the surface of Mars. the event of an accident. This planning is based on the fundamental principles of advance The system that provides electrical power for preparation (including rehearsals of simulated Mars 2020 and its scientific equipment is the launch accident responses), the timely availability same as for the Curiosity rover: a Multi- of technically accurate and reliable information, Mission Radioisotope Thermoelectric Generator and prompt external communication with the (MMRTG). -
Geobiology of the Late Paleoproterozoic Duck Creek Formation, Western Australia
Precambrian Research 179 (2010) 135–149 Contents lists available at ScienceDirect Precambrian Research journal homepage: www.elsevier.com/locate/precamres Geobiology of the late Paleoproterozoic Duck Creek Formation, Western Australia Jonathan P. Wilson a,b,∗, Woodward W. Fischer b, David T. Johnston a, Andrew H. Knoll c, John P. Grotzinger b, Malcolm R. Walter e, Neal J. McNaughton i, Mel Simon d, John Abelson d, Daniel P. Schrag a, Roger Summons f, Abigail Allwood g, Miriam Andres h, Crystal Gammon b, Jessica Garvin j, Sky Rashby b, Maia Schweizer b, Wesley A. Watters f a Department of Earth and Planetary Sciences, Harvard University, USA b Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA c Department of Organismic and Evolutionary Biology, Harvard University, USA d The Agouron Institute, USA e Australian Centre for Astrobiology, University of New South Wales, Australia f Massachusetts Institute of Technology, USA g Jet Propulsion Laboratory, USA h Chevron Corp., USA i Curtin University of Technology, Australia j University of Washington, USA article info abstract Article history: The ca. 1.8 Ga Duck Creek Formation, Western Australia, preserves 1000 m of carbonates and minor Received 25 August 2009 iron formation that accumulated along a late Paleoproterozoic ocean margin. Two upward-deepening Received in revised form 12 February 2010 stratigraphic packages are preserved, each characterized by peritidal precipitates at the base and iron Accepted 15 February 2010 formation and carbonate turbidites in its upper part. Consistent with recent studies of Neoarchean basins, carbon isotope ratios of Duck Creek carbonates show no evidence for a strong isotopic depth gradient, but carbonate minerals in iron formations can be markedly depleted in 13C. -
MARS 2020, CANDIDATES LANDING SITES, EXOMARS and THEIR RELATIONSHIP to MARS SAMPLE RETURN 10:25 A.M
2nd International Mars Sample Return 2018 (LPI Contrib. No. 2071) sess303.pdf Thursday, April 26, 2018 MARS 2020, CANDIDATES LANDING SITES, EXOMARS AND THEIR RELATIONSHIP TO MARS SAMPLE RETURN 10:25 a.m. Forum This session will present a status report on the Mars 2020 sample-caching rover, its candidate landing sites, the Exomars rover mission, and the relationship of all of these to Mars Sample Return. Chairs: Victoria Hipkin (Canadian Space Agency, Canada) Briony Horgan (Purdue University, USA) 10:25 a.m. Williford K. * *Jet Propulsion Laboratory, California Institute of Technology, USA The NASA Mars 2020 Rover Mission The NASA Mars 2020 rover mission will explore an astrobiologically relevant site to characterize its geology, evaluate past habitability, seek signs of ancient life, and assemble a returnable cache of samples. An overview of technical capabilities and scientific strategy in development will be presented with a focus on the role envisioned for Mars 2020 in a possible Mars sample return campaign. 10:45 a.m. Schulte M. * Meyer M. Grant J. Golombek M. *NASA Headquarters, USA The Mars 2020 Rover Mission Landing Site Candidates [#6026] The number of suitable landing sites for the Mars 2020 rover mission has been narrowed to three leading candidates: Jezero Crater, NE Syrtis, and Columbia Hills. Each offers geologic settings with the potential for preservation of biosignatures. 11:00 a.m. Vago J. L. * Svedhem H. Sefton-Nash E. Kminek G. Ruesch O. Haldemann A. F. C. Rodionov D. ExoMars Science Working Team *European Space Agency ExoMars Contributions to Mars Sample Return [#6021] Each of the two ExoMars missions has the potential to make discoveries that could inform and perhaps influence our collective strategy for a future Mars Sample Return mission. -
Jet Propulsion Laboratory, Digital Converters
Jet JUNE Propulsion 2014 Laboratory VOLUME 43 NUMBER 6 JPL 2025 What will JPL be like in 2025? What kind of missions will it be building and flying? How different will the lab be from the JPL of today? Those were the questions on the minds of Executive Council members in early May when they held their annual planning retreat. Over three days they laid out the broad strokes of strategies to make each of the lab’s major program areas robust a decade or more from now. “JPL is currently in good shape, but to remain that way we have to focus on where we are going across the next decade,” JPL Director Charles Elachi said follow- ing the off-site meeting. Among the strategies planned for JPL’s major units, in coming years the Solar System Exploration Director- ate hopes to create missions across a broad spectrum of scales—from flagships to miniature spacecraft. One major focus is to explore the ocean worlds in the outer solar system. The first step for this goal is to continue the development of what is hoped will be the next outer planet mission, Europa Clipper. Thanks to the power of NASA’s new Space Launch System, missions to the outer planets may become more frequent. JPL would also like to execute the first interplanetary mission using a pair of miniature cube- sat spacecraft. The Asteroid Redirect Mission in which JPL has a key role may serve as a model for future Clockwise: 1) Europa Clipper; 2) Mars; 3) Mars Sample Return lander; 4) solar system; 5) Earth satellites; 6) the pulsar planets PSR B1257+12 b, c, and d; 7) spiral closer collaborations with other NASA centers. -
Inventory of CO2 Available for Terraforming Mars
PERSPECTIVE https://doi.org/10.1038/s41550-018-0529-6 Inventory of CO2 available for terraforming Mars Bruce M. Jakosky 1,2* and Christopher S. Edwards3 We revisit the idea of ‘terraforming’ Mars — changing its environment to be more Earth-like in a way that would allow terres- trial life (possibly including humans) to survive without the need for life-support systems — in the context of what we know about Mars today. We want to answer the question of whether it is possible to mobilize gases present on Mars today in non- atmospheric reservoirs by emplacing them into the atmosphere, and increase the pressure and temperature so that plants or humans could survive at the surface. We ask whether this can be achieved considering realistic estimates of available volatiles, without the use of new technology that is well beyond today’s capability. Recent observations have been made of the loss of Mars’s atmosphere to space by the Mars Atmosphere and Volatile Evolution Mission probe and the Mars Express space- craft, along with analyses of the abundance of carbon-bearing minerals and the occurrence of CO2 in polar ice from the Mars Reconnaissance Orbiter and the Mars Odyssey spacecraft. These results suggest that there is not enough CO2 remaining on Mars to provide significant greenhouse warming were the gas to be emplaced into the atmosphere; in addition, most of the CO2 gas in these reservoirs is not accessible and thus cannot be readily mobilized. As a result, we conclude that terraforming Mars is not possible using present-day technology. he concept of terraforming Mars has been a mainstay of sci- Could the remaining planetary inventories of CO2 be mobi- ence fiction for a long time, but it also has been discussed from lized and emplaced into the atmosphere via current or plausible 1 a scientific perspective, initially by Sagan and more recently near-future technologies? Would the amount of CO2 that could T 2 by, for example, McKay et al. -
Mars Reconnaissance Orbiter Maneuver Plan for Mars 2020 Entry, Descent, and Landing Support and Beyond
Jet Propulsion Laboratory California Ins5tute of Technology Mars Reconnaissance Orbiter Maneuver Plan for Mars 2020 Entry, Descent, and Landing Support and Beyond Sean Wagner Premkumar Menon AAS/AIAA Space Flight Mechanics Meeting Ka'anapali, HI January 13{17, 2019 AAS Paper 19-233 c 2019 California Institute of Technology. U.S. Government sponsorship acknowledged. Jet Propulsion Laboratory MarsCalifornia Ins5tute of Technology Reconnaissance Orbiter Project Mars Reconnaissance Orbiter Mission The Mars Reconnaissance Orbiter launched on August 12, 2005 from the Cape Canaveral Air Force Station and arrived at Mars on March 10, 2006. After aerobraking, MRO began the Primary Science Phase (PSP) in November 2006 and continues to perform science observations at Mars. MRO Spacecraft: Spacecraft Bus: 3-axis stabilized ACS system; 3-meter diameter High Gain Antenna; hydrazine propulsion system Instrument Suite: HiRISE Camera, CRISM Imaging Spectrometer, Mars Climate Sounder, Mars Color Imager, Context Camera, Shallow Subsurface Radar, Electra Proximity Link Payload (among other instrument payloads) January 15, 2019 MRO Maneuver Plan for Mars 2020 EDL Support and Beyond SVW { 3 MRO Primary Science Orbit (PSO) The MRO PSO is designed to satisfy science and mission requirements; the spacecraft is flown in an orbit designed to optimize the science instruments performance. The MRO PSO is defined by three key characteristics: Sun-synchronous orbit ascending node at 3:00 PM ± 15 minutes Local Mean Solar Time (LMST) (daylight equatorial crossing) Periapsis -
Valuing Life Detection Missions Edwin S
Valuing life detection missions Edwin S. Kite* (University of Chicago), Eric Gaidos (University of Hawaii), Tullis C. Onstott (Princeton University). * [email protected] Recent discoveries imply that Early Mars was habitable for life-as-we-know-it (Grotzinger et al. 2014); that Enceladus might be habitable (Waite et al. 2017); and that many stars have Earth- sized exoplanets whose insolation favors surface liquid water (Dressing & Charbonneau 2013, Gaidos 2013). These exciting discoveries make it more likely that spacecraft now under construction – Mars 2020, ExoMars rover, JWST, Europa Clipper – will find habitable, or formerly habitable, environments. Did these environments see life? Given finite resources ($10bn/decade for the US1), how could we best test the hypothesis of a second origin of life? Here, we first state the case for and against flying life detection missions soon. Next, we assume that life detection missions will happen soon, and propose a framework (Fig. 1) for comparing the value of different life detection missions: Scientific value = (Reach × grasp × certainty × payoff) / $ (1) After discussing each term in this framework, we conclude that scientific value is maximized if life detection missions are flown as hypothesis tests. With hypothesis testing, even a nondetection is scientifically valuable. Should the US fly more life detection missions? Once a habitable environment has been found and characterized, life detection missions are a logical next step. Are we ready to do this? The case for emphasizing habitable environments, not life detection: Our one attempt to detect life, Viking, is viewed in hindsight as premature or at best uncertain. In-space life detection experiments are expensive. -
Insight Spacecraft Launch for Mission to Interior of Mars
InSight Spacecraft Launch for Mission to Interior of Mars InSight is a robotic scientific explorer to investigate the deep interior of Mars set to launch May 5, 2018. It is scheduled to land on Mars November 26, 2018. It will allow us to better understand the origin of Mars. First Launch of Project Orion Project Orion took its first unmanned mission Exploration flight Test-1 (EFT-1) on December 5, 2014. It made two orbits in four hours before splashing down in the Pacific. The flight tested many subsystems, including its heat shield, electronics and parachutes. Orion will play an important role in NASA's journey to Mars. Orion will eventually carry astronauts to an asteroid and to Mars on the Space Launch System. Mars Rover Curiosity Lands After a nine month trip, Curiosity landed on August 6, 2012. The rover carries the biggest, most advanced suite of instruments for scientific studies ever sent to the martian surface. Curiosity analyzes samples scooped from the soil and drilled from rocks to record of the planet's climate and geology. Mars Reconnaissance Orbiter Begins Mission at Mars NASA's Mars Reconnaissance Orbiter launched from Cape Canaveral August 12. 2005, to find evidence that water persisted on the surface of Mars. The instruments zoom in for photography of the Martian surface, analyze minerals, look for subsurface water, trace how much dust and water are distributed in the atmosphere, and monitor daily global weather. Spirit and Opportunity Land on Mars January 2004, NASA landed two Mars Exploration Rovers, Spirit and Opportunity, on opposite sides of Mars. -
Mars 2020 Mission and NASA’S Mars Exploration Program, Visit: Mars.Nasa.Gov/Mars2020 September 2019 NASA Facts
National Aeronautics and Space Administration Mars 2020 Over the past two decades, missions flown to benefit future robotic and human exploration by NASA’s Mars Exploration Program have of Mars. shown us that Mars was once very different from the cold, dry planet it is today. Evidence Key Objectives discovered by landed and orbital missions point • Explore a geologically diverse landing site to wet conditions billions of years ago. These environments lasted long enough to potentially • Assess ancient habitability support the development of microbial life. • Seek signs of ancient life, particularly in special rocks known to preserve signs of life over time The Mars 2020 rover is designed to better understand the geology of Mars and seek signs of • Gather rock and soil samples that could be ancient life. The mission will collect and store a set returned to Earth by a future NASA mission of rock and soil samples that could be returned to • Demonstrate technology for future robotic and Earth in the future. It will also test new technology human exploration Mission Timeline Key Hardware • Launch in July-August 2020 from Cape The rover will carry seven instruments to conduct Canaveral Air Force Station, Florida unprecedented science and test new technology • Launching on a ULA Atlas 541 procured under on the Red Planet. They are: NASA’s Launch Services Program • Mastcam-Z, an advanced camera system with • Land on Mars on February 18, 2021 at the panoramic and stereoscopic imaging capability site of an ancient river delta in a lake that once with the ability to zoom. The instrument also filled Jezero Crater will determine mineralogy of the Martian surface and assist with rover operations. -
Telephone Remarks to the National Aeronautics and Space
Aug. 13 / Administration of Barack Obama, 2012 Telephone Remarks to the National Aeronautics and Space Administration’s Mars Science Laboratory Team at the Jet Propulsion Laboratory in Pasade- na, California August 13, 2012 The President. Hello, everybody. not know before and laying the groundwork for Jet Propulsion Laboratory Director Charles an even more audacious undertaking in the fu- Elachi. Good morning, Mr. President. ture, and that’s a human mission to the Red The President. Who am I speaking with? Planet. Director Elachi. This is Charles Elachi, the I understand there’s a special Mohawk guy director of JPL. And we have a room full of the that’s working on the mission. [Laughter] He’s mission operation personnel. This is Curiosity been one of the many stars of the show last mission operation on Mars. Sunday night. And I, in the past, thought about The President. Well, it is great to talk to all getting a Mohawk myself—[laughter]—but my of you. And I just want you to know that we team keeps on discouraging me. And now that could not be more excited about what you’ve he’s received marriage proposals and thou- been doing. sands of new Twitter followers, I think that I’m Somebody asked me the other day whether going to go back to my team and see if it makes you’ve already found Martians. [Laughter] I sense. [Laughter] told them we have to give you a little bit of Director Elachi. That’s going to be the new time. But we know you’re all hard at work and fashion at JPL. -
PIXL Seminar, Nov 2015 Why Micro XRF?
Silicon drift detector response function to hard x-rays (with an introduction on quantitative MicroXRF And the Planetary Instrument for X-ray Lithochemistry) Nicolas Michel-Hart with special thanks to Tim Elam for project guidance Applied Physics Laboratory – University of Washington X-ray Fluorescence and μXRF http://in.niton.com/en/ https://xos.com/technologies/xrf/ https://en.wikipedia.org/wiki/X-ray_fluorescence#/media/File:XRFScan.jpg Elam, PIXL Seminar, Nov 2015 Why Micro XRF? Biosignatures (ooids) hosted in a 2.7 billion-year-old carbonate rock Elam, PIXL Seminar, Nov 2015 Some pixels can be very different Area of element maps Visible light image Recent microbialite from the Death Valley Area Elam, PIXL Seminar, Nov 2015 Mars 2020 Mission • M2020 Science Objectives – Habitability: Characterize the geologic record for astrobiologically relevant environments and geologic diversity – Biosignatures: Search for materials with high biosignature preservation potential – Sample Caching: Obtain a pristine set of geologically diverse samples and cache for future return to Earth – Prepare for Humans: Demonstrate in situ resource utilization technologies and characterize dust size and morphology • Mission life: 1.5 Mars years/1005 Martian days • Flight Instruments delivered by Fall 2018, Launch July 2020, Land February 2021 • Instrument Complement: – Mastcam-Z and Supercam for panoramic/stereo imaging and chemical analysis – MEDA for weather – RIMFAX ground penetrating radar – MOXIE technology experiment to produce Oxygen from CO2 – SHERLOC -
The Detection of Long-Chain Bio-Markers Using Atomic Force Microscopy
applied sciences Article The Detection of Long-Chain Bio-Markers Using Atomic Force Microscopy Mark S. Anderson Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA; [email protected]; Tel.: +1-818-354-3278 Received: 15 February 2019; Accepted: 22 March 2019; Published: 27 March 2019 Abstract: The detection of long-chain biomolecules on mineral surfaces is presented using an atomic force microscope (AFM). This is achieved by using the AFM’s ability to manipulate molecules and measure forces at the pico-newton scale. We show that a highly characteristic force-distance signal is produced when the AFM tip is used to detach long-chain molecules from a surface. This AFM force spectroscopy method is demonstrated on bio-films, spores, fossils and mineral surfaces. The method works with AFM imaging and correlated tip enhanced infrared spectroscopy. The use of AFM force spectroscopy to detect this class of long chain bio-markers has applications in paleontology, life detection and planetary science. Keywords: long-chain bio-markers 2; AFM 3; tip enhanced spectroscopy 1. Introduction Scanning probe microscopes are fundamental tools in microscopy and nanotechnology. The most widely utilized of the probe microscopes is the atomic force microscope (AFM) that was first described in 1986 by Binnig, Gerber and Quate [1]. With an AFM, a tip mounted on a micro-fabricated cantilever is scanned over the surface and the interaction between the tip and the substrate is detected by monitoring the deflection of the cantilever [2]. These microscopes are remarkable for their ability to image individual atoms or molecules.