Stardust Sample Return
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The Messenger
10th anniversary of VLT First Light The Messenger The ground layer seeing on Paranal HAWK-I Science Verification The emission nebula around Antares No. 132 – June 2008 –June 132 No. The Organisation The Perfect Machine Tim de Zeeuw a groundbased spectroscopic comple thousand each semester, 800 of which (ESO Director General) ment to the Hubble Space Telescope. are for Paranal. The User Portal has Italy and Switzerland had joined ESO in about 4 000 registered users and 1981, enabling the construction of the the archive contains 74 TB of data and This issue of the Messenger marks the 3.5m New Technology Telescope with advanced data products. tenth anniversary of first light of the Very pioneering advances in active optics, Large Telescope. It is an excellent occa crucial for the next step: the construction sion to look at the broader implications of the Very Large Telescope, which Winning strategy of the VLT’s success and to consider the received the green light from Council in next steps. 1987 and was built on Cerro Paranal in The VLT opened for business some five the Atacama desert between Antofagasta years after the Keck telescopes, but the and Taltal in Northern Chile. The 8.1m decision to take the time to build a fully Mission Gemini telescopes and the 8.3m Subaru integrated system, consisting of four telescope were constructed on a similar 8.2m telescopes and providing a dozen ESO’s mission is to enable scientific dis time scale, while the Large Binocular Tele foci for a carefully thoughtout comple coveries by constructing and operating scope and the Gran Telescopio Canarias ment of instruments together with four powerful observational facilities that are now starting operations. -
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. -
Mars Reconnaissance Orbiter
Chapter 6 Mars Reconnaissance Orbiter Jim Taylor, Dennis K. Lee, and Shervin Shambayati 6.1 Mission Overview The Mars Reconnaissance Orbiter (MRO) [1, 2] has a suite of instruments making observations at Mars, and it provides data-relay services for Mars landers and rovers. MRO was launched on August 12, 2005. The orbiter successfully went into orbit around Mars on March 10, 2006 and began reducing its orbit altitude and circularizing the orbit in preparation for the science mission. The orbit changing was accomplished through a process called aerobraking, in preparation for the “science mission” starting in November 2006, followed by the “relay mission” starting in November 2008. MRO participated in the Mars Science Laboratory touchdown and surface mission that began in August 2012 (Chapter 7). MRO communications has operated in three different frequency bands: 1) Most telecom in both directions has been with the Deep Space Network (DSN) at X-band (~8 GHz), and this band will continue to provide operational commanding, telemetry transmission, and radiometric tracking. 2) During cruise, the functional characteristics of a separate Ka-band (~32 GHz) downlink system were verified in preparation for an operational demonstration during orbit operations. After a Ka-band hardware anomaly in cruise, the project has elected not to initiate the originally planned operational demonstration (with yet-to-be used redundant Ka-band hardware). 201 202 Chapter 6 3) A new-generation ultra-high frequency (UHF) (~400 MHz) system was verified with the Mars Exploration Rovers in preparation for the successful relay communications with the Phoenix lander in 2008 and the later Mars Science Laboratory relay operations. -
Rosetta Craft Makes Historic Comet Rendezvous European Space Agency's Comet-Chasing Mission Arrives After 10-Year Journey
NATURE | NEWS Rosetta craft makes historic comet rendezvous European Space Agency's comet-chasing mission arrives after 10-year journey. Elizabeth Gibney 06 August 2014 ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA Comet 67P/Churyumov–Gerasimenko, as seen by Rosetta from a distance of 285 kilometres. No one can deny that it was an epic trip. The European Space Agency's comet-chasing Rosetta spacecraft has arrived at its quarry, after launching more than a decade ago and travelling 6.4 billion kilometres through the Solar System. That makes it the first spacecraft to rendezvous with a comet, and takes the mission a step closer to its next, more ambitious goal of making the first ever soft landing on a comet. Speaking from mission control in Darmstadt, Germany, Matt Taylor, Rosetta project scientist for the European Space Agency (ESA), called the space mission “the sexiest there’s ever been”. Rosetta is now within 100 kilometres of its target, comet 67P/Churyumov–Gerasimenko (or 67P for short), which in July was discovered to be shaped like a rubber duck. After a six-minute thruster burn, at 11:29 a.m. local time on 6 August, ESA scientists confirmed that Rosetta had moved into the same orbit around the Sun as the comet. Rosetta is now moving at a walking pace relative to the motion of 67P — though both are hurtling through space at 15 kilometres per second. Unlike NASA’s Deep Impact and Stardust craft, and ESA’s Giotto mission, which flew by their target comets at high speed, Rosetta will now stay with the comet, taking a ring-side seat as 67P approaches the Sun, and eventually swings around it in August 2015. -
OSIRIS-Rex, Returning the Asteroid Sample
OSIRIS-REx, Returning the Asteroid Sample Thomas Ajluni Timothy Linn William Willcockson ASRC Federal Space & Defense Lockheed Martin Space Systems Lockheed Martin Space Systems 7000 Muirkirk Meadows Drive Company, P.O. Box 179 Company, P.O. Box 179 Suite 100, Beltsville, MD 20705 Denver, CO 80201 Denver, CO 80201 301.286.1831 303-977-0659 303-977-5094 [email protected] [email protected] [email protected] David Everett Ronald Mink Joshua Wood NASA Goddard Space Flight NASA Goddard Space Flight Lockheed Martin Space Systems Center, 8800 Greenbelt Road Center, 8800 Greenbelt Road Company, P.O. Box 179 Greenbelt, MD 20771 Greenbelt, MD 20771 Denver, CO 80201 301.286.1596 301.286.3524 303-977-3199 [email protected] [email protected] [email protected] Abstract—This paper addresses the technical aspects of the sample return system for the upcoming Origins, Spectral x attitude control Interpretation, Resource Identification, and Security-Regolith x propulsion Explorer (OSIRIS-REx) asteroid sample return mission. The x power overall mission design and current implementation are presented as an overview to establish a context for the x thermal control technical description of the reentry and landing segment of the x telecommunications mission. x command and data handling x structural support to ensure successful rendezvous The prime objective of the OSIRIS-REx mission is to sample a with Bennu primitive, carbonaceous asteroid and to return that sample to Earth in pristine condition for detailed laboratory analysis. x characterization of Bennu’s properties Targeting the near-Earth asteroid Bennu, the mission launches x delivery of the sampler to the surface, and return of in September 2016 with an Earth reentry date of September the spacecraft to the vicinity of the Earth 24, 2023. -
An Overview of Hayabusa2 Mission and Asteroid 162173 Ryugu
Asteroid Science 2019 (LPI Contrib. No. 2189) 2086.pdf AN OVERVIEW OF HAYABUSA2 MISSION AND ASTEROID 162173 RYUGU. S. Watanabe1,2, M. Hira- bayashi3, N. Hirata4, N. Hirata5, M. Yoshikawa2, S. Tanaka2, S. Sugita6, K. Kitazato4, T. Okada2, N. Namiki7, S. Tachibana6,2, M. Arakawa5, H. Ikeda8, T. Morota6,1, K. Sugiura9,1, H. Kobayashi1, T. Saiki2, Y. Tsuda2, and Haya- busa2 Joint Science Team10, 1Nagoya University, Nagoya 464-8601, Japan ([email protected]), 2Institute of Space and Astronautical Science, JAXA, Japan, 3Auburn University, U.S.A., 4University of Aizu, Japan, 5Kobe University, Japan, 6University of Tokyo, Japan, 7National Astronomical Observatory of Japan, Japan, 8Research and Development Directorate, JAXA, Japan, 9Tokyo Institute of Technology, Japan, 10Hayabusa2 Project Summary: The Hayabusa2 mission reveals the na- Combined with the rotational motion of the asteroid, ture of a carbonaceous asteroid through a combination global surveys of Ryugu were conducted several times of remote-sensing observations, in situ surface meas- from ~20 km above the sub-Earth point (SEP), includ- urements by rovers and a lander, an active impact ex- ing global mapping from ONC-T (Fig. 1) and TIR, and periment, and analyses of samples returned to Earth. scan mapping from NIRS3 and LIDAR. Descent ob- Introduction: Asteroids are fossils of planetesi- servations covering the equatorial zone were performed mals, building blocks of planetary formation. In partic- from 3-7 km altitudes above SEP. Off-SEP observa- ular carbonaceous asteroids (or C-complex asteroids) tions of the polar regions were also conducted. Based are expected to have keys identifying the material mix- on these observations, we constructed two types of the ing in the early Solar System and deciphering the global shape models (using the Structure-from-Motion origin of water and organic materials on Earth [1]. -
Genesis Radiation Environment
https://ntrs.nasa.gov/search.jsp?R=20070014073 2019-08-30T00:44:36+00:00Z 1 Source of Acquisition NASA Marshall Space Flight Center Genesis Radiation Environment Joseph I. Minow* NASA Marshull Space Flight Center, Huntsville, AL 35812 USA Richard L. Altstatt' and William C. Skipworth* Jacobs Engineering, Marshall Space Flight Center Group, Huntsville, AL 35812 USA The Genesis spacecraft launched on 8 August 2001 sampled solar wind environments at L1 from 2001 to 2004. After the Science Capsule door was opened, numerous foils and samples were exposed to the various solar wind environments during periods including slow solar wind from the streamer belts, fast solar wind flows from coronal holes, and coronal mass ejections. The Survey and Examination of Eroded Returned Surfaces (SEERS) program led by NASA's Space Environments and Effects program had initiated access for the space materials community to the remaining Science Capsule hardware after the science samples had been removed for evaluation of materials exposure to the space environment. This presentation will describe the process used to generate a reference radiation Genesis Radiation Environment developed for the SEERS program for use by the materials science community in their analyses of the Genesis hardware. I. Introduction ASA's Space Environments and Effects (SEE) Program initiated the Surveying and Examination of Eroded N Returned Surfaces (SEERS) Initiative in 2003. The goal of the Initiative was to provide leadership in the engineering analysis of returned flight hardware by supporting a comprehensive effort to understand environmental effects due to solar W, ionizing radiation, plasmas, neutral contamination, meteoroids, and other conditions experienced during the mission (not primary science mission objectives). -
The Mars 2001 Odyssey and the "Autogen" Process
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by DigitalCommons@USU AUTOGEN: The Mars 2001 Odyssey and the "Autogen" Process By Roy Gladden June 6, 2002 Jet Propulsion Laboratory / California Institute of Technology Pasadena, California Abstract In many deep space and interplanetary missions, it is widely recognized that the scheduling of many commands to operate a spacecraft can follow very regular patterns. In these instances, it is greatly desired to convert the knowledge of how commands are scheduled into algorithms in order to automate the development of command sequences. In doing so, it is possible to dramatically reduce the number of people and work-hours that are required to develop a sequence. The development of the "autogen" process for the Mars 2001 Odyssey spacecraft is one implementation of this concept. It combines robust scheduling algorithms with software that is compatible with pre- existing "uplink" software, and literally reduced the duration of some sequence generation processes from weeks to minutes. This paper outlines the "autogen" tools and processes and describes how they have been implemented for the various phases of the Mars 2001 Odyssey mission. What is autogen? manually building the commands for lengthy and well- understood command sequences, efforts were made to The term "autogen" is applied in two different ways. develop software that would automatically schedule the First, "autogen," in its broadest sense, identifies a commands given certain input data. By taking the process that may be used to automatically generate knowledge for how commands were to be scheduled sequences for a spacecraft and, second, it is a Solaris and writing algorithms to replicate that knowledge, it script that has been used to facilitate this process. -
Chondrule-Like Material in Wild 2: a New Insight from Impact Experiments of Chondrule Fragments on Stardust Analogue Al Foil
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1925.pdf CHONDRULE-LIKE MATERIAL IN WILD 2: A NEW INSIGHT FROM IMPACT EXPERIMENTS OF CHONDRULE FRAGMENTS ON STARDUST ANALOGUE AL FOIL. M. Van Ginneken1 and P. J. Wozniakiewicz1, 1Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, United Kingdom ([email protected]; [email protected]) Introduction: NASA’s Stardust mission was the shape of craters depends mainly on the physical first mission to bring back to Earth material from a properties of the impactor [19]. Solid grains or dense celestial body, i.e. the Jupiter Family Comet (JFC) consolidated aggregates similar to chondrule fragments 81P/Wild 2 (hereafter Wild 2) [1]. Cometary dust was will result in bowl-shaped craters, the depth of which captured via impact into a collector that was deployed depending on the density of the material, whereas loose during a fly-by through the coma of Wild 2 at a relative aggregates of submicron particles result in complex speed of 6 km s-1. The collector consisted of silica features. Simulation of Stardust impacts using silicate aerogel secured into a metal frame by aluminum 1100 grains have shown that about 50% of silicate dominated foil (hereafter Al foil). A major result of the mission was impactors are retained as residue, which can be analysed the discovery that, contrary to expectations, Wild 2 was and provide precious chemical information [20]. not predominantly composed of presolar grains and low Studies of residues in a small (ø < 10 µm) or large temperature outer solar nebula material, but rather high (ø > 10 µm) craters on Stardust foil have shown that temperature (>>1000 °C) material typical of primitive these can give information on the bulk chemistry of the meteorites [1 - 3]. -
A Ballistics Analysis of the Deep Impact Ejecta Plume: Determining Comet Tempel 1’S Gravity, Mass, and Density
Icarus 190 (2007) 357–390 www.elsevier.com/locate/icarus A ballistics analysis of the Deep Impact ejecta plume: Determining Comet Tempel 1’s gravity, mass, and density James E. Richardson a,∗,H.JayMeloshb, Carey M. Lisse c, Brian Carcich d a Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA c Planetary Exploration Group, Space Department, Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA d Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA Received 31 March 2006; revised 8 August 2007 Available online 15 August 2007 Abstract − In July of 2005, the Deep Impact mission collided a 366 kg impactor with the nucleus of Comet 9P/Tempel 1, at a closing speed of 10.2 km s 1. In this work, we develop a first-order, three-dimensional, forward model of the ejecta plume behavior resulting from this cratering event, and then adjust the model parameters to match the flyby-spacecraft observations of the actual ejecta plume, image by image. This modeling exercise indicates Deep Impact to have been a reasonably “well-behaved” oblique impact, in which the impactor–spacecraft apparently struck a small, westward-facing slope of roughly 1/3–1/2 the size of the final crater produced (determined from initial ejecta plume geometry), and possessing an effective strength of not more than Y¯ = 1–10 kPa. The resulting ejecta plume followed well-established scaling relationships for cratering in a medium-to-high porosity target, consistent with a transient crater of not more than 85–140 m diameter, formed in not more than 250–550 s, for the case of Y¯ = 0 Pa (gravity-dominated cratering); and not less than 22–26 m diameter, formed in not less than 1–3 s, for the case of Y¯ = 10 kPa (strength-dominated cratering). -
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Enhanced Gravity Tractor Technique for Planetary Defense
4th IAA Planetary Defense Conference – PDC 2015 13-17 April 2015, Frascati, Roma, Italy IAA-PDC-15-04-11 ENHANCED GRAVITY TRACTOR TECHNIQUE FOR PLANETARY DEFENSE Daniel D. Mazanek(1), David M. Reeves(2), Joshua B. Hopkins(3), Darren W. Wade(4), Marco Tantardini(5), and Haijun Shen(6) (1)NASA Langley Research Center, Mail Stop 462, 1 North Dryden Street, Hampton, VA, 23681, USA, 1-757-864-1739, (2) NASA Langley Research Center, Mail Stop 462, 1 North Dryden Street, Hampton, VA, 23681, USA, 1-757-864-9256, (3)Lockheed Martin Space Systems Company, Mail Stop H3005, PO Box 179, Denver, CO 80201, USA, 1-303- 971-7928, (4)Lockheed Martin Space Systems Company, Mail Stop S8110, PO Box 179, Denver, CO 80201, USA, 1-303-977-4671, (5)Independent, via Tibaldi 5, Cremona, Italy, +393381003736, (6)Analytical Mechanics Associates, Inc., 21 Enterprise Parkway, Suite 300, Hampton, VA 23666, USA, 1-757-865-0000, Keywords: enhanced gravity tractor, in-situ mass augmentation, asteroid and comet deflection, planetary defense, low-thrust, high-efficiency propulsion, gravitational attraction, robotic mass collection Abstract Given sufficient warning time, Earth-impacting asteroids and comets can be deflected with a variety of different “slow push/pull” techniques. The gravity tractor is one technique that uses the gravitational attraction of a rendezvous spacecraft to the impactor and a low-thrust, high-efficiency propulsion system to provide a gradual velocity change and alter its trajectory. An innovation to this technique, known as the Enhanced Gravity Tractor (EGT), uses mass collected in-situ to augment the mass of the spacecraft, thereby greatly increasing the gravitational force between the objects.