Influence of Night Work on Performance During Lunar Telerobotic Operations
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Durham Research Online
Durham Research Online Deposited in DRO: 28 May 2020 Version of attached le: Accepted Version Peer-review status of attached le: Peer-reviewed Citation for published item: Halukeerthi, Siriney O. and Shephard, Jacob J. and Talewar, Sukhpreet K. and Evans, John S. O. and Rosu-Finsen, Alexander and Salzmann, Christoph G. (2020) 'Amorphous mixtures of ice and C60 fullerene.', Journal of physical chemistry A., 124 (24). pp. 5015-5022. Further information on publisher's website: https://doi.org/10.1021/acs.jpca.0c03439 Publisher's copyright statement: This document is the unedited Author's version of a Submitted Work that was subsequently accepted for publication in Journal of Physical Chemistry A, copyright c American Chemical Society after peer review. To access the nal edited and published work see https://doi.org/10.1021/acs.jpca.0c03439 Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full DRO policy for further details. Durham University Library, Stockton Road, Durham DH1 3LY, United Kingdom Tel : +44 (0)191 334 3042 | Fax : +44 (0)191 334 2971 https://dro.dur.ac.uk Subscriber access provided by UNIV OF DURHAM A: Environmental, Combustion, and Atmospheric Chemistry; Aerosol Processes, Geochemistry, and Astrochemistry Amorphous Mixtures of Ice and C60 Fullerene Siriney O. -
Minutes of the January 25, 2010, Meeting of the Board of Regents
MINUTES OF THE JANUARY 25, 2010, MEETING OF THE BOARD OF REGENTS ATTENDANCE This scheduled meeting of the Board of Regents was held on Monday, January 25, 2010, in the Regents’ Room of the Smithsonian Institution Castle. The meeting included morning, afternoon, and executive sessions. Board Chair Patricia Q. Stonesifer called the meeting to order at 8:31 a.m. Also present were: The Chief Justice 1 Sam Johnson 4 John W. McCarter Jr. Christopher J. Dodd Shirley Ann Jackson David M. Rubenstein France Córdova 2 Robert P. Kogod Roger W. Sant Phillip Frost 3 Doris Matsui Alan G. Spoon 1 Paul Neely, Smithsonian National Board Chair David Silfen, Regents’ Investment Committee Chair 2 Vice President Joseph R. Biden, Senators Thad Cochran and Patrick J. Leahy, and Representative Xavier Becerra were unable to attend the meeting. Also present were: G. Wayne Clough, Secretary John Yahner, Speechwriter to the Secretary Patricia L. Bartlett, Chief of Staff to the Jeffrey P. Minear, Counselor to the Chief Justice Secretary T.A. Hawks, Assistant to Senator Cochran Amy Chen, Chief Investment Officer Colin McGinnis, Assistant to Senator Dodd Virginia B. Clark, Director of External Affairs Kevin McDonald, Assistant to Senator Leahy Barbara Feininger, Senior Writer‐Editor for the Melody Gonzales, Assistant to Congressman Office of the Regents Becerra Grace L. Jaeger, Program Officer for the Office David Heil, Assistant to Congressman Johnson of the Regents Julie Eddy, Assistant to Congresswoman Matsui Richard Kurin, Under Secretary for History, Francisco Dallmeier, Head of the National Art, and Culture Zoological Park’s Center for Conservation John K. -
Cubex: a Compact X-Ray Telescope Enables Both X-Ray Fluorescence Imaging Spectroscopy and Pulsar Timing Based Navigation
SSC18-V-05 CubeX: A compact X-Ray Telescope Enables both X-Ray Fluorescence Imaging Spectroscopy and Pulsar Timing Based Navigation Jan Stupl, Monica Ebert, David Mauro SGT / NASA Ames NASA Ames Research Center, Moffett Field, CA; 650-604-4032 [email protected] JaeSub Hong Harvard University Cambridge, MA Suzanne Romaine, Almus Kenter, Janet Evans, Ralph Kraft Smithsonian Astrophysical Observatory Cambridge, MA Larry Nittler Carnegie Institution of Washington Washington, DC Ian Crawford Birkbeck College London, UK David Kring Lunar and Planetary Institute Houston, TX Noah Petro, Keith. Gendreau, Jason Mitchell, Luke Winternitz NASA Goddard Space Flight Center Greenbelt, MD Rebecca. Masterson, Gregory Prigozhin Massachusetts Institute of Technology Cambridge, MA Brittany Wickizer NASA Ames Research Center Moffett Field, CA Kellen Bonner, Ashley Clark, Arwen Dave, Andres Dono-Perez, Ali Kashani, Daniel Larrabee, Samuel Montez, Karolyn Ronzano, Tim Snyder MEI / NASA Ames Research Center Joel Mueting, Laura Plice Metis / NASA Ames Research Center NASA Ames Research Center, Moffett Field, CA Yueh-Liang Shen, Duy Nguyen Booz Allen Hamilton / NASA Ames NASA Ames Research Center, Moffett Field, CA Stupl 1 32nd Annual AIAA/USU Conference on Small Satellites ABSTRACT This paper describes the miniaturized X-ray telescope payload, CubeX, in the context of a lunar mission. The first part describes the payload in detail, the second part summarizes a small satellite mission concept that utilizes its compact form factor and performance. This instrument can be used for both X-ray fluorescence (XRF) imaging spectroscopy and X-ray pulsar timing-based navigation (XNAV). It combines high angular resolution (<1 arcminutes) Miniature Wolter-I X-ray optics (MiXO) with a common focal plane consisting of high spectral resolution (<150 eV at 1 keV) CMOS X-ray sensors and a high timing resolution (< 1 µsec) SDD X-ray sensor. -
A Compact X-Ray Telescope Enables Both X-Ray Fluorescence Imaging Spectroscopy and Pulsar Timing Based Navigation
CubeX: A compact X-Ray Telescope Enables both X-Ray Fluorescence Imaging Spectroscopy and Pulsar Timing Based Navigation Jan Stupl SGT / NASA Ames Research Center Jaesub Hong Harvard & the CubeX team 32nd Annual AIAA/USU Conference on Small Satellites – August 2018 1 2 Remote sensing XRF measurements provide insight into the geology of planetary bodies. 3 Can we navigate Deep Space autonomously? CubeX will also conduct semi-autonomous navigation by using precise time series from millisecond X-ray pulsars as “GPS” in our Galaxy. Competition Sensitive 4 X-ray Imaging Spectrometer (XIS) Terrain Camera LGA Battery X-band Radio Miniature X-ray Reaction Wheels Optics (MiXO) 50 cm focal length Solar X-ray Monitor (SXM) Propulsion Solar Panel System (0.4 m2) Star Tracker Focal plane of CMOS & SDD Thruster • ~6U CubeSat X-ray Telescope: 5.8 kg with 8.6W (S/C: ~40U) X-ray Imaging Spectrometer (XIS) and Solar X-ray Monitor (SXM) • XIS covers 0.4 – 7 keV with <150 eV FWHM @ 1 keV, 1 sq. deg FoV with < 1 arcmin Ang. Res.: 2 – 3 km resolution with 110 km foot print at 6000 km; < 1 µsec timing resolution for XNAV • SXM covers >130 deg FWZI with energy range of 1 – 8 keV 5 ~10 cm 34 NiCo shells Spider Fixture • Achieve <1 arcmin resolution (Al) over 1 sq. deg and 24 cm2 on- axis & 12 cm2 off-axis (@ 33 arcmin) effective area at 1 keV • 34 lightweight NiCo ENR shells (200 µm thick) in a butterfly design with 10 cm dia. x 8 cm length envelope (~1.5 kg) for 50 Cross-sectional view of 34 shells cm focal length Effective area (left) and angular resolution in HPD (right) as a function of off-axis for several discrete energies (color-coded) estimated by ray-tracing simulations. -
Chenangoforks2.Pdf
• Rilles – Lunar Rilles are long, narrow, depressions formed by lava flows, resembling channels. • Rugged Terra – Rugged terra are mountainous regions of the moon. • Wrinkle Ridges – Wrinkle Ridges are created through compression of tectonic plates within the maria. • Graben – Graben are formed from the stress of two fault lines. • Scarps – A displacement of land beside a fault. • Fault – A fault is a fracture on the surface. Grabens Rilles Scarps Fault Rugged Terra Wrinkle Ridge •Scarp‐ A type of fault. It is the displacement of land alongside a fault. • Mare Ridge‐ The raised edges of a mare impact basin. •Trough‐ A depression that is characterized by its shallow ridges • Lineament‐ A linear expression used to characterize a fault lined valley •The wrinkle ridge structures that deform and interrupt the mare basalts are commonly asymmetrical, with the steeper side bounded by a complex scarp composed of multiple overlapping lobate scarp segments that may have rounded crests that make them resemble mare ridges. •Lobate scarps are thrust faults that occur primarily in the Moon's lunar highlands. •a graben is a depressed block of land bordered by parallel faults. •Graben is German for ditch. •A graben is the result of a block of land being downthrown producing a valley with a distinct scarp on each side. •Graben often occur side-by-side with horsts. Horst and graben structures are indicative of tensional forces and crustal stretching. •Horsts are parallel blocks that remain between graben, the bounding faults of a horst typically dip away from the center line of the horst. •Also known as a Dark halo craterlets •Dark-halo craters are formed when an impact unearths lower albedo material from below the surface, then deposits this darker ejecta around the main crater. -
Complex Explosive Volcanic Activity on the Moon Within Oppenheimer Crater
Icarus 273 (2016) 296–314 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Complex explosive volcanic activity on the Moon within Oppenheimer crater ∗ Kristen A. Bennett a, ,BrionyH.N. Horgan b, Lisa R. Gaddis c, Benjamin T. Greenhagen d, Carlton C. Allen e,PaulO. Hayne f, James F. Bell III a, David A. Paige g a School of Earth and Space Exploration, Arizona State University. ISTB4 Room 795, 781 Terrace Mall, Tempe AZ 85287, United States b Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 550 Stadium Mall Drive, West Lafayette, IN 47907, United States c Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001, United States d Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, United States e NASA Johnson Space Center, Emeritus, 2101 NASA Road 1, Houston, TX 77058, United States f NASA Jet Propulsion Laboratory, 4800 Oak Grove Dr, Pasadena, CA 91109, United States g Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, 595 Charles E Young Dr E, Los Angeles, CA 90095, United States a r t i c l e i n f o a b s t r a c t Article history: Oppenheimer crater is a floor-fractured crater located within the South Pole–Aitken basin on the Moon, Received 27 July 2015 and exhibits more than a dozen localized pyroclastic deposits associated with the fractures. Localized Revised 10 December 2015 pyroclastic volcanism on the Moon is thought to form as a result of intermittently explosive Vulcanian Accepted 3 February 2016 eruptions under low effusion rates, in contrast to the higher-effusion rate, Hawaiian-style fire fountaining Available online 10 February 2016 inferred to form larger regional deposits. -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
Geologic Studies of Planetary Surfaces Using Radar Polarimetric Imaging 2
Geologic studies of planetary surfaces using radar polarimetric imaging 2 4 Lynn M. Carter NASA Goddard Space Flight Center 8 Donald B. Campbell 9 Cornell University 10 11 Bruce A. Campbell 12 Smithsonian Institution 13 14 14 Abstract: Radar is a useful remote sensing tool for studying planetary geology because it is 15 sensitive to the composition, structure, and roughness of the surface and can penetrate some 16 materials to reveal buried terrain. The Arecibo Observatory radar system transmits a single 17 sense of circular polarization, and both senses of circular polarization are received, which allows 18 for the construction of the Stokes polarization vector. From the Stokes vector, daughter products 19 such as the circular polarization ratio, the degree of linear polarization, and linear polarization 20 angle are obtained. Recent polarimetric imaging using Arecibo has included Venus and the 21 Moon. These observations can be compared to radar data for terrestrial surfaces to better 22 understand surface physical properties and regional geologic evolution. For example, 23 polarimetric radar studies of volcanic settings on Venus, the Moon and Earth display some 24 similarities, but also illustrate a variety of different emplacement and erosion mechanisms. 25 Polarimetric radar data provides important information about surface properties beyond what can 26 be obtained from single-polarization radar. Future observations using polarimetric synthetic 27 aperture radar will provide information on roughness, composition and stratigraphy that will 28 support a broader interpretation of surface evolution. 29 2 29 1.0 Introduction 30 31 Radar polarimetry has the potential to provide more information about surface physical 32 properties than single-polarization backscatter measurements, and has often been used in remote 33 sensing observations of Solar System objects. -
South Pole-Aitken Basin
Feasibility Assessment of All Science Concepts within South Pole-Aitken Basin INTRODUCTION While most of the NRC 2007 Science Concepts can be investigated across the Moon, this chapter will focus on specifically how they can be addressed in the South Pole-Aitken Basin (SPA). SPA is potentially the largest impact crater in the Solar System (Stuart-Alexander, 1978), and covers most of the central southern farside (see Fig. 8.1). SPA is both topographically and compositionally distinct from the rest of the Moon, as well as potentially being the oldest identifiable structure on the surface (e.g., Jolliff et al., 2003). Determining the age of SPA was explicitly cited by the National Research Council (2007) as their second priority out of 35 goals. A major finding of our study is that nearly all science goals can be addressed within SPA. As the lunar south pole has many engineering advantages over other locations (e.g., areas with enhanced illumination and little temperature variation, hydrogen deposits), it has been proposed as a site for a future human lunar outpost. If this were to be the case, SPA would be the closest major geologic feature, and thus the primary target for long-distance traverses from the outpost. Clark et al. (2008) described four long traverses from the center of SPA going to Olivine Hill (Pieters et al., 2001), Oppenheimer Basin, Mare Ingenii, and Schrödinger Basin, with a stop at the South Pole. This chapter will identify other potential sites for future exploration across SPA, highlighting sites with both great scientific potential and proximity to the lunar South Pole. -
Shoot the Moon – 1967
Video Transcript for Archival Research Catalog (ARC) Identifier 45011 Assignment: Shoot the Moon – 1967 Narrator: The assignment was specific: get photographs of the surface of the Moon that are good enough to determine whether or not it’s safe for a man to land there. But appearances can be deceiving, just as deceiving as trying to get a good picture of, well, a candy apple. Doesn’t seem to be too much of a problem, just set it up, light it, and snap the picture. Easy, quick, simple. But it can be tough. To begin with, the apple is some distance away, so you can’t get to it to just set it up, light it, and so on. To make things even more difficult, it isn’t even holding still; it’s moving around in circles. Now timing is important. You have to take your picture when the apple is nearest to you so you get the most detail and when the light that’s available is at the best angle for the photo. And even that’s not all. You are moving too, in circles. You’re both turning and circling about the apple. Now, about that assignment. As the technology of man in space was developing, it became more and more apparent that our knowledge of the Moon’s surface as a possible landing site was not sufficient. To land man safely on the Moon and get him safely off again, we had to know whether we could set up a precise enough trajectory to reach the Moon. -
15415 Ferroan Anorthosite 269.4 Grams “Don’T Lose Your Bag Now, Jim”
15415 Ferroan Anorthosite 269.4 grams “don’t lose your bag now, Jim” Figure 1: Photo of 15415 before processing. Cube is 1 inch. NASA# S71-44990 Transcript CDR Okay. Now let’s go down and get that unusual one. CDR Yes. We’ll get some of these. - - - No, let’s don’t mix Look at the little crater here, and the one that’s facing us. There is them – let’s make this a special one. I’ll zip it up. Make this bag this little white corner to the thing. What do you think the best 196, a special bag. Our first one. Don’t lose your bag now, Jim. way to sample it would be? O, boy. LMP I think probably – could we break off a piece of the clod underneath it? Or I guess you could probably lift that top fragment Transearth Coast Press Conference off. CC Q2: Near Spur Crater, you found what may be “Genesis CDR Yes. Let me try. Yes. Sure can. And it’s a white clast, Rock”, the oldest yet collected on the Moon. Tell us more about and it’s about – oh, boy! it. LMP Look at the – glint. Almost see twinning in there. CDR Well, I think the one you’re referring to was what we CDR Guess what we found? Guess what we just found? felt was almost entirely plagioclase or perhaps anorthosite. And it LMP I think we found what we came for. was a small fragment sitting on top of a dark brown larger fragment, CDR Crystal rock, huh? Yes, sir. -
Apollo 17 Lunar Sounder Data Provide Insight Into Aitken Crater’S Subsurface Structure
Lunar and Planetary Science XXXIX (2008) 2369.pdf APOLLO 17 LUNAR SOUNDER DATA PROVIDE INSIGHT INTO AITKEN CRATER’S SUBSURFACE STRUCTURE. B. L. Cooper1, 1Oceaneering Space Systems, 16665 Space Center Blvd., Houston TX 77058 (bon- [email protected]). Introduction: In preparation for the forthcoming chosen for high resolution rather than depth of pene- avalanche of data from LRO, we conducted a pilot tration. The ALSE data, although historically chal- study to demonstrate integration of multiple geophysi- lenging to interpret, offer unparalleled depth of pene- cal data sets. We applied methods of data integration tration. Work on restoring the ALSE data set was be- that are used by the commercial mineral exploration gun by [6]. This year, we plan to digitize the VHF industry to enhance the value of historical data sets (150 MHz) portion of the ALSE data, which has a and to provide a roadmap for future efforts. shorter wavelength than the HF-1 data, and thus pro- Background: For studies of the lunar near side and vides a bridge between the ALSE low-frequency data; polar regions, ground-based radar provides informa- future orbital radar data; and the nearside gound-based tion about texture and thickness of various geologic radar data that have been collected in the decades since units [1-4]. It is not possible to obtain ground-based Apollo. radar data for the far side. However, the Apollo Lunar Sounder Experiment (ALSE) data, which covers the orbital track of Apollo 17, can be used to obtain in- formation about the nature of the subsurface at Aitken crater and other farside locations.