Asteroid Redirect Mission (ARM) Formulation Assessment and Support Team (FAST) Final Report Draft for Public Comment
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Wind-Eroded Stratigraphy on the Floor of a Noachian Impact Crater, Noachis Terra, Mars
Third Conference on Early Mars (2012) 7066.pdf WIND-ERODED STRATIGRAPHY ON THE FLOOR OF A NOACHIAN IMPACT CRATER, NOACHIS TERRA, MARS. R. P. Irwin III1,2, J. J. Wray3, T. A. Maxwell1, S. C. Mest2,4, and S. T. Hansen3, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, MRC 315, 6th St. at Independence Ave. SW, Washington DC 20013, [email protected], [email protected]. 2Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson AZ 85719, [email protected]. 3School of Earth and Atmospheric Sciences, Georgia Institute of Technology, 311 Ferst Drive, Atlanta GA 30332-0340, [email protected], [email protected]. 4Planetary Geodynamics Laboratory, Code 698, NASA Goddard Space Flight Center, Greenbelt MD 20771. Introduction: Detailed stratigraphic and spectral cular 12-km depression (a possible highly degraded studies of outcrops exposed in craters and other basins crater) on the southern side. The former received in- have significantly advanced the understanding of early ternal drainage from the north and east, whereas part Mars. Most studies have focused on high-relief sec- of the southern wall drained to the latter (Fig. 2). tions exposed by aeolian deflation, such as those in Gale crater, Arabia Terra, and Valles Marineris [1–3]. Many flat-floored Noachian degraded craters also have wind-eroded strata, suggesting that they lack a cap rock of Gusev-type basalts [4,5]. This study focuses on the youngest materials exposed on the wind-eroded floor of an unnamed Noachian degraded crater in Noachis Terra, Mars. The crater is centered at 20.2ºS, 42.6ºE and is 52 km in diameter. -
Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object
Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object by Nathan C. Shupe B.A., Swarthmore College, 2005 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirements for the degree of Master of Science Department of Aerospace Engineering Sciences 2010 This thesis entitled: Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object written by Nathan C. Shupe has been approved for the Department of Aerospace Engineering Sciences Daniel Scheeres Prof. George Born Assoc. Prof. Hanspeter Schaub Date The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. iii Shupe, Nathan C. (M.S., Aerospace Engineering Sciences) Orbit Options for an Orion-Class Spacecraft Mission to a Near-Earth Object Thesis directed by Prof. Daniel Scheeres Based on the recommendations of the Augustine Commission, President Obama has pro- posed a vision for U.S. human spaceflight in the post-Shuttle era which includes a manned mission to a Near-Earth Object (NEO). A 2006-2007 study commissioned by the Constellation Program Advanced Projects Office investigated the feasibility of sending a crewed Orion spacecraft to a NEO using different combinations of elements from the latest launch system architecture at that time. The study found a number of suitable mission targets in the database of known NEOs, and pre- dicted that the number of candidate NEOs will continue to increase as more advanced observatories come online and execute more detailed surveys of the NEO population. -
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 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. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
(101955) Bennu from OSIRIS-Rex Imaging and Thermal Analysis
ARTICLES https://doi.org/10.1038/s41550-019-0731-1 Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis D. N. DellaGiustina 1,26*, J. P. Emery 2,26*, D. R. Golish1, B. Rozitis3, C. A. Bennett1, K. N. Burke 1, R.-L. Ballouz 1, K. J. Becker 1, P. R. Christensen4, C. Y. Drouet d’Aubigny1, V. E. Hamilton 5, D. C. Reuter6, B. Rizk 1, A. A. Simon6, E. Asphaug1, J. L. Bandfield 7, O. S. Barnouin 8, M. A. Barucci 9, E. B. Bierhaus10, R. P. Binzel11, W. F. Bottke5, N. E. Bowles12, H. Campins13, B. C. Clark7, B. E. Clark14, H. C. Connolly Jr. 15, M. G. Daly 16, J. de Leon 17, M. Delbo’18, J. D. P. Deshapriya9, C. M. Elder19, S. Fornasier9, C. W. Hergenrother1, E. S. Howell1, E. R. Jawin20, H. H. Kaplan5, T. R. Kareta 1, L. Le Corre 21, J.-Y. Li21, J. Licandro17, L. F. Lim6, P. Michel 18, J. Molaro21, M. C. Nolan 1, M. Pajola 22, M. Popescu 17, J. L. Rizos Garcia 17, A. Ryan18, S. R. Schwartz 1, N. Shultz1, M. A. Siegler21, P. H. Smith1, E. Tatsumi23, C. A. Thomas24, K. J. Walsh 5, C. W. V. Wolner1, X.-D. Zou21, D. S. Lauretta 1 and The OSIRIS-REx Team25 Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the for- mation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo. -
Non-Principal Axis Rotation (Tumbling) Asteroids
NON-PRINCIPAL AXIS ROTATION (TUMBLING) ASTEROIDS Asteroid PAR Per1 Amp1 Per2 Amp2 Reference 244 Sita T0 129.51 0.82 0 129.51 0.82 Brinsfield, 09 253 Mathilde T 417.7 0.50 –3 417.7 0.45 250. Mottola, 95 –3 418. 0.5 250. Pravec, 05 288 Glauke T 1170. 0.9 –1 1200. 0.9 Harris, 99 0 Pravec, 14 –2 1170. 0.37 740. Pilcher, 15 299∗ Thora T– 272.9 0.50 0 274. 0.39 Pilcher, 14 +2 272.9 0.47 Pilcher, 17 319∗ Leona T 430. 0.5 –2 430. 0.5 1084. Pilcher, 17 341∗ California T 318. 0.92 –2 318. 0.9 250. Pilcher, 17 –2 317.0 0.54 Polakis, 17 –1 317.0 0.92 Polakis, 17 408 Fama T0 202.1 0.58 0 202.1 0.58 Stephens, 08 470 Kilia T0 290. 0.26 0 290. 0.26 Stephens, 09 0 Stephens, 09 496∗ Gryphia T 1072. 1.25 –2 1072. 1.25 Pilcher, 17 571 Dulcinea T 126.3 0.50 –2 126.3 0.50 Stephens, 11 630 Euphemia T0 350. 0.45 0 350. 0.45 Warner, 11 703∗ No¨emi T? 200. 0.78 –1 201.7 0.78 Noschese, 17 0 115.108 0.28 Sada, 17 –2 200. 0.62 Franco, 17 707 Ste¨ına T0 414. 1.00 0 Pravec, 14 763∗ Cupido T 151.5 0.45 –1 151.1 0.24 Polakis, 18 –2 151.5 0.45 101. Pilcher, 18 823 Sisigambis T0 146. -
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]. -
Impact Process of Boulders on the Surface of Asteroid 25143 Itokawa— Fragments from Collisional Disruption
Earth Planets Space, 60, 7–12, 2008 Impact process of boulders on the surface of asteroid 25143 Itokawa— fragments from collisional disruption A. M. Nakamura1, T. Michikami2, N. Hirata3, A. Fujiwara4, R. Nakamura5, M. Ishiguro6, H. Miyamoto7,8, H. Demura3, K. Hiraoka1, T. Honda1, C. Honda4, J. Saito9, T. Hashimoto4, and T. Kubota4 1Graduate School of Science, Kobe University, Kobe, 657-8501, Japan 2Fukushima National College of Technology, Iwaki, Fukushima 970-8034, Japan 3School of Computer Science and Engineering, University of Aizu, Aizuwakamatsu, Fukushima 965-8580, Japan 4Institute of Space and Astronautical Sciences (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 229-8510, Japan 5National Institute of Advanced Industrial Science and Technology, Tsukuba 306-8568, Japan 6Astronomy Department, Seoul National University, Seoul 151-747, Korea 7The University Museum, University of Tokyo, Tokyo 113-0033, Japan 8Planetary Science Institute, Tucson, AZ 85719, USA 9School of Engineering, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan (Received November 3, 2006; Revised March 29, 2007; Accepted April 11, 2007; Online published February 12, 2008) The subkilometer-size asteroid 25143 Itokawa is considered to have a gravitationally bounded rubble-pile structure. Boulders appearing in high-resolution images retrieved by the Hayabusa mission revealed the genuine outcome of the collisional event involving the asteroid’s parent body. Here we report that the boulders’ shapes and structures are strikingly similar to laboratory rock impact fragments despite differences of orders of magnitude in scale and complexities of the physical processes. These similarities suggest the universal character of the process throughout the range of these scales, and the brittle and structurally continuous nature regarding the parent body of the boulders. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Topography of Large Craters and Equatorial Bulge of 162173 Ryugu
EPSC Abstracts Vol. 13, EPSC-DPS2019-1723-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Topography of large craters and equatorial bulge of 162173 Ryugu Noriyuki Namiki (1,2), Takahide Mizuno (2,3), Hiroki Senshu (4), Hirotomo Noda (1,2), Koji Matsumoto (1,2), Naru Hirata (5), Ryuhei Yamada (5), Yoshiaki Ishihara (6), Hitoshi Ikeda (3), Hiroshi Araki (1,2), Keiko Yamamoto (1), Sinsuke Abe (7), Yousuke Masuda (7), Fumi Yoshida (4), Sho Sasaki (8), Shoko Oshigami (1), Makoto Shizugami (1), Arika Higuchi (1), Seiitsu Tsuruta (1), Kazuyoshi Asari (1), Toshimichi Otsubo (9), Naoyuki Hirata (10), Fuyuto Terui (3), Teiji Kase (11), Katsunori Mayuzumi (11), Sei-ichiro Watanabe (12), Takanao Saiki (3), Satoru Nakazawa (3), Makoto Yoshikawa (3), and Yuichi Tsuda (3) (1) National Astronomical Observatory of Japan, Japan, (2) SOKENDAI (The Graduate University for Advanced Studies), Japan, (3) Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, Japan, (4) Chiba Institute of Technology, Japan, (5) The University of Aizu, Japan, (6) National Institute of Advanced Industrial Science and Technology, Japan, (7) Nihon University, Japan, (8) Osaka University, Japan, (9) Hitotsubashi University, Japan, (10) Kobe University, Japan, (11) NEC Corporation, Japan, (12) Nagoya University, Japan ([email protected]) Abstract Lutetia, and Bennu which was recently visited by OSIRIS-REx spacecraft. Hayabusa2 Laser Altimeter (LIDAR) conducted two- dimensional scanning observation of the equatorial Ryugu is the second asteroid whose topography is band of asteroid, 162173 Ryugu on Oct. 30, 2018 to measured accurately by laser altimeter (LIDAR) [5] obtain detailed topography data. -
Near-Infrared Observations of Active Asteroid (3200) Phaethon Reveal No Evidence for Hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P
ARTICLE https://doi.org/10.1038/s41467-020-15637-7 OPEN Near-infrared observations of active asteroid (3200) Phaethon reveal no evidence for hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P. Emery3, Josef Hanuš 4, Vishnu Reddy2, Ellen S. Howell2, Andrew S. Rivkin5 & Tomoko Arai6 Asteroid (3200) Phaethon is an active near-Earth asteroid and the parent body of the Geminid Meteor Shower. Because of its small perihelion distance, Phaethon’s surface reaches 1234567890():,; temperatures sufficient to destabilize hydrated materials. We conducted rotationally resolved spectroscopic observations of this asteroid, mostly covering the northern hemisphere and the equatorial region, beyond 2.5-µm to search for evidence of hydration on its surface. Here we show that the observed part of Phaethon does not exhibit the 3-µm hydrated mineral absorption (within 2σ). These observations suggest that Phaethon’s modern activity is not due to volatile sublimation or devolatilization of phyllosilicates on its surface. It is possible that the observed part of Phaethon was originally hydrated and has since lost volatiles from its surface via dehydration, supporting its connection to the Pallas family, or it was formed from anhydrous material. 1 JETS/ARES, NASA Johnson Space Center, Houston, TX 77058-3696, USA. 2 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721- 0092, USA. 3 Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ 86011, USA. 4 Institute of Astronomy, Charles University, CZ-18000 Prague 8, Czech Republic. 5 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20273, USA. 6 Planetary Exploration Research Center, Chiba Institute of Technology, Narashino, Japan. -
An Orthoimage Map Using Data Obtained from the Mars Orbiter Camera of Mars Global Surveyor
An Orthoimage map using data obtained from the Mars Orbiter Camera of Mars Global Surveyor G. Niedermaier1,2, M. WŠhlisch1, F. Scholten1, F. Wewel1, Th. Roatsch1, R. Jaumann1, Th. Wintges2 (1 German Aerospace Center (DLR), Institute of Space Sensor Technology and Planetary Exploration, Berlin-Adlershof, 2University for Applied Sciences Munich (FHM), e-mail: [email protected]) Introduction. A basic requirement for the planning of future, perhaps even manned Mars missions are precise and high resolution maps of our neighbour planet and, especially, of the landing area. Here we present a new orthoimage map of Mars using data obtained from the Mars Orbiter Camera (MOC) of the Mars Global Surveyor (MGS). Since 1998, the National Aeronautics and Space Agency (NASA) uses the MGS for exploration and mapping of the global Martian surface. The new map covers the Mars surface from 0° to 180° West and from 60° South to 60° North, respectively, with a resolution of 231m/pixel. For map composing digital image processing methods have been used. Furthermore, we have succeeded to de- velop a processing method for composing image mosaics based on MOC data. This method may be used for composing image mosaics using CCD line camera data and is applicable also for other mars missions, whenever a CCD line camera is employed. Methods. Image data processing has been performed using multiple Video Image Commu- nication and Retrieval (VICAR) programs, developed by the Jet Propulsion Laboratory (JPL), DLR and the Technical University of Berlin (TUB), Department of Photogrammetry and Cartography. Also United States Geological Survey (USGS) Integrated Software for Imagers and Spectrometers (ISIS) programs were used.