Oil Team Is Off to the Moon BULLETIN the Rocket and Spacecraft, Are to Detach the Fragile, Spi- You-Very Much
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Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
Identification of Volcanic Rootless Cones, Ice Mounds, and Impact 3 Craters on Earth and Mars: Using Spatial Distribution As a Remote 4 Sensing Tool
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, XXXXXX, doi:10.1029/2005JE002510, 2006 Click Here for Full Article 2 Identification of volcanic rootless cones, ice mounds, and impact 3 craters on Earth and Mars: Using spatial distribution as a remote 4 sensing tool 1 1 1 2 3 5 B. C. Bruno, S. A. Fagents, C. W. Hamilton, D. M. Burr, and S. M. Baloga 6 Received 16 June 2005; revised 29 March 2006; accepted 10 April 2006; published XX Month 2006. 7 [1] This study aims to quantify the spatial distribution of terrestrial volcanic rootless 8 cones and ice mounds for the purpose of identifying analogous Martian features. Using a 9 nearest neighbor (NN) methodology, we use the statistics R (ratio of the mean NN distance 10 to that expected from a random distribution) and c (a measure of departure from 11 randomness). We interpret R as a measure of clustering and as a diagnostic for 12 discriminating feature types. All terrestrial groups of rootless cones and ice mounds are 13 clustered (R: 0.51–0.94) relative to a random distribution. Applying this same 14 methodology to Martian feature fields of unknown origin similarly yields R of 0.57–0.93, 15 indicating that their spatial distributions are consistent with both ice mound or rootless 16 cone origins, but not impact craters. Each Martian impact crater group has R 1.00 (i.e., 17 the craters are spaced at least as far apart as expected at random). Similar degrees of 18 clustering preclude discrimination between rootless cones and ice mounds based solely on 19 R values. -
Geologic Map of Mars 1: 600 000 Gusev Crater Region M 600K 14.00S/175.50E G
Geologic Map of Mars 1: 600 000 Gusev Crater Region M 600k 14.00S/175.50E G GEOLOGIC UNITS 188°00’ West 187°30’ 187°00’ 186°30’ 186°00’ 185°30’ 185°00’ 184°30’ 184°00’ 183°30’ 183°00’ 182°30’ 182°00’ 181°30’ 181°00’ West 172°00’ East 172°30’ 173°00’ 173°30’ 174°00’ 174°30’ 175°00’ 175°30’ 176°00’ 176°30’ 177°00’ 177°30’ 178°00’ 178°30’ 179°00’ East -10°00’ -10°00’ Highlands -10°07’ A -10°07’ v Modified Gusev highland formation (MGHf) e r n Durius formation (Df) u -10°30’ -10°30’ s Gusev highland formation (GHf) -10°30’ R -10°30’ Himalaya formation (Hf) u p Lowlands e s A p o l l i n a r i s P a t e r a Suici formation (2) (Sf2) -11°00’ -11°00’ Suici formation (1) (Sf1) -11°00’ Zutphen Galdakao formation (ZGf) Death Valley formation (DVf) A p o l l i n a r i s S u l c i Bermuda formation (Bf) -11°30’ -11°30’ Z e p h y r i a M e n s a e -11°30’ -11°30’ Apollinaris formation (Af) Vaucouleurs formation-mesas (Vfm) Vaucouleurs formation (1) (Vf1) -12°00’ -12°00’ Vaucouleurs formation (2) (Vf2) -12°00’ -12°00’ Gusev Crater Gusev Crivitz formation (GCf) Ma'adim Vallis formation (MVf) -12°30’ -12°30’ Manhattan formation (Mf) -12°30’ -12°30’ Thira formation(Tf) Paris formation (Pf) -13°00’ -13°00’ Zandfoort formation (Zf) Gusev rim formation (Grf) -13°00’ -13°00’ Features G a l d a k a o Groove -13°30’ -1330’ Ridge -13°30’ Channel Crater rim d e V a u c o u l e u r s Degraded, buried crater rim -14°00’ -14°00’ Z u t p h e n Central peak of impact crater -14°00’ -14°00’ Landslide G u s e v Contacts Certain -14°30’ -14°30’ Approximate T h i r a -14°30’ -
Sundayiournal
STANDING STRONG FOR 1,459 DAYS — THE FIGHT'S NOT OVER YET JULY 11-17, 1999 THE DETROIT VOL. 4 NO. 34 75 CENTS S u n d a yIo u r n a l PUBLISHED BY LOCKED-OUT DETROIT NEWSPAPER WORKERS ©TDSJ JIM WEST/Special to the Journal Nicholle Murphy’s support for her grandmother, Teamster Meka Murphy, has been unflagging. Marching fourward Come Tuesday, it will be four yearsstrong and determined. In this editionOwens’ editorial points out the facthave shown up. We hope that we will since the day in July of 1995 that ofour the Sunday Journal, co-editor Susanthat the workers are in this strugglehave contracts before we have to put Detroit newspaper unions were forcedWatson muses on the times of happiuntil the end and we are not goingtogether any another anniversary edition. to go on strike. Although the companess and joy, in her Strike Diarywhere. on On Pages 19-22 we show offBut four years or 40, with your help, nies tried mightily, they never Pagedid 3. Starting on Page 4, we putmembers the in our annual Family Albumsolidarity and support, we will be here, break us. Four years after pickingevents up of the struggle on the record.and also give you a glimpse of somestanding of strong. our first picket signs, we remainOn Page 10, locked-out worker Keiththe far-flung places where lawn signs— Sunday Journal staff PAGE 10 JULY 11 1999 Co-editors:Susan Watson, Jim McFarlin --------------------- Managing Editor: Emily Everett General Manager: Tom Schram Published by Detroit Sunday Journal Inc. -
Distribution of Rocks on the Gusev Plains and on Husband Hill, Mars J
GEOPHYSICAL RESEARCH LETTERS, VOL. 33, L16202, doi:10.1029/2006GL026964, 2006 Click Here for Full Article Distribution of rocks on the Gusev Plains and on Husband Hill, Mars J. A. Grant,1 S. A. Wilson,1 S. W. Ruff,2 M. P. Golombek,3 and D. L. Koestler4 Received 19 May 2006; revised 12 July 2006; accepted 21 July 2006; published 29 August 2006. [1] The population of rocks larger than 15 cm in diameter al., 2000, Greeley et al., 2005], but perhaps Noachian) was measured at 36 locations imaged by the Spirit rover and of uncertain origin [Squyres et al., 2006; Arvidson et al., over 4 km of the traverse across the Gusev plains and 2006]. We examined the rock population of the surfaces at Husband Hill in Gusev crater on Mars. The rock population regular intervals along the traverse of the Spirit rover observed on plains surfaces is consistent with impact (Figure 1) to determine whether there was any significant fragmentation of rubbly/fractured volcanics and reveals variability among presumably different geomorphic surfa- little evidence for modification by secondary processes or ces that might reflect a fluvial/alluvial contribution to the weathering. Interpretation of counts from Husband Hill impact-derived blocks and/or modification by weathering or suggest an influence by bedrock for rocks larger than 0.5 m alternate geomorphic processes. across, but the distribution of smaller rocks is consistent with ejecta possessing contributions from pre-plains impact 2. Measuring the Rock Population events. Results indicate plains surfaces experienced only tens of centimeters of eolian erosion/deposition since the [4] The rock population was characterized by measuring Hesperian, whereas meters rather than tens of meters of the maximum visible axis of all rocks larger than 15 cm at erosion modified Husband Hill since the early Hesperian. -
Geologic Mapping of Gusev Crater, Mars: Gusev Rim and Floor Characteristics
Planetary Geologic Mappers 2021 (LPI Contrib. No. 2610) 7020.pdf GEOLOGIC MAPPING OF GUSEV CRATER, MARS: GUSEV RIM AND FLOOR CHARACTERISTICS. David A. Crown1, Frank C. Chuang1, James W. Rice1, Steven W. Ruff2, and Stephen P. Scheidt1,3,4, 1Planetary Science Institute, 1700 E. Ft. Lowell Rd., Suite 106, Tucson, AZ 85719 ([email protected]), 2Arizona State University, Tempe, AZ 85287, 3Howard University, Washington, DC 20059, 4Center for Research & Exploration in Space Science and Technology, Greenbelt, MD 20771. Introduction: The geologic complexity of Gusev the crater floor. crater (~160 km diameter; 14.53°S, 175.52°E) and its Gusev Crater Floor: Gusev floor materials have surroundings have been revealed through orbital been attributed to aeolian deposits overlying lava flows remote sensing coupled with in situ exploration of the [11]; mass-wasting and channel deposits [12]; fluvio- Columbia Hills and adjacent volcanic plains by the lacustrine deposits [6-7]; and basaltic lava flows [8, MER Spirit rover [e.g., 1-4]. Gusev crater’s geologic 13-15]. Although Spirit confirmed the presence of history has been attributed to the combined effects of a basalt, questions remain regarding the overall geologic variety of geologic processes that span much of evolution of Gusev. Martian history. We have initiated a new geologic Figure 1 shows our preliminary geologic map of mapping investigation of Gusev crater, designed to Gusev floor materials. Using 5-6 m/pixel CTX images, produce a 1:250K-scale, formal geologic map focused we have identified eight geologic units, including: two on the geologic evolution of the Gusev rim and floor ridged volcanic plains, Ma’adim debris flow, dissected (Figures 1-3). -
Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
Chapter Vi Report of Divisions, Commissions, and Working
CHAPTER VI REPORT OF DIVISIONS, COMMISSIONS, AND WORKING GROUPS Downloaded from https://www.cambridge.org/core. IP address: 170.106.33.42, on 24 Sep 2021 at 09:23:58, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0251107X00011937 DIVISION I FUNDAMENTAL ASTRONOMY Division I provides a focus for astronomers studying a wide range of problems related to fundamental physical phenomena such as time, the intertial reference frame, positions and proper motions of celestial objects, and precise dynamical computation of the motions of bodies in stellar or planetary systems in the Universe. PRESIDENT: P. Kenneth Seidelmann U.S. Naval Observatory, 3450 Massachusetts Ave NW Washington, DC 20392-5100, US Tel. + 1 202 762 1441 Fax. +1 202 762 1516 E-mail: [email protected] BOARD E.M. Standish President Commission 4 C. Froeschle President Commisison 7 H. Schwan President Commisison 8 D.D. McCarthy President Commisison 19 E. Schilbach President Commisison 24 T. Fukushima President Commisison 31 J. Kovalevsky Past President Division I PARTICIPATING COMMISSIONS: COMMISSION 4 EPHEMERIDES COMMISSION 7 CELESTIAL MECHANICS AND DYNAMICAL ASTRONOMY COMMISSION 8 POSITIONAL ASTRONOMY COMMISSION 19 ROTATION OF THE EARTH COMMISSION 24 PHOTOGRAPHIC ASTROMETRY COMMISSION 31 TIME Downloaded from https://www.cambridge.org/core. IP address: 170.106.33.42, on 24 Sep 2021 at 09:23:58, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0251107X00011937 COMMISSION 4: EPHEMERIDES President: H. Kinoshita Secretary: C.Y. Hohenkerk Commission 4 held one business meeting. -
APP Notes Programs
Blue iPods are 6th Generation, iOS 11.3 VR Resources Detailed List- TEACHERS Silver iPods are 5th Generation, iOS 9.1 updated 10/27/2017 APP Notes Operating Programs systems Bosch VR Paintings- Hieronymus Bosch iOS 8.0; Go inside the “Garden of Earthly Delights.” Android Note: the other paintings are fee-based. Brastours Ancient Rome tours iOS 8.0 or later; Tour ancient Rome- uses a map of Rome with icons to launch the Android VR. Includes the Forum, the Coliseum, Circus Maximus & Palatine Hill; Navigate using device, select VR mode at the locations. Cardboard Introductory VRs iOS 8.0 or later; Launch Cardboard demos. Includes: Android Tutorial Explorer- toggle through a series of 360 photospheres, Exhibit – toggle through a series of sculpted masks Urban Hike- toggle through 360 photospheres of major cities Kaleidoscope – colorful kaleidoscopic patterns Arctic Journey- Fly through the arctic like a bird. Cardboard Create your own 360 iOS 9.0 or later; Document your location in a 360 photosphere. photospheres. Android camera Discovery VR Many different VR shows iOS 9.1 or later; See Appendix A Available in 360 Android Eon Short, CG VRs, many with iOS 7.0 or later; Education Tab computer narration; Android Magi Chapel (voice okay) Some are available in 360. King Tut (computer voice) Neferititi (computer voice) Machu Picchu (computer voice) Edutainment tab: Egypt 360 Expeditions Teacher driven field trips. iOS 8.0 or later; Inclusive of many curricula; Available in 360. Android See Appendix B 1 Blue iPods are 6th Generation, iOS 11.3 VR Resources Detailed List- TEACHERS Silver iPods are 5th Generation, iOS 9.1 updated 10/27/2017 Google Street Works adequately in VR; iOS 9.0 or later; “Walk” through the streets of cities and towns around the View Works best in 360. -
Ebook < Impact Craters on Mars # Download
7QJ1F2HIVR # Impact craters on Mars « Doc Impact craters on Mars By - Reference Series Books LLC Mrz 2012, 2012. Taschenbuch. Book Condition: Neu. 254x192x10 mm. This item is printed on demand - Print on Demand Neuware - Source: Wikipedia. Pages: 50. Chapters: List of craters on Mars: A-L, List of craters on Mars: M-Z, Ross Crater, Hellas Planitia, Victoria, Endurance, Eberswalde, Eagle, Endeavour, Gusev, Mariner, Hale, Tooting, Zunil, Yuty, Miyamoto, Holden, Oudemans, Lyot, Becquerel, Aram Chaos, Nicholson, Columbus, Henry, Erebus, Schiaparelli, Jezero, Bonneville, Gale, Rampart crater, Ptolemaeus, Nereus, Zumba, Huygens, Moreux, Galle, Antoniadi, Vostok, Wislicenus, Penticton, Russell, Tikhonravov, Newton, Dinorwic, Airy-0, Mojave, Virrat, Vernal, Koga, Secchi, Pedestal crater, Beagle, List of catenae on Mars, Santa Maria, Denning, Caxias, Sripur, Llanesco, Tugaske, Heimdal, Nhill, Beer, Brashear Crater, Cassini, Mädler, Terby, Vishniac, Asimov, Emma Dean, Iazu, Lomonosov, Fram, Lowell, Ritchey, Dawes, Atlantis basin, Bouguer Crater, Hutton, Reuyl, Porter, Molesworth, Cerulli, Heinlein, Lockyer, Kepler, Kunowsky, Milankovic, Korolev, Canso, Herschel, Escalante, Proctor, Davies, Boeddicker, Flaugergues, Persbo, Crivitz, Saheki, Crommlin, Sibu, Bernard, Gold, Kinkora, Trouvelot, Orson Welles, Dromore, Philips, Tractus Catena, Lod, Bok, Stokes, Pickering, Eddie, Curie, Bonestell, Hartwig, Schaeberle, Bond, Pettit, Fesenkov, Púnsk, Dejnev, Maunder, Mohawk, Green, Tycho Brahe, Arandas, Pangboche, Arago, Semeykin, Pasteur, Rabe, Sagan, Thira, Gilbert, Arkhangelsky, Burroughs, Kaiser, Spallanzani, Galdakao, Baltisk, Bacolor, Timbuktu,... READ ONLINE [ 7.66 MB ] Reviews If you need to adding benefit, a must buy book. Better then never, though i am quite late in start reading this one. I discovered this publication from my i and dad advised this pdf to find out. -- Mrs. Glenda Rodriguez A brand new e-book with a new viewpoint. -
Meter-Scale Slopes of Candidate MER Landing Sites from Point Photoclinometry Ross A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. E12, 8085, doi:10.1029/2003JE002120, 2003 Meter-scale slopes of candidate MER landing sites from point photoclinometry Ross A. Beyer and Alfred S. McEwen Department of Planetary Sciences, University of Arizona, Tucson, Arizona, USA Randolph L. Kirk Astrogeology Team, U.S. Geological Survey, Flagstaff, Arizona, USA Received 13 May 2003; revised 16 July 2003; accepted 22 August 2003; published 4 December 2003. [1] Photoclinometry was used to analyze the small-scale roughness of areas that fall within the proposed Mars Exploration Rover (MER) 2003 landing ellipses. The landing ellipses presented in this study were those in Athabasca Valles, Elysium Planitia, Eos Chasma, Gusev Crater, Isidis Planitia, Melas Chasma, and Meridiani Planum. We were able to constrain surface slopes on length scales comparable to the image resolution (1.5 to 12 m/pixel). The MER 2003 mission has various engineering constraints that each candidate landing ellipse must satisfy. These constraints indicate that the statistical slope values at 5 m baselines are an important criterion. We used our technique to constrain maximum surface slopes across large swaths of each image, and built up slope statistics for the images in each landing ellipse. We are confident that all MER 2003 landing site ellipses in this study, with the exception of the Melas Chasma ellipse, are within the small-scale roughness constraints. Our results have provided input into the landing hazard assessment process. In addition to evaluating the safety of the landing sites, our mapping of small-scale roughnesses can also be used to better define and map morphologic units. -
Collection of Research Materials for the HBO Television Series, from the Earth to the Moon, 1940-1997, Bulk 1958-1997
http://oac.cdlib.org/findaid/ark:/13030/kt8290214d No online items Finding Aid for the Collection of Research Materials for the HBO Television Series, From the Earth to the Moon, 1940-1997, bulk 1958-1997 Processed by Manuscripts Division staff; machine-readable finding aid created by Caroline Cubé © 2004 The Regents of the University of California. All rights reserved. 561 1 Finding Aid for the Collection of Research Materials for the HBO Television Series, From the Earth to the Moon, 1940-1997, bulk 1958-1997 Collection number: 561 UCLA Library, Department of Special Collections Manuscripts Division Los Angeles, CA Processed by: Manuscripts Division staff, 2004 Encoded by: Caroline Cubé © 2004 The Regents of the University of California. All rights reserved. Descriptive Summary Title: Collection of Research Materials for the HBO Television Series, From the Earth to the Moon, Date (inclusive): 1940-1997, bulk 1958-1997 Collection number: 561 Creator: Home Box Office (Firm) Extent: 86 boxes (43 linear ft.) Repository: University of California, Los Angeles. Library. Dept. of Special Collections. Los Angeles, California 90095-1575 Abstract: From the earth to the moon was a Clavius Base/Imagine Entertainment production that followed the experiences of the Apollo astronauts in their mission to place a man on the moon. The collection covers a variety of subjects related to events and issues of the United States manned space flight program through Project Apollo and the history of the decades it covered, primarily the 1960s and the early 1970s. The collection contains books, magazines, unidentified excerpts from books and magazines, photographs, videorecordings, glass slides and audiotapes.