Table 1: Classical Albedo Names from Ancient Geography
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MID-LATITUDE MARTIAN ICE AS a TARGET for HUMAN EXPLORATION, ASTROBIOLOGY, and IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A
First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1011.pdf MID-LATITUDE MARTIAN ICE AS A TARGET FOR HUMAN EXPLORATION, ASTROBIOLOGY, AND IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A. S. McEwen1, and C. M. Dundas2. 1University of Arizona, Department of Planetary Sciences, 2USGS, Astrogeology Science Center. Introduction: Future human missions to Mars will region of late Noachian highlands terrain, and is com- need to rely on resources available near the Martian prised of a series of grabens and ridges surrounded by surface. Water is of primary importance, and is known later Hesperian/Amazonian lava flows from the Thar- to be abundant on Mars in multiple forms, including sis region [7]. The proposed landing site is within these hydrated minerals [1] and pore-filling and excess ice lava flows (HAv), and provides access to a region of deposits [2]. Of these sources, excess ice (or ice which late Hesperian lowlands in the western region of the exceeds the available regolith pore space) may be the EZ. There is evidence for Amazonian glacial and peri- most promising for in-situ resource utilization (ISRU). glacial activity [e.g., HiRISE images Since Martian excess ice is thought to contain a low PSP_008671_2210 and ESP_017374_2210], and the fraction of dust and other contaminants (~<10% by Gamma Ray Spectrometer water map suggests that volume, [3]) only a modest deposit of excess ice will there is abundant subsurface ice in the uppermost me- be sufficient to support a human presence. ter within this region [10]. Meandering channel-like Subsurface water ice may also be of astrobiological features have been identified in HiRISE images (e.g., interest as a potential current habitat or as a preserva- PSP_003529_2195 in close proximity to apparent ice tion medium for biosignatures. -
Review of the MEPAG Report on Mars Special Regions
THE NATIONAL ACADEMIES PRESS This PDF is available at http://nap.edu/21816 SHARE Review of the MEPAG Report on Mars Special Regions DETAILS 80 pages | 8.5 x 11 | PAPERBACK ISBN 978-0-309-37904-5 | DOI 10.17226/21816 CONTRIBUTORS GET THIS BOOK Committee to Review the MEPAG Report on Mars Special Regions; Space Studies Board; Division on Engineering and Physical Sciences; National Academies of Sciences, Engineering, and Medicine; European Space Sciences Committee; FIND RELATED TITLES European Science Foundation Visit the National Academies Press at NAP.edu and login or register to get: – Access to free PDF downloads of thousands of scientific reports – 10% off the price of print titles – Email or social media notifications of new titles related to your interests – Special offers and discounts Distribution, posting, or copying of this PDF is strictly prohibited without written permission of the National Academies Press. (Request Permission) Unless otherwise indicated, all materials in this PDF are copyrighted by the National Academy of Sciences. Copyright © National Academy of Sciences. All rights reserved. Review of the MEPAG Report on Mars Special Regions Committee to Review the MEPAG Report on Mars Special Regions Space Studies Board Division on Engineering and Physical Sciences European Space Sciences Committee European Science Foundation Strasbourg, France Copyright National Academy of Sciences. All rights reserved. Review of the MEPAG Report on Mars Special Regions THE NATIONAL ACADEMIES PRESS 500 Fifth Street, NW Washington, DC 20001 This study is based on work supported by the Contract NNH11CD57B between the National Academy of Sciences and the National Aeronautics and Space Administration and work supported by the Contract RFP/IPL-PTM/PA/fg/306.2014 between the European Science Foundation and the European Space Agency. -
Workshop on the Martiannorthern Plains: Sedimentological,Periglacial, and Paleoclimaticevolution
NASA-CR-194831 19940015909 WORKSHOP ON THE MARTIANNORTHERN PLAINS: SEDIMENTOLOGICAL,PERIGLACIAL, AND PALEOCLIMATICEVOLUTION MSATT ..V",,2' :o_ MarsSurfaceandAtmosphereThroughTime Lunar and PlanetaryInstitute 3600 Bay AreaBoulevard Houston TX 77058-1113 ' _ LPI/TR--93-04Technical, Part 1 Report Number 93-04, Part 1 L • DISPLAY06/6/2 94N20382"£ ISSUE5 PAGE2088 CATEGORY91 RPT£:NASA-CR-194831NAS 1.26:194831LPI-TR-93-O4-PT-ICNT£:NASW-4574 93/00/00 29 PAGES UNCLASSIFIEDDOCUMENT UTTL:Workshopon the MartianNorthernPlains:Sedimentological,Periglacial, and PaleoclimaticEvolution TLSP:AbstractsOnly AUTH:A/KARGEL,JEFFREYS.; B/MOORE,JEFFREY; C/PARKER,TIMOTHY PAA: A/(GeologicalSurvey,Flagstaff,AZ.); B/(NationalAeronauticsand Space Administration.GoddardSpaceFlightCenter,Greenbelt,MD.); C/(Jet PropulsionLab.,CaliforniaInst.of Tech.,Pasadena.) PAT:A/ed.; B/ed.; C/ed. CORP:Lunarand PlanetaryInst.,Houston,TX. SAP: Avail:CASIHC A03/MFAOI CIO: UNITEDSTATES Workshopheld in Fairbanks,AK, 12-14Aug.1993;sponsored by MSATTStudyGroupandAlaskaUniv. MAJS:/*GLACIERS/_MARSSURFACE/*PLAINS/*PLANETARYGEOLOGY/*SEDIMENTS MINS:/ HYDROLOGICALCYCLE/ICE/MARS CRATERS/MORPHOLOGY/STRATIGRAPHY ANN: Papersthathavebeen acceptedforpresentationat the Workshopon the MartianNorthernPlains:Sedimentological,Periglacial,and Paleoclimatic Evolution,on 12-14Aug. 1993in Fairbanks,Alaskaare included.Topics coveredinclude:hydrologicalconsequencesof pondedwateron Mars; morpho!ogical and morphometric studies of impact cratersin the Northern Plainsof Mars; a wet-geology and cold-climateMarsmodel:punctuation -
Separating Fact from Fiction in the Aiolian Migration
hesperia yy (2008) SEPARATING FACT Pages399-430 FROM FICTION IN THE AIOLIAN MIGRATION ABSTRACT Iron Age settlementsin the northeastAegean are usuallyattributed to Aioliancolonists who journeyed across the Aegean from mainland Greece. This articlereviews the literary accounts of the migration and presentsthe relevantarchaeological evidence, with a focuson newmaterial from Troy. No onearea played a dominantrole in colonizing Aiolis, nor is sucha widespread colonizationsupported by the archaeologicalrecord. But the aggressive promotionof migrationaccounts after the PersianWars provedmutually beneficialto bothsides of theAegean and justified the composition of the Delian League. Scholarlyassessments of habitation in thenortheast Aegean during the EarlyIron Age are remarkably consistent: most settlements are attributed toAiolian colonists who had journeyed across the Aegean from Thessaly, Boiotia,Akhaia, or a combinationof all three.1There is no uniformityin theancient sources that deal with the migration, although Orestes and his descendantsare named as theleaders in mostaccounts, and are credited withfounding colonies over a broadgeographic area, including Lesbos, Tenedos,the western and southerncoasts of theTroad, and theregion betweenthe bays of Adramyttion and Smyrna(Fig. 1). In otherwords, mainlandGreece has repeatedly been viewed as theagent responsible for 1. TroyIV, pp. 147-148,248-249; appendixgradually developed into a Mountjoy,Holt Parker,Gabe Pizzorno, Berard1959; Cook 1962,pp. 25-29; magisterialstudy that is includedhere Allison Sterrett,John Wallrodt, Mal- 1973,pp. 360-363;Vanschoonwinkel as a companionarticle (Parker 2008). colm Wiener, and the anonymous 1991,pp. 405-421; Tenger 1999, It is our hope that readersinterested in reviewersfor Hesperia. Most of trie pp. 121-126;Boardman 1999, pp. 23- the Aiolian migrationwill read both articlewas writtenin the Burnham 33; Fisher2000, pp. -
Vertical Distribution of Dust in the Martian Atmosphere During Northern Spring and Summer: High‐Altitude Tropical Dust Maximum at Northern Summer Solstice N
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 116, E01007, doi:10.1029/2010JE003692, 2011 Vertical distribution of dust in the Martian atmosphere during northern spring and summer: High‐altitude tropical dust maximum at northern summer solstice N. G. Heavens,1,2 M. I. Richardson,3 A. Kleinböhl,4 D. M. Kass,4 D. J. McCleese,4 W. Abdou,4 J. L. Benson,4 J. T. Schofield,4 J. H. Shirley,4 and P. M. Wolkenberg4 Received 7 July 2010; revised 2 November 2010; accepted 12 November 2010; published 20 January 2011. [1] The vertical distribution of dust in Mars’ atmosphere is a critical unknown in the simulation of its general circulation and a source of insight into the lifting and transport of dust. Zonal average vertical profiles of dust opacity retrieved by Mars Climate Sounder show that the vertical dust distribution is mostly consistent with Mars general circulation model (GCM) simulations in southern spring and summer but not in northern spring and summer. Unlike the GCM simulations, the mass mixing ratio of dust has a maximum at 15– 25 km over the tropics during much of northern spring and summer: the high‐altitude tropical dust maximum (HATDM). The HATDM has significant and characteristic longitudinal variability, which it maintains for time scales on the order of or greater than those on which advection, sedimentation, and vertical eddy diffusion would act to eliminate both the longitudinal and vertical inhomogeneity of the distribution. While outflow from dust storms is able to produce enriched layers of dust at altitudes much greater than 25 km, tropical dust storm activity during the period in which the HATDM occurs is likely too rare to support the HATDM. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Bio-Preservation Potential of Sediment in Eberswalde Crater, Mars
Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Fall 2020 Bio-preservation Potential of Sediment in Eberswalde crater, Mars Cory Hughes Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Hughes, Cory, "Bio-preservation Potential of Sediment in Eberswalde crater, Mars" (2020). WWU Graduate School Collection. 992. https://cedar.wwu.edu/wwuet/992 This Masters Thesis is brought to you for free and open access by the WWU Graduate and Undergraduate Scholarship at Western CEDAR. It has been accepted for inclusion in WWU Graduate School Collection by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. Bio-preservation Potential of Sediment in Eberswalde crater, Mars By Cory M. Hughes Accepted in Partial Completion of the Requirements for the Degree Master of Science ADVISORY COMMITTEE Dr. Melissa Rice, Chair Dr. Charles Barnhart Dr. Brady Foreman Dr. Allison Pfeiffer GRADUATE SCHOOL David L. Patrick, Dean Master’s Thesis In presenting this thesis in partial fulfillment of the requirements for a master’s degree at Western Washington University, I grant to Western Washington University the non-exclusive royalty-free right to archive, reproduce, distribute, and display the thesis in any and all forms, including electronic format, via any digital library mechanisms maintained by WWU. I represent and warrant this is my original work, and does not infringe or violate any rights of others. I warrant that I have obtained written permissions from the owner of any third party copyrighted material included in these files. -
Dissertation Master
APOSTROPHE TO THE GODS IN OVID’S METAMORPHOSES, LUCAN’S PHARSALIA, AND STATIUS’ THEBAID By BRIAN SEBASTIAN A DISSERTATION PRESENTED TO THE GRADUATE SCHOOL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY UNIVERSITY OF FLORIDA 2013 1 © 2013 Brian Sebastian 2 To my students, for believing in me 3 ACKNOWLEDGMENTS A great many people over a great many years made this possible, more than I could possibly list here. I must first thank my wonderful, ideal dissertation committee chair, Dr. Victoria Pagán, for her sage advice, careful reading, and steadfast encouragement throughout this project. When I grow up, I hope I can become half the scholar she is. For their guidance and input, I also thank the members of my dissertation committee, Drs. Jennifer Rea, Robert Wagman, and Mary Watt. I am very lucky indeed to teach at the Seven Hills School, where the administration has given me generous financial support and where my colleagues and students have cheered me on at every point in this degree program. For putting up with all the hours, days, and weeks that I needed to be away from home in order to indulge this folly, I am endebted to my wife, Kari Olson. I am grateful for the best new friend that I made on this journey, Generosa Sangco-Jackson, who encouraged my enthusiasm for being a Gator and made feel like I was one of the cool kids whenever I was in Gainesville. I thank my parents, Ray and Cindy Sebastian, for without the work ethic they modeled for me, none of the success I have had in my academic life would have been possible. -
Water and Lava Both Seem Viable for the Formation of One of Mars' Densest and Largest Channel Networks
EPSC Abstracts Vol. 14, EPSC2020-19, 2020 https://doi.org/10.5194/epsc2020-19 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Water and lava both seem viable for the formation of one of Mars' densest and largest channel networks Hannes Bernhardt and David A. Williams Arizona State University, School of Earth and Space Exploration, Tempe, United States of America ([email protected]) The Axius Valles on the Malea Planum region’s (MPR) northern flank down into the Hellas basin are one of the most extensive and densest channel networks on Mars [1,2]. While previous studies tentatively interpreted the area as pyroclastic deposits dissected by sapped water/lahar flows [3-8] we considered their viability versus low-viscosity lava flows. Physiography The Axius Valles and adjacent channels to the west consist of ~22,550 km of mostly parallel sinuous valleys dissecting a plain (drainage density of 0.09 km-1) of gentle but relatively uniform northnortheast tilt, i.e., long-wavelength dip, at ~0.6 to 0.9° (~1 to 1.6%) towards the Hellas basin floor. The channels are up to ~20 km wide and ~100 m deep, although most are narrower and shallower than ~5 km and ~50 m, respectively. The majority of the valleys originates around the rim of Amphitrites Patera between elevations of ~1,200 and ~1,600 m. Smaller subsets originate at or below the rim of Peneus Patera between elevations of ~0 m and ~600 m, or are traceable further south into the wrinkle-ridged plains of the MPR. -
A PRELIMINARY STUDY. MA De Pa
Lunar and Planetary Science XXXIII (2002) 1032.pdf DESCRIPTION, ORIGIN AND EVOLUTION OF A BASIN IN SIRENUM TERRAE, MARS, INCLUDING ATLANTIS CHAOS: A PRELIMINARY STUDY. M. A. de Pablo and M. Druet. Seminar on Planetary Sciences. Fac- ultad de Ciencias Geológicas. Universidad Complutense de Madrid. 28040 Madrid. Spain. [email protected]. INTRODUCTION The volcanic activity of the area is reflected Atlantis is the name proposed in this pre- in the presence of two volcanic constructs. The first liminary study for the basin where (at 35ºS, 177ºW) one, fissural in character, closes the basin by its NE the chaotic terrain Atlantis Chaos is located. We pro- edge. The second one, an ancient massive volcanic pose that this basin harbored a lake during one of the building, is located at the SSW. These two constructs ‘humid Mars’ epochs [1, 2]. The main evidences for have already been portrayed in some thematic maps this hypothesis are the circular morphology, the bor- [4]. dering fracture and ridge systems, the volcanic con- The center of Atlantis is occupied by a cha- structs, and a variety of erosive and sedimentary otic terrain that gives its name to the basin. The chaos landforms associated. Cross-cutting relationship of is extensively eroded, and partially covered by detritic these features permits the partial reconstruction of the sediments which cover the whole basin area, as well history of this basin, which could be one of the few as an impact crater located in it. These epiclastic lay- such basins not clearly housed in an impact crater. ers are probably related with the run-off areas that cover most of the North, South and East edges of the METHODOLOGY basin. -
UNIVERSITY of PENNSYLVANIA Two Hundred Thirty-Fifth Commencement for the Conferring of Degrees
UNIVERSITY of PENNSYLVANIA Two Hundred Thirty-Fifth Commencement for the Conferring of Degrees FRANKLIN FIELD Tuesday, May 21, 1991 SEATING DIAGRAM Guests will find this diagram helpful in locating the approximate seating of the degree candidates. The seating roughly corresponds to the order by school in which the candidates for degrees are presented, beginning at top left with the College of Arts and Sciences. The actual sequence is shown in the Contents on the opposite page under Degrees in Course. Reference to the paragraph on page seven describing the colors of the candidates' hoods according to their fields of study may further assist guests in placing the locations of the various schools. STAGE Graduate Faculty Faculty Faculties Engineering Nursing Medicin College College Wharton Dentaline Arts Dental Medicine Veterinary Medicine Wharton Education Graduate Social Work Annenberg Contents Page Seating Diagram of the Graduating Students . 2 The Commencement Ceremony .. 4 Commencement Notes .. 6 Degrees in Course . 8 The College of Arts and Sciences .. 8 The College of General Studies . 17 The School of Engineering and Applied Science .. 18 The Wharton School .. 26 The Wharton Evening School .. 30 The Wharton Graduate Division .. 32 The School of Nursing .. 37 The School of Medicine .. 39 The Law School .. 40 The Graduate School of Fine Arts .. 42 The School of Dental Medicine .. 45 The School of Veterinary Medicine .. 46 The Graduate School of Education .. 47 The School of Social Work .. 49 The Annenberg School for Communication .. 50 The Graduate Faculties .. 51 Certificates .. 57 General Honors Program .. 57 Advanced Dental Education .. 57 Education .. 58 Fine Arts .. 58 Commissions . -
Modeling the Development of Martian Sublimation Thermokarst Landforms
Icarus 262 (2015) 154–169 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Modeling the development of martian sublimation thermokarst landforms a, b b Colin M. Dundas ⇑, Shane Byrne , Alfred S. McEwen a Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA article info abstract Article history: Sublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsur- Received 8 August 2014 face. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the mid- Revised 17 June 2015 latitudes and considered likely thermokarst features. We describe a landscape evolution model that cou- Accepted 29 July 2015 ples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens of thou- Available online 21 August 2015 sands of Mars years under conditions similar to the present, the model produces scallop-like features similar to those on the martian surface, starting from much smaller initial disturbances. The model also Keywords: indicates crater expansion when impacts occur in surfaces underlain by excess ice to some depth, with Mars, surface morphologies similar to observed landforms on the martian northern plains. In order to produce these Geological processes Mars, climate landforms by sublimation, substantial quantities of excess ice are required, at least comparable to the vertical extent of the landform, and such ice must remain in adjacent terrain to support the non- deflated surface. We suggest that martian thermokarst features are consistent with formation by subli- mation, without melting, and that significant thicknesses of very clean excess ice (up to many tens of meters, the depth of some scalloped depressions) are locally present in the martian mid-latitudes.