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Planetary Geologic Mappers Annual Meeting
Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m. -
Optical Astronomy Catalogues, Coordinates Visible Objects on the Sky • Stars • Planets • Comets & Asteroids • Nebulae & Galaxies
Astrophysics Content: 2+2, 2×13×90 = 2 340 minutes = 39 hours Tutor: Martin Žáček [email protected] department of Physics, room 49 On-line informations: http://fyzika.feld.cvut.cz/~zacek/ … this presentation Many years (20?) teaching astrophysics (Prof. Petr Kulhanek), many texts and other materials but mostly in Czech (for example electronic journal Aldebaran Bulletin). 2011 … first year of teaching Astrophysics in English 2012-16 … 2017 … about 6 students, lextures on Thursday 11:00 lecture and 12:45 exercise https://www.fel.cvut.cz/cz/education/bk/predmety/12/77/p12773704.html ... AE0B02ASF https://www.fel.cvut.cz/cz/education/bk/predmety/12/78/p12784304.html ... AE0M02ASF Syllabus Classes: Astronomy & astrophysics 1. Astrophysics, history and its place in context of natural sciences. 2. Foundations of astronomy, history, its methods, instruments. 3. Solar system, inner and outer planets, Astronomical coordinates. Physics of stars 4. Statistics of stars, HR diagram. The star formation and evolution. Hyashi line. 5. Final evolutionary stages. White dwarfs, neutron stars, black holes. 6. Variable stars. Cepheids. Novae and supernovae stars. Binary systems. 7. Other galactic and extragalactic objects, nebulae, star clusters, galaxies. Cosmology 8. Principle of special and general theory of relativity. Relativistic experiments. 9. Cosmology. The Universe evolution, cosmological principle. Friedman models. 10. Supernovae Ia, cosmological parameters of the Universe, dark matter and dark energy. 11. Elementary particles, fundamental forces, quantum field theory, Feynman diagrams. 12. The origin of the Universe. Quark-gluon plasma. Nucleosynthesis. Microwave background radiation. 13. Cosmology with the inflationary phase, long-scale structure of the Universe. 14. Reserve Syllabus Practices: Astronomy & astrophysics 1. -
Back Matter (PDF)
Index Page numbers in italics refer to Tables or Figures Acasta gneiss 137, 138 Chladni, Ernst 94, 97 Adam, Robert 8, 11 chlorite 70, 71 agriculture, Hutton on 177 chloritoid stability 70 Albritton, Claude C. 100 Clerk Jnr, John 3 alumina (A1203), reaction in metamorphism 67-71 Clerk of Odin, John 5, 6, 7, 10, 11 andalusite stability 67 Clerk-Maxwell, George 10 anthropic principle 79-80 climate change 142 Apex basalt 140 Lyell on 97-8 Archean cratons (archons) 28, 31-2 coal as Earth heat source 176 Arizona Crater 98-9 coesite stability 65 Arran, Isle of 170 Columbia River basalts 32 asthenosphere 22 comets 89-90, 147-8 astrobleme 101 short v. long period 92 atmospheric composition 83-6 as source of life 148-9 Austral Volcanic Chain 24 continental flood basalt (CFB) 20, 23, 32 cordierite stability 67 craters, impact Bacon, Francis 21 Chixulub 109, 110, 143 Baldwin, Ralph 102 early ideas on 90, 98 Banks, Sir Joseph 96 modern occurrences 91, 98-101 Barringer, Daniel Moreau 99 Morokweng 142 Barringer Crater 99, 102, 103 modern research 102-3 basalt periodicity of 111-12 described by Hall 40-1 creation, Hutton's views on 76 mid-ocean ridge (MORB) 16-17, 20-1, 22, 23, 30-1 Creech, William 5 modern experiments on 44-7 Cretaceous-Tertiary impacts 141 ocean island (OIB) 20, 23 crust formation 17 see also flood basalt cryptoexplosion structures 101 Benares (India) meteorite shower 96 cryptovolcanic structures 100-1 Biot, Jean-Baptiste 97 Black, Joseph 4, 9, 10, 11, 42, 171 Boon, John D. -
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. -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Exploring Comets and Modeling for Mission Success
Exploring Comets and Modeling for Mission Success National Science Education Standards Alignment Created for Deep Impact, A NASA Discovery mission Maura Rountree-Brown and Art Hammon Educator-Enrichment Grades 5 – 8 Science as Inquiry Abilities necessary to do scientific inquiry − Identify questions that can be answered through scientific investigations. • Exploring Comets: Reflections on comets, missions and modeling − Develop descriptions, explanations, predictions, and models using evidence. • Make a Comet and Eat It!, Chemistry and Thermodynamics of Ice Cream, Comet on a Stick, Paper Comet with a Deep Impact, and Comet Models Based on the Deep Impact Mission − Think critically and logically to make the relationships between evidence and explanations. • Make a Comet and Eat It!, Comet on a Stick, Paper Comet with a Deep Impact, and Comet Models Based on the Deep Impact Mission − Communicate scientific procedures and explanations. • Make a Comet and Eat It! Understandings about scientific inquiry − Different kinds of questions suggest different kinds of scientific investigations. Some investigations involve observing and describing objects, or events; some involve experiments; some involve seeking more information; some involve discovery of new objects and phenomena; and some involve making models. • Make a Comet and Eat It!, Chemistry and Thermodynamics of Ice Cream, Comet on a Stick, Paper Comet with a Deep Impact, Comet Models Based on the Deep Impact Mission, and Deep Impact Comet Modeling − Current scientific knowledge and understanding guide scientific investigations. Different scientific domains employ different methods, core theories, and standards to advance scientific knowledge and understanding. • A Comet’s Place in the Solar System, Exploring Comets: Reflections on comets, missions and modeling, Deep Impact Comet Modeling, Deep Impact: Interesting Comet Facts, and Small Bodies Missions − Scientific explanations emphasize evidence, have logically consistent arguments, and use scientific principles, models, and theories. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
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. -
1 the Comets of Caroline Herschel (1750-1848)
Inspiration of Astronomical Phenomena, INSAP7, Bath, 2010 (www.insap.org) 1 publication: Culture and Cosmos, Vol. 16, nos. 1 and 2, 2012 The Comets of Caroline Herschel (1750-1848), Sleuth of the Skies at Slough Roberta J. M. Olson1 and Jay M. Pasachoff2 1The New-York Historical Society, New York, NY, USA 2Hopkins Observatory, Williams College, Williamstown, MA, USA Abstract. In this paper, we discuss the work on comets of Caroline Herschel, the first female comet-hunter. After leaving Bath for the environs of Windsor Castle and eventually Slough, she discovered at least eight comets, five of which were reported in the Philosophical Transactions of the Royal Society. We consider her public image, astronomers' perceptions of her contributions, and the style of her astronomical drawings that changed with the technological developments in astronomical illustration. 1. General Introduction and the Herschels at Bath Building on the research of Michael Hoskini and our book on comets and meteors in British art,ii we examine the comets of Caroline Herschel (1750-1848), the first female comet-hunter and the first salaried female astronomer (Figure 1), who was more famous for her work on nebulae. She and her brother William revolutionized the conception of the universe from a Newtonian one—i.e., mechanical with God as the great clockmaker watching over its movements—to a more modern view—i.e., evolutionary. Figure 1. Silhouette of Caroline Herschel, c. 1768, MS. Gunther 36, fol. 146r © By permission of the Oxford University Museum of the History of Science Inspiration of Astronomical Phenomena, INSAP7, Bath, 2010 (www.insap.org) 2 publication: Culture and Cosmos, Vol. -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Alexandre Amorim -.:: GEOCITIES.Ws
Alexandre Amorim (org) 2 3 PREFÁCIO O Boletim Observe! é uma iniciativa da Coordenação de Observação Astronômica do Núcleo de Estudo e Observação Astronômica “José Brazilício de Souza” (NEOA-JBS). Durante a reunião administrativa do NEOA-JBS em maio de 2010 foi apresentada a edição de Junho de 2010 para apreciação dos demais coordenadores do Núcleo onde houve aprovação unânime em usar o Boletim Observe! como veículo de informação das atividades e, principalmente, observações astronômicas. O Boletim Observe! é publicado mensalmente em formato eletrônico ou impresso separadamente, prezando pela simplicidade das informações e encorajando os leitores a observar, registrar e publicar os eventos astronômicos. Desde a sua primeira edição o Boletim Observe! conta com a colaboração espontânea de diversos astrônomos amadores e profissionais. Toda edição do Observe! do mês de dezembro é publicado um índice dos artigos do respectivo ano. Porém, desde aquela edição de Junho de 2010 foram publicados centenas de artigos e faz-se necessário consultar assuntos que foram tratados nas edições anteriores do Observe! e seus respectivos autores. Para isso publicaremos anualmente esse Índice de Assuntos, permitindo a consulta rápida dos temas abordados. Florianópolis, 1º de dezembro de 2018 Alexandre Amorim Coordenação de Observação Astronômica do NEOA-JBS 4 Ano I (2010) Nº 1 – Junho 2010 Eclipse da Lua em 26 de junho de 2010 Amorim, A. Júpiter sem a Banda Equatorial Sul Amorim, A. Conjunção entre Júpiter e Urano Amorim, A. Causos do Avelino Alves, A. A. Quem foi Eugênia de Bessa? Amorim, A. Nº 2 – Julho 2010 Aprendendo a dimensionar as distâncias angulares no céu Neves, M. -
Crater Geometry and Ejecta Thickness of the Martian Impact Crater Tooting
Meteoritics & Planetary Science 42, Nr 9, 1615–1625 (2007) Abstract available online at http://meteoritics.org Crater geometry and ejecta thickness of the Martian impact crater Tooting Peter J. MOUGINIS-MARK and Harold GARBEIL Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i, Honolulu, Hawai‘i 96822, USA (Received 25 October 2006; revision accepted 04 March 2007) Abstract–We use Mars Orbiter Laser Altimeter (MOLA) topographic data and Thermal Emission Imaging System (THEMIS) visible (VIS) images to study the cavity and the ejecta blanket of a very fresh Martian impact crater ~29 km in diameter, with the provisional International Astronomical Union (IAU) name Tooting crater. This crater is very young, as demonstrated by the large depth/ diameter ratio (0.065), impact melt preserved on the walls and floor, an extensive secondary crater field, and only 13 superposed impact craters (all 54 to 234 meters in diameter) on the ~8120 km2 ejecta blanket. Because the pre-impact terrain was essentially flat, we can measure the volume of the crater cavity and ejecta deposits. Tooting crater has a rim height that has >500 m variation around the rim crest and a very large central peak (1052 m high and >9 km wide). Crater cavity volume (i.e., volume below the pre-impact terrain) is ~380 km3 and the volume of materials above the pre-impact terrain is ~425 km3. The ejecta thickness is often very thin (<20 m) throughout much of the ejecta blanket. There is a pronounced asymmetry in the ejecta blanket, suggestive of an oblique impact, which has resulted in up to ~100 m of additional ejecta thickness being deposited down-range compared to the up-range value at the same radial distance from the rim crest.