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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. -
A La Torre Aaker Aalbers Aaldert Aarmour Aaron
A LA TORRE ABDIE ABLEMAN ABRAMOWITCH AAKER ABE ABLES ABRAMOWITZ AALBERS ABEE ABLETSON ABRAMOWSKY AALDERT ABEEL ABLETT ABRAMS AARMOUR ABEELS ABLEY ABRAMSEN AARON ABEKE ABLI ABRAMSKI AARONS ABEKEN ABLITT ABRAMSON AARONSON ABEKING ABLOTT ABRAMZON AASEN ABEL ABNER ABRASHKIN ABAD ABELA ABNETT ABRELL ABADAM ABELE ABNEY ABREU ABADIE ABELER ABORDEAN ABREY ABALOS ABELES ABORDENE ABRIANI ABARCA ABELI ABOT ABRIL ABATE ABELIN ABOTS ABRLI ABB ABELL ABOTSON ABRUZZO ABBA ABELLA ABOTT ABSALOM ABBARCROMBIE ABELLE ABOTTS ABSALON ABBAS ABELLS ABOTTSON ABSHALON ABBAT ABELMAN ABRAHAM ABSHER ABBATE ABELS ABRAHAMER ABSHIRE ABBATIELLO ABELSON ABRAHAMI ABSOLEM ABBATT ABEMA ABRAHAMIAN ABSOLOM ABBAY ABEN ABRAHAMOF ABSOLON ABBAYE ABENDROTH ABRAHAMOFF ABSON ABBAYS ABER ABRAHAMOV ABSTON ABBDIE ABERCROMBIE ABRAHAMOVITZ ABT ABBE ABERCROMBY ABRAHAMOWICZ ABTS ABBEKE ABERCRUMBIE ABRAHAMS ABURN ABBEL ABERCRUMBY ABRAHAMS ABY ABBELD ABERCRUMMY ABRAHAMSEN ABYRCRUMBIE ABBELL ABERDEAN ABRAHAMSOHN ABYRCRUMBY ABBELLS ABERDEEN ABRAHAMSON AC ABBELS ABERDEIN ABRAHAMSSON ACASTER ABBEMA ABERDENE ABRAHAMY ACCA ABBEN ABERG ABRAHM ACCARDI ABBERCROMBIE ABERLE ABRAHMOV ACCARDO ABBERCROMMIE ABERLI ABRAHMOVICI ACE ABBERCRUMBIE ABERLIN ABRAHMS ACERO ABBERDENE ABERNATHY ABRAHMSON ACESTER ABBERDINE ABERNETHY ABRAM ACETO ABBERLEY ABERT ABRAMCHIK ACEVEDO ABBETT ABEYTA ABRAMCIK ACEVES ABBEY ABHERCROMBIE ABRAMI ACHARD ABBIE ABHIRCROMBIE ABRAMIN ACHENBACH ABBING ABIRCOMBIE ABRAMINO ACHENSON ABBIRCROMBIE ABIRCROMBIE ABRAMO ACHERSON ABBIRCROMBY ABIRCROMBY ABRAMOF ACHESON ABBIRCRUMMY ABIRCROMMBIE ABRAMOFF -
Dust Coatings on Basaltic Rocks and Implications for Thermal Infrared Spectroscopy of Mars Jeffrey R
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. E6, 10.1029/2000JE001405, 2002 Dust coatings on basaltic rocks and implications for thermal infrared spectroscopy of Mars Jeffrey R. Johnson Branch of Astrogeology, U.S. Geological Survey, Flagstaff, Arizona, USA Philip R. Christensen Department of Geology, Arizona State University, Tempe, Arizona, USA Paul G. Lucey Hawaii Institute for Geology and Planetology, University of Hawaii at Manoa, Honolulu, Hawaii, USA Received 2 October 2000; revised 6 July 2001; accepted 12 October 2001; published 5 June 2002. [1] Thin coatings of atmospherically deposited dust can mask the spectral characteristics of underlying surfaces on Mars from the visible to thermal infrared wavelengths, making identification of substrate and coating mineralogy difficult from lander and orbiter spectrometer data. To study the spectral effects of dust coatings, we acquired thermal emission and hemispherical reflectance spectra (5–25 mm; 2000–400 cmÀ1) of basaltic andesite coated with different thicknesses of air fall-deposited palagonitic soils, fine-grained ceramic clay powders, and terrestrial loess. The results show that thin coatings (10–20 mm) reduce the spectral contrast of the rock substrate substantially, consistent with previous work. This contrast reduction continues linearly with increasing coating thickness until a ‘‘saturation thickness’’ is reached, after which little further change is observed. The saturation thickness of the spectrally flat palagonite coatings is 100–120 mm, whereas that for coatings with higher spectral contrast is only 50–75 mm. Spectral differences among coated and uncoated samples correlate with measured coating thicknesses in a quadratic manner, whereas correlations with estimated surface area coverage are better fit by linear functions. -
Global Spectral Classification of Martian Low-Albedo Regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) Data A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, E02004, doi:10.1029/2006JE002726, 2007 Global spectral classification of Martian low-albedo regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) data A. Deanne Rogers,1 Joshua L. Bandfield,2 and Philip R. Christensen2 Received 4 April 2006; revised 12 August 2006; accepted 13 September 2006; published 14 February 2007. [1] Martian low-albedo surfaces (defined here as surfaces with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) albedo values 0.15) were reexamined for regional variations in spectral response. Low-albedo regions exhibit spatially coherent variations in spectral character, which in this work are grouped into 11 representative spectral shapes. The use of these spectral shapes in modeling global surface emissivity results in refined distributions of previously determined global spectral unit types (Surface Types 1 and 2). Pure Type 2 surfaces are less extensive than previously thought, and are mostly confined to the northern lowlands. Regional-scale spectral variations are present within areas previously mapped as Surface Type 1 or as a mixture of the two surface types, suggesting variations in mineral abundance among basaltic units. For example, Syrtis Major, which was the Surface Type 1 type locality, is spectrally distinct from terrains that were also previously mapped as Type 1. A spectral difference also exists between southern and northern Acidalia Planitia, which may be due in part to a small amount of dust cover in southern Acidalia. Groups of these spectral shapes can be averaged to produce spectra that are similar to Surface Types 1 and 2, indicating that the originally derived surface types are representative of the average of all low-albedo regions. -
IUGG03-Program.Pdf
The Science Council of Japan and sixteen Japanese scientific societies will host IUGG2003, the XXIII General Assembly of the International Union of Geodesy and Geophysics. Hosts Science Council of Japan The Geodetic Society of Japan Seismological Society of Japan The Volcanological Society of Japan Meteorological Society of Japan Society of Geomagnetism and Earth, Planetary and Space Sciences Japan Society of Hydrology and Water Resources The Japanese Association of Hydrological Sciences The Japanese Society of Snow and Ice The Oceanographic Society of Japan The Japanese Society for Planetary Sciences The Japanese Society of Limnology Japan Society of Civil Engineers Japanese Association of Groundwater Hydrology The Balneological Society of Japan Japan Society of Erosion Control Engineering The Geochemical Society of Japan Special Support Hokkaido Prefecture City of Sapporo Co-Sponsor National Research Institute for Earth Science and Disaster Prevention (JSS01 Hagiwara Symposium on Monitoring and Modeling of Earthquake and Volcanic Processes for Prediction) Center for Climate System Research, University of Tokyo (JSM01 Toward High Resolution Climate Models and Earth System Models) Support Ministry of Education, Culture, Sports, Science and Technology Ministry of Economy, Trade and Industry Ministry of Land, Infrastructure and Transport Japan Marine Science and Technology Center National Institute of Advanced Industrial Science and Technology Japan Earth and Planetary Science Joint Meeting Organization Japanese Forestry Society Japan Business -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Fichier National Des Sites Classés
Ministère de la transition écologique et solidaire FICHIER NATIONAL DES SITES CLASSES ( mise à jour 29 décembre 2019) superficie (ha) A : arrêté Région dep commune nom DNP critère date territoire dpm total D : décret La tourbière de Malebronde située à Brenod, parcelle 9 Auvergne-Rhône- 1 Brenod TC A 30 avril 1934 0,2 0,2 Alpes section B Auvergne-Rhône- Alpes 1 Chaley La cascade de Charabotte, à Chaley A A 14 juin 1909 0,24 0,24 Auvergne-Rhône- Alpes 1 Charix Cascade du Moulin de Charix A A 14 juin 1909 0 0 L'ensemble formé par le lac Genin et ses abords situés Auvergne-Rhône- Alpes 1 Charix, Échallon, Oyonnax sur le territoire des communes de Charix, Échallon et TC A 1 mars 1935 50 50 Oyonnax Extension du site du Défilé de Fort l'Écluse sur les communes de Collonges et de Léaz (ne remplaçant pas Auvergne-Rhône- 1 Collonges, Léaz P D 19 mai 1992 1844 1844 Alpes l'arrêté du 6 novembre 1946 que pour la partie concernant la commune de Chevrier en Haute-Savoie) Auvergne-Rhône- Alpes 1 Corveissiat La grotte de Corveissiat A A 8 juin 1909 0 0 Auvergne-Rhône- Alpes 1 Courmangoux, Pressiat Le Mont Myon et ses abords à Courmangoux et Pressiat P A 10 avril 1946 46 46 La Pierre des Marais sur la commune de Divonne-les- Auvergne-Rhône- 1 Divonne-les-Bains A A 14 juin 1909 Alpes Bains L'ensemble formé sur la commune de Fareins par le site Auvergne-Rhône- 1 Fareins P D 1 mars 1982 78,49 78,49 Alpes des abords du château de Fléchères Fareins, Genouilleux, Guéreins, Lurcy, Messimy-sur-Saône, L'ensemble dit "Val de Saône" parmi les sites des Auvergne-Rhône- -
Elevation and Deformation Extraction from Tomosar
Title Elevation and Deformation Extraction from TomoSAR Lang Feng Thesis submitted for the degree of Doctor of Philosophy Mullard Space Science Laboratory Department of Space and Climate Physics University College London 2019 1 This page is intentionally left blank. 2 Author Declaration I, Lang Feng, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. LANG FENG 2019-02-01 3 This page is intentionally left blank. 4 Abstract 3D SAR tomography (TomoSAR) and 4D SAR differential tomography (Diff- TomoSAR) exploit multi-baseline SAR data stacks to provide an essential innovation of SAR Interferometry for many applications, sensing complex scenes with multiple scatterers mapped into the same SAR pixel cell. However, these are still influenced by DEM uncertainty, temporal decorrelation, orbital, tropospheric and ionospheric phase distortion and height blurring. In this thesis, these techniques are explored. As part of this exploration, the systematic procedures for DEM generation, DEM quality assessment, DEM quality improvement and DEM applications are first studied. Besides, this thesis focuses on the whole cycle of systematic methods for 3D & 4D TomoSAR imaging for height and deformation retrieval, from the problem formation phase, through the development of methods to testing on real SAR data. After DEM generation introduction from spaceborne bistatic InSAR (TanDEM- X) and airborne photogrammetry (Bluesky), a new DEM co-registration method with line feature validation (river network line, ridgeline, valley line, crater boundary feature and so on) is developed and demonstrated to assist the study of a wide area DEM data quality. -
Information to Users
RELATIVE AGES AND THE GEOLOGIC EVOLUTION OF MARTIAN TERRAIN UNITS (MARS, CRATERS). Item Type text; Dissertation-Reproduction (electronic) Authors BARLOW, NADINE GAIL. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 06/10/2021 23:02:22 Link to Item http://hdl.handle.net/10150/184013 INFORMATION TO USERS While the most advanced technology has been used to photograph and reproduce this manuscript, the quality of the reproduction is heavily dependent upon the quality of the material submitted. For example: • Manuscript pages may have indistinct print. In such cases, the best available copy has been filmed. o Manuscripts may not always be complete. In such cases, a note will indicate that it is not possible to obtain missing pages. • Copyrighted material may have been removed from the manuscript. In such cases, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, and charts) are photographed by sectioning the original, beginning at the upper left-hand corner and continuing from left to right in equal sections with small overlaps. Each oversize page is also filmed as one exposure and is available, for an additional charge, as a standard 35mm slide or as a 17"x 23" black and white photographic print. Most photographs reproduce acceptably on positive microfilm or microfiche but lack the clarity on xerographic copies made from the microfilm. -
Source Crater of HED Meteorites on Vesta and Impact Risk of Vestoids Meteoritics & Planetary Science 54, Nr 5, 953–1008 (2019) Doi: 10.1111/Maps.13258
The Sariçiçek howardite fall in Turkey: Source crater of HED meteorites on Vesta and impact risk of Vestoids Meteoritics & Planetary Science 54, Nr 5, 953–1008 (2019) doi: 10.1111/maps.13258 Ozan UNSALAN1,2, Peter JENNISKENS3,4, *, Qing-Zhu YIN5, Ersin KAYGISIZ1, Jim ALBERS3, David L. CLARK6, Mikael GRANVIK7, Iskender DEMIRKOL8, Ibrahim Y. ERDOGAN8, Aydin S. BENGU8, Mehmet E. ÖZEL9, Zahide TERZIOGLU10, Nayeob GI6, Peter BROWN6, Esref YALCINKAYA11, Tuğba TEMEL1, Dinesh K. PRABHU4,12, Darrel K. ROBERTSON4,13, Mark BOSLOUGH14, Daniel R. OSTROWSKI4,15, Jamie KIMBERLEY16, Selman ER11, Douglas J. ROWLAND5, Kathryn L. BRYSON4,15, Cisem ALTUNAYAR2, Bogdan RANGUELOV17, Alexander KARAMANOV17, Dragomir TATCHEV17, Özlem KOCAHAN18, Michael I. OSHTRAKH19, Alevtina A. MAKSIMOVA19, Maxim S. KARABANALOV19, Kenneth L. VEROSUB5, Emily LEVIN5, Ibrahim UYSAL20, Viktor HOFFMANN21,22, Takahiro HIROI23, Vishnu REDDY24, Gulce O. ILDIZ25, Olcay BOLUKBASI1, Michael E. ZOLENSKY26, Rupert HOCHLEITNER27, Melanie KALIWODA27, Sinan ÖNGEN11, Rui FAUSTO28, Bernardo A. NOGUEIRA28, Andrey V. CHUKIN19, Daniela KARASHANOVA29, Vladimir A. SEMIONKIN19, Mehmet YEŞILTAŞ30, Timothy GLOTCH30, Ayberk YILMAZ1, Jon M. FRIEDRICH31,32, Matthew E. SANBORN5, Magdalena HUYSKENS5, Karen ZIEGLER33, Curtis D. WILLIAMS5, Maria SCHÖNBÄCHLER34, Kerstin BAUER34, Matthias M. M. MEIER34, Colin MADEN34, Henner BUSEMANN34, Kees C. WELTEN35, Marc W. CAFFEE36, Matthias LAUBENSTEIN37, Qin ZHOU38, Qiu-Li LI39, Xian-Hua LI39, Yu LIU39, Guo-Qiang TANG39, Derek W. G. SEARS13,4, Hannah L. MCLAIN40, Jason P. DWORKIN41, Jamie E. ELSILA41, Daniel P. GLAVIN41, Philippe SCHMITT-KOPPLIN42,43, Alexander RUF42,43, Lucille LE CORRE24, & Nico SCHMEDEMANN44 (The Sariçiçek Meteorite Consortium) 1 University of Istanbul, 34134 Vezneciler, Fatih, Istanbul, Turkey. 2 Ege University, 35100 Bornova, Izmir, Turkey. 3 SETI Institute, Mountain View, CA 94043, USA. -
Adams Adkinson Aeschlimann Aisslinger Akkermann
BUSCAPRONTA www.buscapronta.com ARQUIVO 27 DE PESQUISAS GENEALÓGICAS 189 PÁGINAS – MÉDIA DE 60.800 SOBRENOMES/OCORRÊNCIA Para pesquisar, utilize a ferramenta EDITAR/LOCALIZAR do WORD. A cada vez que você clicar ENTER e aparecer o sobrenome pesquisado GRIFADO (FUNDO PRETO) corresponderá um endereço Internet correspondente que foi pesquisado por nossa equipe. Ao solicitar seus endereços de acesso Internet, informe o SOBRENOME PESQUISADO, o número do ARQUIVO BUSCAPRONTA DIV ou BUSCAPRONTA GEN correspondente e o número de vezes em que encontrou o SOBRENOME PESQUISADO. Número eventualmente existente à direita do sobrenome (e na mesma linha) indica número de pessoas com aquele sobrenome cujas informações genealógicas são apresentadas. O valor de cada endereço Internet solicitado está em nosso site www.buscapronta.com . Para dados especificamente de registros gerais pesquise nos arquivos BUSCAPRONTA DIV. ATENÇÃO: Quando pesquisar em nossos arquivos, ao digitar o sobrenome procurado, faça- o, sempre que julgar necessário, COM E SEM os acentos agudo, grave, circunflexo, crase, til e trema. Sobrenomes com (ç) cedilha, digite também somente com (c) ou com dois esses (ss). Sobrenomes com dois esses (ss), digite com somente um esse (s) e com (ç). (ZZ) digite, também (Z) e vice-versa. (LL) digite, também (L) e vice-versa. Van Wolfgang – pesquise Wolfgang (faça o mesmo com outros complementos: Van der, De la etc) Sobrenomes compostos ( Mendes Caldeira) pesquise separadamente: MENDES e depois CALDEIRA. Tendo dificuldade com caracter Ø HAMMERSHØY – pesquise HAMMERSH HØJBJERG – pesquise JBJERG BUSCAPRONTA não reproduz dados genealógicos das pessoas, sendo necessário acessar os documentos Internet correspondentes para obter tais dados e informações. DESEJAMOS PLENO SUCESSO EM SUA PESQUISA. -
Constraining Ceres' Interior from Its Rotational Motion
A&A 535, A43 (2011) Astronomy DOI: 10.1051/0004-6361/201116563 & c ESO 2011 Astrophysics Constraining Ceres’ interior from its rotational motion N. Rambaux1,2, J. Castillo-Rogez3, V. Dehant4, and P. Kuchynka2,3 1 Université Pierre et Marie Curie, UPMC–Paris 06, France e-mail: [nicolas.rambaux;kuchynka]@imcce.fr 2 IMCCE, Observatoire de Paris, CNRS UMR 8028, 77 avenue Denfert-Rochereau, 75014 Paris, France 3 Jet Propulsion Laboratory, Caltech, Pasadena, USA e-mail: [email protected] 4 Royal Observatory of Belgium, 3 avenue Circulaire, 1180 Brussels, Belgium Received 24 January 2011 / Accepted 14 July 2011 ABSTRACT Context. Ceres is the most massive body of the asteroid belt and contains about 25 wt.% (weight percent) of water. Understanding its thermal evolution and assessing its current state are major goals of the Dawn mission. Constraints on its internal structure can be inferred from various types of observations. In particular, detailed knowledge of the rotational motion can help constrain the mass distribution inside the body, which in turn can lead to information about its geophysical history. Aims. We investigate the signature of internal processes on Ceres rotational motion and discuss future measurements that can possibly be performed by the spacecraft Dawn and will help to constrain Ceres’ internal structure. Methods. We compute the polar motion, precession-nutation, and length-of-day variations. We estimate the amplitudes of the rigid and non-rigid responses for these various motions for models of Ceres’ interior constrained by shape data and surface properties. Results. As a general result, the amplitudes of oscillations in the rotation appear to be small, and their determination from spaceborne techniques will be challenging.