The Faint Young Sun Problem Revisited SCIENCE EDITOR GSA Is Soliciting Applications for Three Science Co-Editors for the Journal Geology
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INFORMATION TO USERS This manuscript has bean raproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event tfiat tfie author did not send UMI a complete manuscript and there are missing pages, these wilt be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Photographs included in the original manuscript have been reproduced xerographically in this copy. Higher quality 6* x 9* black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. Bell & Howell Infbrmation and Learning 300 North Zeab Road. Ann Arbor. Ml 48106-1346 USA 800-521-0600 u m t NOTE TO USERS This reproduction Is the best copy available. UMI UNIVERSITY OF OKLAHOMA GRADUATE COLLEGE THE GEOARCHAEOLOGY OF DAY CREEK CHERT: LITHOSTRATIGRAFHY, PETROLOGY, AND THE INDIGENOUS LANDSCAPE OF NORTHWEST OKLAHOMA AND SOUTHWEST KANSAS A Dissertation SUBMITTED TO THE GRADUATE FACULTY in partial fulfilment of the requirements for the degree of Doctor of Philosophy By BERKLEY BARNETT BAILEY Norman, Oklahoma 200 0 UMI Number 9975805 UMI* UMI MiCFOform9975805 Copyright 2000 by Bell & Howell Information and Learning Company. -
MARS DURING the PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- Boratory, University of Arizona
Fourth Conference on Early Mars 2017 (LPI Contrib. No. 2014) 3078.pdf MARS DURING THE PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- boratory, University of Arizona, Tucson, AZ 85721, [email protected], 2Southwest Research Institute and NASA’s SSERVI-ISET team, 1050 Walnut St., Suite 300, Boulder, CO 80302. Introduction: The surface geology of Mars appar- ing the pre-Noachian was ~10% of that during the ently dates back to the beginning of the Early Noachi- LHB. Consideration of the sawtooth-shaped exponen- an, at ~4.1 Ga, leaving ~400 Myr of Mars’ earliest tially declining impact fluxes both in the aftermath of evolution effectively unconstrained [1]. However, an planet formation and during the Late Heavy Bom- enduring record of the earlier pre-Noachian conditions bardment [5] suggests that the impact flux during persists in geophysical and mineralogical data. We use much of the pre-Noachian was even lower than indi- geophysical evidence, primarily in the form of the cated above. This bombardment history is consistent preservation of the crustal dichotomy boundary, to- with a late heavy bombardment (LHB) of the inner gether with mineralogical evidence in order to infer the Solar System [6] during which HUIA formed, which prevailing surface conditions during the pre-Noachian. followed the planet formation era impacts during The emerging picture is a pre-Noachian Mars that was which the dichotomy formed. less dynamic than Noachian Mars in terms of impacts, Pre-Noachian Tectonism and Volcanism: The geodynamics, and hydrology. crust within each of the southern highlands and north- Pre-Noachian Impacts: We define the pre- ern lowlands is remarkably uniform in thickness, aside Noachian as the time period bounded by two impacts – from regions in which it has been thickened by volcan- the dichotomy-forming impact and the Hellas-forming ism (e.g., Tharsis, Elysium) or thinned by impacts impact. -
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. -
Pioneering the Red Planet
RVD NASA PIONEERING THE RED PLANET Adventures on Martian soil Mars has always obsessed humankind - the Red planet, the ‘New Earth’. And with the recent successful landing of NASA’s Curiosity rover, Mars is closer than ever. Ever since 1960, we have actively been sending probes and rovers to observe the planet, but not without defeat. The road to the red planet is long, and the landing is rough. And since we do not have the technology yet to bring pieces of Mars to our laboratories, we’ll have to bring the laboratories to Mars. TEXT Ivo van der Peijl and Marijn Veraart, Students Aerospace Engineering, President and Treasurer of the 27th Space Department. THE EARLY DAYS ther attempts, the Mars 4 through 7, were velocity of 1cm/s. The main task of the rov- Between October 10, 1960 and 1967, six all partially successful. They all gathered er was to examine rocks nearby the land- Mars missions were undertaken, ! ve by some data, but none of them were able to ing site. Equipped with an Alpha Particle the USSR and one by USA. This was maybe either enter the intended orbit, or make a X-ray Spectrometer (APXS), the composi- too ambitious for the early days, because successful landing. tion of rocks could be determined. two failed to reach earth orbit, two failed It was NASA who had the next success. The oldest Mars-related spacecraft that is to leave it and two had problems en route. The Viking 1 landed on the Martian sur- still in use today is the 2001 Mars Odys- It was December 20, 1967 when the Mari- face July 20, 1976, shortly followed by the sey. -
Obituary "C" Index
Obituary "C" Index Copyright © 2004 - 2021 GRHS DISCLAIMER: GRHS cannot guarantee that should you purchase a copy of what you would expect to be an obituary from its obituary collection that you will receive an obituary per se. The obituary collection consists of such items as a) personal cards of information shared with GRHS by researchers, b) www.findagrave.com extractions, c) funeral home cards, d) newspaper death notices, and e) obituaries extracted from newspapers and other publications as well as funeral home web sites. Some obituaries are translations of obituaries published in German publications, although generally GRHS has copies of the German versions. These German versions would have to be ordered separately for they are kept in a separate file in the GRHS library. The list of names and dates contained herein is an alphabetical listing [by surname and given name] of the obituaries held at the Society's headquarters for the letter combination indicated. Each name is followed by the birth date in the first column and death date in the second. Dates may be extrapolated or provided from another source. Important note about UMLAUTS: Surnames in this index have been entered by our volunteers exactly as they appear in each obituary but the use of characters with umlauts in obits has been found to be inconsistant. For example the surname Büchele may be entered as Buchele or Bahmüller as Bahmueller. This is important because surnames with umlauted characters are placed in alphabetic order after regular characters so if you are just scrolling down this sorted list you may find the surname you are looking for in an unexpected place (i.e. -
Conference Program
Conference Program 24th WRMISS Conference Program: Tuesday 3rd September 2019 08.30 – 09:00 Registration 09.00 – 10:00 Opening 10.00 – 10:30 Scientific Session 1 10.30 – 11.30 Coffee/Tea Break 11.30 – 13:00 Scientific Session 2 13:00 – 14:00 Lunch 14.00 – 15:30 Scientific Session 3 15.30 – 16:30 Coffee/Tea Break 16:30 – 18.15 Scientific Session 4 Major of Athens, Ministry of Ministry of digital policy Ministry of Ministry of Development and Investment Opening speeches President of Hellenic Space Center Greek ESA‐ representative NASA Radiation Health Officer: Edward Semones Guenther Reitz, Marianthi Fragopoulou Welcome and Organisational Issues Scientific Session 1 Reviewing ISS‐member cancer and non‐cancer risk models and their Samy El‐Jaby differences for exploration class missions Scientific Session 2 Xiaojing Xu Validation of Trapped Proton Environments with EFT‐1 Measurements Solar Modulation, Forbush decreases and Solar Particle Events by AMS Claudio Cordi onboard ISS Validation of NASA’s Radiation Analysis Tools with ISS Radiation Martha Clowdsley Environment (REM) Measurements Scientific Session 3 Pawel Bilski Fluorescent Nuclear Track detectors based on LiF single crystals Lawrence Pinsky The Timepix 2 from the Medipix 2 Collaboration – First results The AMS‐02 experiment as a cosmic ray flux and radiation monitor on the Valerie Formato ISS Scientific Session 4 GCR flux and dose rates variations observed experimentally by 13 Liulin Tsvetan Dachev Type instruments between 1991 and 2019 Attila Hirn Pille Measurements on ISS (February -
Volcanism on Mars
Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny. -
Item 7, Appeal No. 20-042 @ 2900 25Th Street.Pdf
BOARD OF APPEALS, CITY & COUNTY OF SAN FRANCISCO Appeal of Appeal No. 20-042 RICHARD SEGOVIA, ) Appellant(s) ) ) vs. ) ) SAN FRANCISCO PUBLIC WORKS, ) BUREAU OF STREET USE & MAPPING, ) Respondent NOTICE OF APPEAL NOTICE IS HEREBY GIVEN THAT on June 19, 2020, the above named appellant(s) filed an appeal with the Board of Appeals of the City and County of San Francisco from the decision or order of the above named department(s), commission, or officer. The substance or effect of the decision or order appealed from is the ISSUANCE on June 18, 2020 to Extenet Systems LLC, of a Wireless Box Permit (installation of Personal Wireless Service Facility in a Zoning Protected location) at 2900 25th Street. APPLICATION NO. 18WR-0369 FOR HEARING ON July 29, 2020 Address of Appellant(s): Address of Other Parties: Richard Segovia, Appellant(s) Extenet Systems LLC, Determination Holder(s) 2880 25th Street c/o Joseph Camicia, Agent for Determination Holder(s) San Francisco, CA 94110 2000 Crow Canyon Place #210 San Ramon, CA 94582 c/o Rick Hirsch, Agent for Determination Holder(s) 5957 Keith Ave. Oakland, CA 94618 Date Filed: June 19, 2020 CITY & COUNTY OF SAN FRANCISCO BOARD OF APPEALS PRELIMINARY STATEMENT FOR APPEAL NO. 20-042 I / We, Richard Segovia, hereby appeal the following departmental action: ISSUANCE of Wireless Box Permit No. 18WR-0369 by the San Francisco Public Works, Bureau of Street Use & Mapping which was issued or became effective on: June 18, 2020, to: Extenet Systems LLC, for the property located at: 2900 25th Street. BRIEFING SCHEDULE: The Appellant may, but is not required to, submit a one page (double-spaced) supplementary statement with this Preliminary Statement of Appeal. -
Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°. -
Pacing Early Mars Fluvial Activity at Aeolis Dorsa: Implications for Mars
1 Pacing Early Mars fluvial activity at Aeolis Dorsa: Implications for Mars 2 Science Laboratory observations at Gale Crater and Aeolis Mons 3 4 Edwin S. Kitea ([email protected]), Antoine Lucasa, Caleb I. Fassettb 5 a Caltech, Division of Geological and Planetary Sciences, Pasadena, CA 91125 6 b Mount Holyoke College, Department of Astronomy, South Hadley, MA 01075 7 8 Abstract: The impactor flux early in Mars history was much higher than today, so sedimentary 9 sequences include many buried craters. In combination with models for the impactor flux, 10 observations of the number of buried craters can constrain sedimentation rates. Using the 11 frequency of crater-river interactions, we find net sedimentation rate ≲20-300 μm/yr at Aeolis 12 Dorsa. This sets a lower bound of 1-15 Myr on the total interval spanned by fluvial activity 13 around the Noachian-Hesperian transition. We predict that Gale Crater’s mound (Aeolis Mons) 14 took at least 10-100 Myr to accumulate, which is testable by the Mars Science Laboratory. 15 16 1. Introduction. 17 On Mars, many craters are embedded within sedimentary sequences, leading to the 18 recognition that the planet’s geological history is recorded in “cratered volumes”, rather than 19 just cratered surfaces (Edgett and Malin, 2002). For a given impact flux, the density of craters 20 interbedded within a geologic unit is inversely proportional to the deposition rate of that 21 geologic unit (Smith et al. 2008). To use embedded-crater statistics to constrain deposition 22 rate, it is necessary to distinguish the population of interbedded craters from a (usually much 23 more numerous) population of craters formed during and after exhumation. -
Learning About the Earth As a System. International Conference on Geoscience Education Conference Proceedings (2Nd, Hilo, HI, July 28-31, 1997)
DOCUMENT RESUME ED 422 163 SE 061 669 AUTHOR Fortner, Rosanne W., Ed.; Mayer, Victor J., Ed. TITLE Learning about the Earth as a System. International Conference on Geoscience Education Conference Proceedings (2nd, Hilo, HI, July 28-31, 1997). INSTITUTION Ohio State Univ., Columbus. PUB DATE 1998-00-00 NOTE 190p. PUB TYPE Collected Works Proceedings (021) EDRS PRICE MF01/PC08 Plus Postage. DESCRIPTORS *Earth Science; *Educational Strategies; Elementary Secondary Education; Geology; Higher Education; Learning Strategies; Public Policy; Science and Society; *Science Curriculum; *Science Education ABSTRACT Learning about the earth as a system was the/focus of the 1997 International Conference on Geoscience Education. This proceedings contains details on the organization of the conference as well as five general sessions by various participants. The interactive poster sessions are organized according to three themes:(1) Earth Systems/Science Programs; (2) Earth Systems/Science Instruction; and (3) Public Information, Research, and Innovation. Addresses related to the conferring of four lifetime service awards are also included along with conference highlights, participants' evaluation of the conference, participant addresses, and an index to program contributors. (DDR) ******************************************************************************** * Reproductions supplied by EDRS are the best that can be made * * from the original document. * ******************************************************************************** . , arra2.m' a -
USGS Open-File Report 2006-1263
Abstracts of the Annual Meeting of Planetary Geologic Mappers, Nampa, Idaho 2006 Edited By Tracy K.P. Gregg,1 Kenneth L. Tanaka,2 and R. Stephen Saunders3 Open-File Report 2006-1263 2006 Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government. U.S. DEPARTMENT OF THE INTERIOR U.S. GEOLOGICAL SURVEY 1 The State University of New York at Buffalo, Department of Geology, 710 Natural Sciences Complex, Buffalo, NY 14260-3050. 2 U.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001. 3 NASA Headquarters, Office of Space Science, 300 E. Street SW, Washington, DC 20546. Report of the Annual Mappers Meeting Northwest Nazarene University Nampa, Idaho June 30 – July 2, 2006 Approximately 18 people attended this year’s mappers meeting, and many more submitted abstracts and maps in absentia. The meeting was held on the campus of Northwest Nazarene University (NNU), and was graciously hosted by NNU’s School of Health and Science. Planetary mapper Dr. Jim Zimbelman is an alumnus of NNU, and he was pivotal in organizing the meeting at this location. Oral and poster presentations were given on Friday, June 30. Drs. Bill Bonnichsen and Marty Godchaux led field excursions on July 1 and 2. USGS Astrogeology Team Chief Scientist Lisa Gaddis led the meeting with a brief discussion of the status of the planetary mapping program at USGS, and a more detailed description of the Lunar Mapping Program. She indicated that there is now a functioning website (http://astrogeology.usgs.gov/Projects/PlanetaryMapping/Lunar/) which shows which lunar quadrangles are available to be mapped.