Supporting Information (SI) Appendix Persistence and Origin of the Lunar Core Dynamo
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Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
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. -
Earth: Atmospheric Evolution of a Habitable Planet
Earth: Atmospheric Evolution of a Habitable Planet Stephanie L. Olson1,2*, Edward W. Schwieterman1,2, Christopher T. Reinhard1,3, Timothy W. Lyons1,2 1NASA Astrobiology Institute Alternative Earth’s Team 2Department of Earth Sciences, University of California, Riverside 3School of Earth and Atmospheric Science, Georgia Institute of Technology *Correspondence: [email protected] Table of Contents 1. Introduction ............................................................................................................................ 2 2. Oxygen and biological innovation .................................................................................... 3 2.1. Oxygenic photosynthesis on the early Earth .......................................................... 4 2.2. The Great Oxidation Event ......................................................................................... 6 2.3. Oxygen during Earth’s middle chapter ..................................................................... 7 2.4. Neoproterozoic oxygen dynamics and the rise of animals .................................. 9 2.5. Continued oxygen evolution in the Phanerozoic.................................................. 11 3. Carbon dioxide, climate regulation, and enduring habitability ................................. 12 3.1. The faint young Sun paradox ................................................................................... 12 3.2. The silicate weathering thermostat ......................................................................... 12 3.3. Geological -
Origin of the Solar System
Creation Myths The rise of the monotheistic religions changed this view. When one of the gods got a higher Old Myths status than others (who in some cases became Speculation about the origin and evolution of demons or devils), he continued to increase in the earth and the celestial bodies is probably as prestige and power until he became the Supreme old as human thinking. During the millennia that Lord, the undisputed ruler of the whole world. are covered by the history of science, philosphy, Then it was not enough for him to create the world and religion we can distinguish three types of ap in the sense of organizing a preexisting chaos; he proach to this problem. had to create it all from nothing (ex nihilo) by The first is the "theocratic-myth" approach, pronouncing a magic word or by his will power. according to which the evolution of the world was This is the meaning of "creation" when we use it governed by gods who once upon a time created today, but it is a relatively new concept. It was it. However, we must remember that the meaning generally accepted in Christianity in the second of "creation" has changed. The earliest meaning century A.D. but the Genesis description of the of this term seems to have been that the gods Creation seems to have either meaning. The crea brought order into a preexisting chaos. The world tion ex nihilo was not generally accepted by the was "ungenerated and indestructible"-as Aris philosophical-scientific community until the syn totle puts it-and the gods were part of this world thesis by St. -
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 -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to contain- ing a treasure trove of the Moon’s history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently avail- able samples, such as those related to the age of the Moon, duration of lunar volcanism, the Role of Sample Return in Addressing Major Questions in Planetary Sciences Edited by Mahesh Anand, Sara Russell, Yangting Lin, Meenakshi Wadhwa, Kuljeet Kaur Marhas and Shogo Tachibana B R. -
Lunar Impact Basins Revealed by Gravity Recovery and Interior
Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, Sean Solomon, David Smith, Frank Lemoine, Erwan Mazarico, Terence Sabaka, et al. To cite this version: Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, et al.. Lunar im- pact basins revealed by Gravity Recovery and Interior Laboratory measurements. Science Advances , American Association for the Advancement of Science (AAAS), 2015, 1 (9), pp.e1500852. 10.1126/sci- adv.1500852. hal-02458613 HAL Id: hal-02458613 https://hal.archives-ouvertes.fr/hal-02458613 Submitted on 26 Jun 2020 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. RESEARCH ARTICLE PLANETARY SCIENCE 2015 © The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. Distributed Lunar impact basins revealed by Gravity under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC). Recovery and Interior Laboratory measurements 10.1126/sciadv.1500852 Gregory A. Neumann,1* Maria T. Zuber,2 Mark A. Wieczorek,3 James W. Head,4 David M. H. Baker,4 Sean C. Solomon,5,6 David E. Smith,2 Frank G. -
Climate Change and Freshwater Fisheries
See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/282814011 Climate change and freshwater fisheries Chapter · September 2015 DOI: 10.1002/9781118394380.ch50 CITATIONS READS 15 1,011 1 author: Chris Harrod University of Antofagasta 203 PUBLICATIONS 2,695 CITATIONS SEE PROFILE Some of the authors of this publication are also working on these related projects: "Characterizing the Ecological Niche of Native Cockroaches in a Chilean biodiversity hotspot: diet and plant-insect associations" National Geographic Research and Exploration GRANT #WW-061R-17 View project Effects of seasonal and monthly hypoxic oscillations on seabed biota: evaluating relationships between taxonomical and functional diversity and changes on trophic structure of macrobenthic assemblages View project All content following this page was uploaded by Chris Harrod on 28 February 2018. The user has requested enhancement of the downloaded file. Chapter 7.3 Climate change and freshwater fisheries Chris Harrod Instituto de Ciencias Naturales Alexander Von Humboldt, Universidad de Antofagasta, Antofagasta, Chile Abstract: Climate change is among the most serious environmental challenge facing humanity and the ecosystems that provide the goods and services on which it relies. Climate change has had a major historical influence on global biodiversity and will continue to impact the structure and function of natural ecosystems, including the provision of natural services such as fisheries. Freshwater fishery professionals (e.g. fishery managers, fish biologists, fishery scientists and fishers) need to be informed regarding the likely impacts of climate change. Written for such an audience, this chapter reviews the drivers of climatic change and the means by which its impacts are predicted. -
GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins. -
Who Got Moseley's Prize?
Chapter 4 Who Got Moseley’s Prize? Virginia Trimble1 and Vera V. Mainz*,2 1Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, United States 2Department of Chemistry, University of Illinois at Urbana-Champaign, Urbana, Illinois 61802, United States *E-mail: [email protected]. Henry Gwyn Jeffreys Moseley (1887-1915) made prompt and very skilled use of the then new technique of X-ray scattering by crystals (Bragg scattering) to solve several problems about the periodic table and atoms. He was nominated for both the chemistry and physics Nobel Prizes by Svante Arrhenius in 1915, but was dead at Gallipoli before the committees finished their deliberations. Instead, the 1917 physics prize (announced in 1918 and presented on 6 June 1920) went to Charles Glover Barkla (1877-1944) “for discovery of the Röntgen radiation of the elements.” This, and his discovery of X-ray polarization, were done with earlier techniques that he never gave up. Moseley’s contemporaries and later historians of science have written that he would have gone on to other major achievements and a Nobel Prize if he had lived. In contrast, after about 1916, Barkla moved well outside the scientific mainstream, clinging to upgrades of his older methods, denying the significance of the Bohr atom and quantization, and continuing to report evidence for what he called the J phenomenon. This chapter addresses the lives and scientific endeavors of Moseley and Barkla, something about the context in which they worked and their connections with other scientists, contemporary, earlier, and later. © 2017 American Chemical Society Introduction Henry Moseley’s (Figure 1) academic credentials consisted of a 1910 Oxford BA with first-class honors in Mathematical Moderations and a second in Natural Sciences (physics) and the MA that followed more or less automatically a few years later. -
Science Concept 3: Key Planetary
Science Concept 6: The Moon is an Accessible Laboratory for Studying the Impact Process on Planetary Scales Science Concept 6: The Moon is an accessible laboratory for studying the impact process on planetary scales Science Goals: a. Characterize the existence and extent of melt sheet differentiation. b. Determine the structure of multi-ring impact basins. c. Quantify the effects of planetary characteristics (composition, density, impact velocities) on crater formation and morphology. d. Measure the extent of lateral and vertical mixing of local and ejecta material. INTRODUCTION Impact cratering is a fundamental geological process which is ubiquitous throughout the Solar System. Impacts have been linked with the formation of bodies (e.g. the Moon; Hartmann and Davis, 1975), terrestrial mass extinctions (e.g. the Cretaceous-Tertiary boundary extinction; Alvarez et al., 1980), and even proposed as a transfer mechanism for life between planetary bodies (Chyba et al., 1994). However, the importance of impacts and impact cratering has only been realized within the last 50 or so years. Here we briefly introduce the topic of impact cratering. The main crater types and their features are outlined as well as their formation mechanisms. Scaling laws, which attempt to link impacts at a variety of scales, are also introduced. Finally, we note the lack of extraterrestrial crater samples and how Science Concept 6 addresses this. Crater Types There are three distinct crater types: simple craters, complex craters, and multi-ring basins (Fig. 6.1). The type of crater produced in an impact is dependent upon the size, density, and speed of the impactor, as well as the strength and gravitational field of the target. -
Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)
ASTROBIOLOGY Volume 14, Number 11, 2014 News & Views ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2014.1227 A New Analysis of Mars ‘‘Special Regions’’: Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2) John D. Rummel,1 David W. Beaty,2 Melissa A. Jones,2 Corien Bakermans,3 Nadine G. Barlow,4 Penelope J. Boston,5 Vincent F. Chevrier,6 Benton C. Clark,7 Jean-Pierre P. de Vera,8 Raina V. Gough,9 John E. Hallsworth,10 James W. Head,11 Victoria J. Hipkin,12 Thomas L. Kieft,5 Alfred S. McEwen,13 Michael T. Mellon,14 Jill A. Mikucki,15 Wayne L. Nicholson,16 Christopher R. Omelon,17 Ronald Peterson,18 Eric E. Roden,19 Barbara Sherwood Lollar,20 Kenneth L. Tanaka,21 Donna Viola,13 and James J. Wray22 Abstract A committee of the Mars Exploration Program Analysis Group (MEPAG) has reviewed and updated the description of Special Regions on Mars as places where terrestrial organisms might replicate (per the COSPAR Planetary Protection Policy). This review and update was conducted by an international team (SR-SAG2) drawn from both the biological science and Mars exploration communities, focused on understanding when and where Special Regions could occur. The study applied recently available data about martian environments and about terrestrial organisms, building on a previous analysis of Mars Special Regions (2006) undertaken by a similar team. Since then, a new body of highly relevant information has been generated from the Mars Reconnaissance Orbiter (launched in 2005) and Phoenix (2007) and data from Mars Express and the twin Mars Exploration Rovers (all 2003).