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Open Hanagan Thesis Schreyer.Pdf
THE PENNSYLVANIA STATE UNIVERSITY SCHREYER HONORS COLLEGE DEPARTMENT OF EARTH AND MINERAL SCIENCES CHANGES IN CRATER MORPHOLOGY ASSOCIATED WITH VOLCANIC ACTIVITY AT TELICA VOLCANO, NICARAGUA: INSIGHT INTO SUMMIT CRATER FORMATION AND ERUPTION TRIGGERING CATHERINE E. HANAGAN SPRING 2019 A thesis submitted in partial fulfillment of the requirements for a baccalaureate degree in the Geosciences with honors in the Geosciences Reviewed and approved* by the following: Peter La Femina Associate Professor of Geosciences Thesis Supervisor Maureen Feineman Associate Research Professor and Associate Head for Undergraduate Programs Honors Adviser * Signatures are on file in the Schreyer Honors College. i ABSTRACT Telica is a persistently active basaltic-andesite stratovolcano in the Central American Volcanic Arc of Nicaragua. Poorly predicted sub-decadal, low explosivity (VEI 1-2) phreatic eruptions and background persistent activity with high-rates of seismic unrest and frequent degassing contribute to morphologic change in Telica’s active crater on a small spatiotemporal scale. These changes sustain a morphology similar to those of commonly recognized calderas or pit craters (Roche et al., 2001; Rymer et al., 1998), and have been related to sealing of the hydrothermal system prior to eruption (INETER Buletin Anual, 2013). We use photograph observations and Structure from Motion point cloud construction and comparison (Multiscale Model to Model Cloud Comparison, Lague et al., 2013; Westoby et al., 2012) from 1994 to 2017 to correlate changes in Telica’s crater with sustained summit crater formation and eruptive pre- cursors. Two previously proposed mechanisms for sealing at Telica are: 1) widespread hydrothermal mineralization throughout the magmatic-hydrothermal system (Geirsson et al., 2014; Rodgers et al., 2015; Roman et al., 2016); and/or 2) surficial blocking of the vent by landslides and rock fall (INETER Buletin Anual, 2013). -
Astrophysics in 2006 3
ASTROPHYSICS IN 2006 Virginia Trimble1, Markus J. Aschwanden2, and Carl J. Hansen3 1 Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, Las Cumbres Observatory, Santa Barbara, CA: ([email protected]) 2 Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Organization ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304: ([email protected]) 3 JILA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309: ([email protected]) Received ... : accepted ... Abstract. The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords: cosmology: general, galaxies: general, ISM: general, stars: general, Sun: gen- eral, planets and satellites: general, astrobiology CONTENTS 1. Introduction 6 1.1 Up 6 1.2 Down 9 1.3 Around 10 2. Solar Physics 12 2.1 The solar interior 12 2.1.1 From neutrinos to neutralinos 12 2.1.2 Global helioseismology 12 2.1.3 Local helioseismology 12 2.1.4 Tachocline structure 13 arXiv:0705.1730v1 [astro-ph] 11 May 2007 2.1.5 Dynamo models 14 2.2 Photosphere 15 2.2.1 Solar radius and rotation 15 2.2.2 Distribution of magnetic fields 15 2.2.3 Magnetic flux emergence rate 15 2.2.4 Photospheric motion of magnetic fields 16 2.2.5 Faculae production 16 2.2.6 The photospheric boundary of magnetic fields 17 2.2.7 Flare prediction from photospheric fields 17 c 2008 Springer Science + Business Media. -
Apollo 17 Index: 70 Mm, 35 Mm, and 16 Mm Photographs
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) Preparation, Scanning, Editing, and Conversion to Adobe Portable Document Format (PDF) by: Ronald A. Wells University of California Berkeley, CA 94720 May 2000 A P O L L O 1 7 I N D E X 7 0 m m, 3 5 m m, A N D 1 6 m m P H O T O G R A P H S M a p p i n g S c i e n c e s B r a n c h N a t i o n a l A e r o n a u t i c s a n d S p a c e A d m i n i s t r a t i o n J o h n s o n S p a c e C e n t e r H o u s t o n, T e x a s APPROVED: Michael C . -
Volcano Collapse Promoted by Hydrothermal Alteration and Edifice
Volcano collapse promoted by hydrothermal alteration and edifice shape, Mount Rainier, Washington Mark E. Reid* Thomas W. Sisson U.S. Geological Survey, 345 Middlefield Road, MS 910, Menlo Park, California 94025, USA Dianne L. Brien ABSTRACT FLANK COLLAPSES AT MOUNT RAINIER Catastrophic collapses of steep volcano flanks threaten many At Mount Rainier, some volcanic debris flows or lahars began as populated regions, and understanding factors that promote collapse fluid-saturated flank collapses (large landslides), whereas others were could save lives and property. Large collapses of hydrothermally al- likely triggered by pyroclastic flows entraining snow and ice, glacial tered parts of Mount Rainier have generated far-traveled debris flows; outburst floods, or torrential rains. Hydrothermally derived clay min- future flows would threaten densely populated parts of the Puget erals are abundant in some of the most widespread lahar deposits, in- Sound region. We evaluate edifice collapse hazards at Mount Rainier cluding the massive ;3.8 km3 Osceola Mudflow of 5600 yr ago (Cran- using a new three-dimensional slope stability method incorporating dell and Waldron, 1956; Vallance and Scott, 1997), the ;0.2 km3 detailed geologic mapping and subsurface geophysical imaging to de- Round Pass mudflow of ;2600 yr ago, and the ;0.26 km3 Electron termine distributions of strong (fresh) and weak (altered) rock. Quan- mudflow of ;500 yr ago (Scott et al., 1995). This association is evi- titative three-dimensional slope stability calculations reveal that size- dence that weakening of edifice rocks by acid sulfate-argillic hydro- able flank collapse (.0.1 km3)ispromotedbyvoluminous,weak, thermal alteration promoted flank collapse (Crandell, 1971; Scott et al., hydrothermally altered rock situated high on steep slopes. -
1 the Lifecycle of Hollows on Mercury
The Lifecycle of Hollows on Mercury: An Evaluation of Candidate Volatile Phases and a Novel Model of Formation. 1 1 2 3 M. S. Phillips , J. E. Moersch , C. E. Viviano , J. P. Emery 1Department of Earth and Planetary Sciences, University of Tennessee, Knoxville 2Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory 3Department of Astronomy and Planetary Sciences, Northern Arizona University Corresponding author: Michael Phillips ([email protected]) Keywords: Mercury, hollows, thermal model, fumarole. Abstract On Mercury, high-reflectance, flat-floored depressions called hollows are observed nearly globally within low-reflectance material, one of Mercury’s major color units. Hollows are thought to be young, or even currently active, features that form via sublimation, or a “sublimation-like” process. The apparent abundance of sulfides within LRM combined with spectral detections of sulfides associated with hollows suggests that sulfides may be the phase responsible for hollow formation. Despite the association of sulfides with hollows, it is still not clear whether sulfides are the hollow-forming phase. To better understand which phase(s) might be responsible for hollow formation, we calculated sublimation rates for 57 candidate hollow-forming volatile phases from the surface of Mercury and as a function of depth beneath regolith lag deposits of various thicknesses. We found that stearic acid (C18H36O2), fullerenes (C60, C70), and elemental sulfur (S) have the appropriate thermophysical properties to explain hollow formation. Stearic acid and fullerenes are implausible hollow-forming phases because they are unlikely to have been delivered to or generated on Mercury in high enough volume to account for hollows. -
Radar Imaging of Solar System Ices
RADAR IMAGING OF SOLAR SYSTEM ICES A DISSERTATION SUBMITTED TO THE DEPARTMENT OF ELECTRICAL ENGINEERING AND THE COMMITTEE ON GRADUATE STUDIES OF STANFORD UNIVERSITY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Leif J. Harcke May 2005 © Copyright by Leif J. Harcke 2005 All Rights Reserved ii iv Abstract We map the planet Mercury and Jupiter’s moons Ganymede and Callisto using Earth-based radar telescopes and find that all bodies have regions exhibiting high, depolarized radar backscatter and polarization inversion (µc > 1). Both characteristics suggest volume scat- tering from water ice or similar cold-trapped volatiles. Synthetic aperture radar mapping of Mercury’s north and south polar regions at fine (6 km) resolution at 3.5 cm wavelength corroborates the results of previous 13 cm investigations of enhanced backscatter and po- larization inversion (0:9 µc 1:3) from areas on the floors of craters at high latitudes, ≤ ≤ where Mercury’s near-zero obliquity results in permanent Sun shadows. Co-registration with Mariner 10 optical images demonstrates that this enhanced scattering cannot be caused by simple double-bounce geometries, since the bright, reflective regions do not appear on the radar-facing wall but, instead, in shadowed regions not directly aligned with the radar look direction. A simple scattering model accounts for exponential, wavelength-dependent attenuation through a protective regolith layer. Thermal models require the existence of this layer to protect ice deposits in craters at other than high polar latitudes. The additional attenuation (factor 1:64 15%) of the 3.5 cm wavelength data from these experiments over previous 13 cm radar observations supports multiple interpretations of layer thickness, ranging from 0 11 to 35 15 cm, depending on the assumed scattering law exponent n. -
Morphometric Characterization and Reconstruction Effect Among Lunar Impact Craters
Earth Moon Planets (2014) 111:139–155 DOI 10.1007/s11038-014-9431-0 Morphometric Characterization and Reconstruction Effect Among Lunar Impact Craters Weiming Cheng • Jiao Wang • Cong Wan Received: 2 January 2014 / Accepted: 11 March 2014 / Published online: 19 March 2014 Ó Springer Science+Business Media Dordrecht 2014 Abstract Impact craters on the lunar surface have a variety of morphometric charac- teristics that are very useful in understanding the evolutionary history of lunar landscape morphologies. Based on digital elevation model data and photographs from China’s Chang’E-1 lunar orbiter, we develop morphologic parameters and quantitative methods for presenting the morphometric characteristics of impact craters, analyzing their relational distribution, and estimating the relative order of their formation. We also analyze features in profile where craters show signs of having formed on the edge of previously existing craters to show that superimposed impacts affect morphologic reconstructions. As a result, impact craters have significant effects on the reconstruction of ancient topography and the estimation of relative formation ages. Keywords Morphometric characterization Á Position relationship Á Relative construction age Á Chang’E-1 1 Introduction The Earth’s Moon, it’s only natural satellite, has a potentially complete record of the 4.5- billion year evolutionary history of the solar system (Ronca 1966; Ouyang 2005). Impact craters are the most obvious and typical geomorphologic units (Ronca 1969; Neukum and Ivanov 1994; Neukum et al. 1975); they form when a planetary body (meteoro, comet, etc.) impact against the surface (King 1976). The diameters of impact craters on the lunar W. Cheng (&) Á J. -
Science Concept 2: the Structure and Composition of the Lunar Interior Provide Fundamental Information on the Evolution of a Differentiated Planetary Body
Science Concept 2: The Structure and Composition of the Lunar Interior Provide Fundamental Information on the Evolution of a Differentiated Planetary Body Science Concept 2: The Structure and Composition of the Lunar Interior Provide Fundamental Information on the Evolution of a Differentiated Planetary Body Science Goals: a. Determine the thickness of the lunar crust (upper and lower) and characterize its lateral variability on regional and global scales. b. Characterize the chemical/physical stratification in the mantle, particularly the nature of the putative 500-km discontinuity and the composition of the lower mantle. c. Determine the size, composition, and state (solid/liquid) of the core of the Moon. d. Characterize the thermal state of the interior and elucidate the workings of the planetary heat engine. INTRODUCTION Each of the Science Goals addressed by Science Concept 2 is linked: data regarding the crust, mantle, and core must be obtained in order to understand the thermal state of the interior and the planetary heat engine. Much about these Science Goals is currently unknown: crustal thickness and lateral variability are constrained by gravity and seismic models which suffer from non-uniqueness and a lack of control points; mantle composition is ambiguously estimated from seismic velocity profiles and assumed lunar bulk compositions; mantle structure is obtained through seismic velocity profiles, but fine-scale structure is not resolved and any structure outside the Apollo network and below 1000 kilometers depth is unknown; the size, composition and state of the core are obtained through models with few constraints, where the size and state are dependent on an unknown composition, making any core characteristic estimates highly variable; and the thermal state of the interior is constrained by heat flow measurements and characteristics of the core, but current heat flow data are not representative of the global heat flux and core models are non-unique. -
The Messenger
THE MESSENGER ( , New Meteorite Finds At Imilac No. 47 - March 1987 H. PEDERSEN, ESO, and F. GARe/A, elo ESO Introduction hand, depend more on the preserving some 7,500 meteorites were recovered Stones falling from the sky have been conditions of the terrain, and the extent by Japanese and American expeditions. collected since prehistoric times. They to which it allows meteorites to be spot They come from a smaller, but yet un were, until recently, the only source of ted. Most meteorites are found by known number of independent falls. The extraterrestrial material available for chance. Active searching is, in general, meteorites appear where glaciers are laboratory studies and they remain, too time consuming to be of interest. pressed up towards a mountain range, even in our space age, a valuable However, the blue-ice fields of Antarctis allowing the ice to evaporate. Some source for investigation of the solar sys have proven to be a happy hunting have been Iying in the ice for as much as tem's early history. ground. During the last two decades 700,000 years. It is estimated that, on the average, each square kilometre of the Earth's surface is hit once every million years by a meteorite heavier than 500 grammes. Most are lost in the oceans, or fall in sparsely populated regions. As a result, museums around the world receive as few as about 6 meteorites annually from witnessed falls. Others are due to acci dental finds. These have most often fallen in prehistoric times. Each of the two groups, 'falls' and 'finds', consists of material from about one thousand catalogued, individual meteorites. -
An Inventory of Subglacial Volcanoes in West Antarctica
Downloaded from http://sp.lyellcollection.org/ by guest on October 2, 2021 A new volcanic province: an inventory of subglacial volcanoes in West Antarctica MAXIMILLIAN VAN WYK DE VRIES*, ROBERT G. BINGHAM & ANDREW S. HEIN School of GeoSciences, University of Edinburgh, Drummond Street, Edinburgh EH8 9XP, UK *Correspondence: [email protected] Abstract: The West Antarctic Ice Sheet overlies the West Antarctic Rift System about which, due to the comprehensive ice cover, we have only limited and sporadic knowledge of volcanic activity and its extent. Improving our understanding of subglacial volcanic activity across the province is important both for helping to constrain how volcanism and rifting may have influenced ice-sheet growth and decay over previous glacial cycles, and in light of concerns over whether enhanced geo- thermal heat fluxes and subglacial melting may contribute to instability of the West Antarctic Ice Sheet. Here, we use ice-sheet bed-elevation data to locate individual conical edifices protruding upwards into the ice across West Antarctica, and we propose that these edifices represent subglacial volcanoes. We used aeromagnetic, aerogravity, satellite imagery and databases of confirmed volca- noes to support this interpretation. The overall result presented here constitutes a first inventory of West Antarctica’s subglacial volcanism. We identified 138 volcanoes, 91 of which have not previ- ously been identified, and which are widely distributed throughout the deep basins of West Antarc- tica, but are especially concentrated and orientated along the >3000 km central axis of the West Antarctic Rift System. Gold Open Access: This article is published under the terms of the CC-BY 3.0 license. -
Impact Cratering – Fundamental Process in Geoscience and Planetary Science
Impact cratering – fundamental process in geoscience and planetary science JKPati1 and WUReimold2 1Department of Earth and Planetary Sciences, Nehru Science Centre, University of Allahabad, Allahabad 211 002, India. e-mail: [email protected] 2Museum f. Natural History (Mineralogy), Humboldt-University in Berlin, Invalidenstrasse 43, D-10115 Berlin, Germany. e-mail: [email protected] Impact cratering is a geological process characterized by ultra-fast strain rates, which generates extreme shock pressure and shock temperature conditions on and just below planetary surfaces. Despite initial skepticism, this catastrophic process has now been widely accepted by geoscientists with respect to its importance in terrestrial – indeed, in planetary – evolution. About 170 impact structures have been discovered on Earth so far, and some more structures are considered to be of possible impact origin. One major extinction event, at the Cretaceous–Paleogene boundary, has been firmly linked with catastrophic impact, but whether other important extinction events in Earth history, including the so-called “Mother of All Mass Extinctions” at the Permian–Triassic boundary, were triggered by huge impact catastrophes is still hotly debated and a subject of ongoing research. There is a beneficial side to impact events as well, as some impact structures worldwide have been shown to contain significant (in some cases, world class) ore deposits, including the gold– uranium province of the Witwatersrand basin in South Africa, the enormous Ni and PGE deposits of the Sudbury structure in Canada, as well as important hydrocarbon resources, especially in North America. Impact cratering is not a process of the past, and it is mandatory to improve knowledge of the past-impact record on Earth to better constrain the probability of such events in the future. -
Bulk Mineralogy of Lunar Crater Central Peaks Via Thermal Infrared Spectra from the Diviner Lunar Radiometer - a Study of the Moon’S Crustal Composition at Depth
Bulk mineralogy of Lunar crater central peaks via thermal infrared spectra from the Diviner Lunar Radiometer - A study of the Moon’s crustal composition at depth Eugenie Song A thesis submitted in partial fulfillment of the requirements for the degree of Master of Sciences University of Washington 2012 Committee: Joshua Bandfield Alan Gillespie Bruce Nelson Program Authorized to Offer Degree: Earth and Space Sciences 1 Table of Contents List of Figures ............................................................................................................................................... 3 List of Tables ................................................................................................................................................ 3 Abstract ......................................................................................................................................................... 4 1 Introduction .......................................................................................................................................... 5 1.1 Formation of the Lunar Crust ................................................................................................... 5 1.2 Crater Morphology ................................................................................................................... 7 1.3 Spectral Features of Rock-Forming Silicates in the Lunar Environment ................................ 8 1.4 Compositional Studies of Lunar Crater Central Peaks ...........................................................