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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. -
Another Giant Caldera Volcano?
www.MantlePlumes.org McCall (2008) http://www.mantleplumes.org/Mercury.html Mercury’s “spider” – another giant caldera volcano? G.J.H. McCall 44 Robert Franklin Way, South Cerney, Glos. GL7 5UD [email protected] Dr Joe McCall, retired, is a former Reader (Associate Professor) of Geology at the University of Western Australia. He also curated the meteorites at the Western Australian Museum during his time in Perth. Besides his professional work on terrestrial geology he has long had an interest in the extraterrestrial extensions of geology, to the Moon, Mars, Mercury and other bodies in the Solar System. He was recently leading editor of a history of Meteoritics and key collections, published by the Geological Society of London, of which he is a Senior Fellow. He was awarded its prestigious Coke medal in 1994. This letter reports the discovery, by means of comparison of a MESSENGER image of part of the Caloris Basin, Mercury, with images of Martian caldera volcanoes, of a very large caldera volcano. The structure, which has been called "the spider" informally by the MESSENGER team, and has hitherto been unexplained, is ~330 km in diameter and shows remarkable similarities to the giant Martian caldera volcanoes Ceraunius Tholus, Uranius Tholus and Tyrrhenia Patera. I have long had an interest in Mercury and regretted its long neglect without follow-ups to the Mariner 10 visit1. I have also written about the giant caldera volcano of Olympus Mons on Mars2. Mercury’s newly revealed and surprising image of a structure within the Caloris Basin, informally named "the spider" by the MESSENGER team, was recently discussed in Science Daily, as downloaded from the Web on 13.3.083 (Figure 1). -
Abrupt Climatic Changes As Triggering Mechanisms of Massive Volcanic Collapses
Journal of Volcanology and Geothermal Research 155 (2006) 329–333 www.elsevier.com/locate/jvolgeores Short communication Abrupt climatic changes as triggering mechanisms of massive volcanic collapses Lucia Capra Instituto de Geografía, UNAM, CU Coyoacan, 04510, Mexico DF, Mexico Received 7 March 2006; received in revised form 31 March 2006; accepted 19 April 2006 Available online 5 June 2006 Abstract Abrupt climate change can trigger volcanic collapses, phenomena that cause the destruction of the entire sector of a volcano, including its summit. During the past 30 ka, major volcanic collapses occurred just after main glacial peaks that ended with rapid deglaciation. Glacial debuttressing, load discharge and fluid circulation coupled with the post-glacial increase of humidity and heavy rains can activate the failure of unstable edifices. Furthermore, significant global warming can be responsible for the collapse of ice-capped unstable volcanoes, an unpredictable hazard that in few minutes can bury inhabited areas. © 2006 Published by Elsevier B.V. Keywords: volcanic collapse; global warming 1. Introduction Wyk de Vries et al., 2001; Clavero et al., 2002). Several analogue experiments have been performed to demon- Although climate changes have been considered to be strate how faults can deform volcanoes that finally a triggering mechanism for large eruptions (Rampino et collapse (Van Wyk de Vries and Borgia, 1996; Lagmay et al., 1979; McGuire et al., 1997), they have not, so far, al., 2000; Acocella, 2005; Norini and Lagmay, 2005). been related to the collapse of volcanoes. Unstable This is probably a very common mechanism, but it is volcanoes, whatever the origin of their instability, can spatially localized and can occur in an indeterminate collapse from the same triggering mechanism (McGuire, period of time. -
Numerical Modeling of the Emplacement of Socompa Rock Avalanche, Chile K
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 110, B12202, doi:10.1029/2005JB003758, 2005 Numerical modeling of the emplacement of Socompa rock avalanche, Chile K. Kelfoun and T. H. Druitt Laboratoire Magmas et Volcans, OPGC, UBP–CNRS–IRD, Clermont-Ferrand, France Received 1 April 2005; revised 27 June 2005; accepted 14 September 2005; published 16 December 2005. 3 [1] The 7.5 ka Socompa sector collapse emplaced 25 km of fragmented rock as a thin, but widespread (500 km2), avalanche deposit, followed by late stage sliding of 11 km3 as Toreva blocks. Most of the avalanche mass was emplaced dry, although saturation of a basal shear layer cannot be excluded. Modeling was carried out using the depth-averaged granular flow equations in order to provide information on the flow behavior of this well-preserved, long run-out avalanche. Results were constrained using structures preserved on the surface of the deposit, as well as by deposit outline and run-up (a proxy for velocity). Models assuming constant dynamic friction fail to produce realistic results because the low basal friction angles (1 to 3.5°) necessary to generate observed run-out permit neither adequate deposition on slopes nor preservation of significant morphology on the deposit surface. A reasonable fit is obtained, however, if the avalanche is assumed simply to experience a constant retarding stress of 50–100 kPa during flow. This permits long run-out as well as deposition on slopes and preservation of realistic depositional morphology. In particular the model explains a prominent topographic escarpment on the deposit surface as the frozen front of a huge wave of debris reflected off surrounding hills. -
Volcanic Hazards
have killed more than 5,000 people. Two important points are demonstrated by this. The first is that the most deadly eruptions are generally pyroclastic: lava flows are rarely a main cause of death. The second is that it is not always the biggest eruptions that cause the most deaths. Even quite small eruptions can be major killers – for example the 1985 eruption of Ruiz, which resulted in 5 the second largest number of volcanic fatalities of the twentieth century. Sometimes volcanoes kill people even when they are not erupting: Iliwerung 1979 (a landslide, not associated with an Volcanic hazards eruption, that caused a tsunami when it entered the sea) and Lake Nyos 1986 (escaping gas) being examples of death by two different non-eruptive mechanisms. In this chapter you will learn: • about the most devastating volcanic eruptions of historic times Some of the causes of death listed in Table 5.1 may need further • about the wide variety of ways in which eruptions can cause death elaboration. Famine, for example, is a result of crop failure and/ and destruction (including by triggering a tsunami). or the loss of livestock because of fallout, pyroclastic flows or gas poisoning. It is often accompanied by the spread of disease In previous chapters I dealt with the different types of volcano as a result of insanitary conditions brought about by pollution that occur and the ways in which they can erupt. The scene is now of the water supply. In the modern world it is to be hoped that set to examine the hazards posed to human life and well-being international food aid to a stricken area would prevent starvation by volcanic eruptions. -
Science for a Changing World
science for a changing world Cover photograph Mount Rainier, Washington, with the flood plain of the Puyallup River in the foreground, 50 kilometers downstream from the volcano. The flood plain is a pathway for debris flows (lahars) from the volcano, most recently by the Electron Mudflow about 500 to 600 years ago. (Photograph by David Wieprecht, U.S. Geological Survey.) Catastrophic Debris Flows Transformed from Landslides in Volcanic Terrains: Mobility, Hazard Assessment, and Mitigation Strategies By Kevin M. Scott, Jose Luis Macias, Jose Antonio Naranjo, Sergio Rodriguez, and John P. McGeehin U.S. Geological Survey Professional Paper 1630 U.S. DEPARTMENT OF THE INTERIOR GALE A. NORTON, Secretary U.S. GEOLOGICAL SURVEY CHARLES G. GROAT, Director Any use of trade, product, or firm names in this publication is for descriptive purposes only and does not imply endorsement by the U.S. Government. Reston, Virginia 2001 For sale by the U.S. Geological Survey, Information Services Box 25286, Federal Center Denver, CO 80225 Library of Congress Cataloging-in-Publication Data Scott, Kevin M., 1935- Catastrophic debris flows transformed from landslides in volcanic terrains: mobility, hazard assessment and mitigation strategies I by Kevin M. Scott ... [et al.]. p. em.- (U.S. Geological Survey professional paper; 1630) Includes bibliographical references and index. 1. Debris avalanches. 2. Lahars. 3. Catastrophes (Geology). I. Scott, Kevin M., 1935- 11. Series QE75.P9 no. 1630 [QE599.A2] 557.3 s-dc21 [551.3'07] 2001058484 ISBN 0-607-98578-X CONTENTS -
USGS Open-File Report 2009-1133, V. 1.2, Table 3
Table 3. (following pages). Spreadsheet of volcanoes of the world with eruption type assignments for each volcano. [Columns are as follows: A, Catalog of Active Volcanoes of the World (CAVW) volcano identification number; E, volcano name; F, country in which the volcano resides; H, volcano latitude; I, position north or south of the equator (N, north, S, south); K, volcano longitude; L, position east or west of the Greenwich Meridian (E, east, W, west); M, volcano elevation in meters above mean sea level; N, volcano type as defined in the Smithsonian database (Siebert and Simkin, 2002-9); P, eruption type for eruption source parameter assignment, as described in this document. An Excel spreadsheet of this table accompanies this document.] Volcanoes of the World with ESP, v 1.2.xls AE FHIKLMNP 1 NUMBER NAME LOCATION LATITUDE NS LONGITUDE EW ELEV TYPE ERUPTION TYPE 2 0100-01- West Eifel Volc Field Germany 50.17 N 6.85 E 600 Maars S0 3 0100-02- Chaîne des Puys France 45.775 N 2.97 E 1464 Cinder cones M0 4 0100-03- Olot Volc Field Spain 42.17 N 2.53 E 893 Pyroclastic cones M0 5 0100-04- Calatrava Volc Field Spain 38.87 N 4.02 W 1117 Pyroclastic cones M0 6 0101-001 Larderello Italy 43.25 N 10.87 E 500 Explosion craters S0 7 0101-003 Vulsini Italy 42.60 N 11.93 E 800 Caldera S0 8 0101-004 Alban Hills Italy 41.73 N 12.70 E 949 Caldera S0 9 0101-01= Campi Flegrei Italy 40.827 N 14.139 E 458 Caldera S0 10 0101-02= Vesuvius Italy 40.821 N 14.426 E 1281 Somma volcano S2 11 0101-03= Ischia Italy 40.73 N 13.897 E 789 Complex volcano S0 12 0101-041 -
Direct Constraints on the Timing of Martian Valley Network Formation Derived Using Buffered Crater Counting
Seventh International Conference on Mars 3050.pdf DIRECT CONSTRAINTS ON THE TIMING OF MARTIAN VALLEY NETWORK FORMATION DERIVED USING BUFFERED CRATER COUNTING. C. I. Fassett and J. W. Head III, Dept. of Geological Sciences, Brown University, Providence, RI 02912 ([email protected] and [email protected]). Introduction: Valley networks on Mars are mostly (Fig. 1), as has been attempted before for other planetary found in the heavily cratered highland terrain that dates from surface features [e.g., 12]. The advantage of this technique the Noachian era (the earliest period of martian history) [e.g., is that it utilizes the fact that large craters subtend a much 1]. These valley features are commonly invoked as geomor- larger area than small ones. We first map the valley we wish phological evidence for an early surface environment differ- to examine, and then find all craters clearly superposed upon ing from that of today [2], although their implications for the valley which a within an area appropriate for its diame- climate has continued to be controversial [e.g., 3]. Because ter. For each crater (and its ejecta), a stratigraphic judgment the processes of valley network formation are important for is required, and we assume that any topographic barrier (e.g., understanding surface conditions on early Mars, there has a crater rim or its ejecta) that is superposed on a valley and is long been substantial interest in constraining when valleys unmodified by further valley activity must have formed after were active [e.g., 4, 5] and when the transition occurred from valley activity ceased. -
The GEAS Project: Astronomy Laboratory
Lab 4 Cratering and the Martian Surface 4.1 Introduction Human space travel enthusiasts hope that our manned missions to the Moon will serve as stepping stones for an eventual trip to Mars. Our “visit” to the Moon in our previous lunar cratering laboratory exercise has prepared us similarly to visit Mars today. We have already learned that cratering is a key process in shaping the appearance of terrestrial planetary surfaces, and that counting craters can help determine the ages of surface features. We studied techniques used to decide which geological event occurred first, or which surface is younger (relative dating techniques), and also learned how to determine absolute ages based on radioactive dating of physical samples. Lunar and Martian surfaces are similar in many ways (both types are heavily cratered in some places and covered with smooth ancient lava flows in others), but they exhibit several important differences. First, volcanic features on Mars are much more prominent than those on the Moon. Mars has the largest volcanoes in the entire solar system, and some of them have clearly become inactive only recently. (Some planetary scientists suspect that the largest Martian volcano of all, Olympus Mons, may still be active today.) Second, unlike the bone-dry Moon, Mars was once a very wet planet. Its surface contains channel and river delta-like features that were undeniably formed by flowing water in the past. These differences lead us to two important questions. When did the last volcanic eruptions occur on Mars, and when did water last flow freely there? In this lab, you’ll use crater counting techniques to help reconstruct a Martian surface chronology and investigate these questions. -
Across-Arc Geochemical Variations in the Southern Volcanic Zone, Chile (34.5–38.0°S): Constraints on Mantle Wedge and Slab Input Compositions
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 123 (2013) 218–243 www.elsevier.com/locate/gca Across-arc geochemical variations in the Southern Volcanic Zone, Chile (34.5–38.0°S): Constraints on mantle wedge and slab input compositions G. Jacques a,⇑, K. Hoernle a,b, J. Gill c, F. Hauff b, H. Wehrmann a, D. Garbe-Scho¨nberg d, P. van den Bogaard a,b, I. Bindeman e, L.E. Lara f a Collaborative Research Center (SFB574), University of Kiel and GEOMAR, 24148 Kiel, Germany b GEOMAR Helmholtz Centre for Ocean Research Kiel, 24148 Kiel, Germany c University of California, Santa Cruz, CA 95064, USA d Institute of Geosciences of the University of Kiel, 24118 Kiel, Germany e University of Oregon, Eugene, OR 97403, USA f Servicio Nacional de Geologı´a y Minerı´a, Santiago, Chile Received 7 September 2012; accepted in revised form 13 May 2013; available online 23 May 2013 Abstract Crustal assimilation (e.g. Hildreth and Moorbath, 1988) and/or subduction erosion (e.g. Stern, 1991; Kay et al., 2005) are believed to control the geochemical variations along the northern portion of the Chilean Southern Volcanic Zone. In order to evaluate these hypotheses, we present a comprehensive geochemical data set (major and trace elements and O–Sr–Nd–Hf–Pb isotopes) from Holocene primarily olivine-bearing volcanic rocks across the arc between 34.5°S and 38.0°S, including volcanic front centers from Tinguiririca to Callaqui, the rear arc centers of Infernillo Volcanic Field, Laguna del Maule and Copahue, and extending 300 km into the backarc. -
GEOLOGY of URANIUS THOLUS, MARS. J. B. Plescia, U. S. Geological Survey, 2255 N
Lunar and Planetary Science XXX 1648.pdf GEOLOGY OF URANIUS THOLUS, MARS. J. B. Plescia, U. S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001. The Uranius group of volcanoes in the northeast some ejecta can be traced a short distance onto the part of Tharsis includes Uranius Patera, Uranius northern flank. Tholus, and Ceraunius Tholus; these are among the Numerous closed depressions occur on the flank; smaller and older tholi and paterae. Analysis of they appear rimless and are interpreted to be collapse these constructs is important for understanding the features. In several cases troughs occur down slope nature and style of early volcanism in Tharsis. Pre- from the depressions, but the troughs are not physi- vious studies have considered these volcanoes only in cally connected to the depressions at the surface. a general manner (1, 2). Here the geology of Ura- Several troughs are clearly observed on the flank nius Tholus is presented; Ceraunius Tholus and and additional unresolved troughs are suggested by Uranius Patera are described elsewhere (3). the flank texture. Most troughs begin just below the Uranius Tholus (Table 1) is the smallest and caldera rim; none breach the rim. The heads of most poorly imaged construct of the Uranius group, some troughs are marked by a wider, shallow depres- making geologic analysis difficult. The flanks are sion; others by simple theater-headed end. Troughs characterized by troughs and several large craters; are 600 - 1200 m wide. The southern side of the the summit region by a caldera complex. flank lacks obvious troughs and has a texture sug- gesting the flank is covered with lava flows. -
Rheological Behaviour of Volcanic Granular Flows K
Brigham Young University BYU ScholarsArchive 4th International Congress on Environmental International Congress on Environmental Modelling and Software - Barcelona, Catalonia, Modelling and Software Spain - July 2008 Jul 1st, 12:00 AM Rheological Behaviour of Volcanic Granular Flows K. Kelfoun Follow this and additional works at: https://scholarsarchive.byu.edu/iemssconference Kelfoun, K., "Rheological Behaviour of Volcanic Granular Flows" (2008). International Congress on Environmental Modelling and Software. 281. https://scholarsarchive.byu.edu/iemssconference/2008/all/281 This Event is brought to you for free and open access by the Civil and Environmental Engineering at BYU ScholarsArchive. It has been accepted for inclusion in International Congress on Environmental Modelling and Software by an authorized administrator of BYU ScholarsArchive. For more information, please contact [email protected], [email protected]. iEMSs 2008: International Congress on Environmental Modelling and Software Integrating Sciences and Information Technology for Environmental Assessment and Decision Making 4th Biennial Meeting of iEMSs, http://www.iemss.org/iemss2008/index.php?n=Main.Proceedings M. Sànchez-Marrè, J. Béjar, J. Comas, A. Rizzoli and G. Guariso (Eds.) International Environmental Modelling and Software Society (iEMSs), 2008 Rheological Behaviour of Volcanic Granular Flows K. Kelfoun 1. IRD - Instituto Geofisico, Escuela Politecnica Nacional, Quito, Ecuador 2. Laboratoire Magmas et Volcans - Université Blaise Pascal, CNRS, IRD – OPGC, 5 rue Kessler, 63038 Clermont-Ferrand, France ([email protected]) Abstract Numerical simulations of volcanic granular flows are increasingly being used for hazard assessment on volcanoes and appear to be essential for future hazard mitigation. A potential problem of such an approach, however, is that the rheological behaviour of such flows is very complex and currently impossible to describe fully from a physical point of view.