Volcanoes and the Frequency and Style of Their Eruptions (A Geological Problem)

Total Page:16

File Type:pdf, Size:1020Kb

Volcanoes and the Frequency and Style of Their Eruptions (A Geological Problem) Prediction of Volcanic Eruptions Vo s l c e Long Term Prediction a no Identify volcanoes and the frequency and style of their eruptions (a geological problem). Establish probabilities of eruption, style and location for Part II individual volcanoes. Prediction Establish the level of risk based on historic and geologic Impact of eruptions record. Supervolcanoes E.g., for individual volcanoes: determine most likely routes Volcanoes in space for lahars, nuees ardentes, lava flows, etc., and avoid construction in those areas. Hazard zones have been distinguished around Mt. Shasta Hazard zones have been distinguished around Mt. Shasta based on topography and past experience with eruptions. based on topography and past experience with eruptions. Zone 1: areas likely to be affected Zone 1: areas likely to be affected Zone 1 most frequently. Most future flows Zone 2 most frequently. Most future flows from summit eruptions probably from summit eruptions probably would stay within this zone. would stay within this zone. Zone 2: areas likely to be affected by lava flows erupted from vents on the flank of the volcano or that move into zone 2 from zone 1. Short-term prediction Hazard zones have been distinguished around Mt. Shasta based on topography and past experience with eruptions. Based on the recognition of a pattern of events prior to Zone 1: areas likely to be affected previous eruptions. Zone 3 most frequently. Most future flows from summit eruptions probably Gas emissions: rates of emission and type of gas changes in would stay within this zone. some volcanoes. Zone 2: areas likely to be affected Important gases include sulfur dioxide (SO2) and carbon by lava flows erupted from vents dioxide (CO ) on the flank of the volcano or that 2 move into zone 2 from zone 1. Changes in concentration may reflect movement of the Zone 3: areas likely to be affected magma up the vent. infrequently and then only by long lava flows that originate at vents in zones 1 and 2 1 Surface tilting: recognition of changes in the land Earthquakes: generated as the magma moves up the surface due to building pressure in the conduit. feeder conduit to the vent. A surface bulge appeared on Mt. St. Helens prior to its eruption. When viscous magma becomes stuck in the conduit strain April 8, 1980 energy builds as more magma tries to push out. Movement takes place in a series of “jerks” as the rock material breaks. Each “jerk” produces an earthquake. Magnitudes generally less than 5 M. April 26 May 2 The more earthquakes the further the magma has moved. Mount Spurr, Alaska: The 1992 Eruption of Crater Peak Vent A combination of approaches is likely the key to short-term prediction. Black bars: earthquake USGS frequency. Red lines: volcanic eruptions. The impact of volcanic eruptions Volcanic Hazards Lava flows Commonly destroy property in Hawaii and Iceland. Damage limited to the vicinity in the immediate area of the volcano. Fatalities rare due to slow speed of advancing lava flow. 2 Ash fall An ashfall 10 million years ago killed these rhinos that are preserved at Ashfall Fossil Beds State Historic Park, Nebraska. Extensive property damage and fatalities can result from heavy ash falls. Death was not by burial but by lung failure due to inhaling the ash. Significant ash in the upper atmosphere can circle the globe in a matter of weeks. More than 80 commercial jets have been damaged by flying through volcanic ash clouds. Mt. St. Helens’ ash cloud Pyroclastic flows Lahars can be the most devastating outcome of many volcanoes. Lahars are fast moving mudflows that can inundate urban areas that are nearby the eruption. A relatively small eruption of Nevada del Ruiz, Columbia, in 1985, generated a lahar when the volcano melted a 2.5 km2 area of snow and ice. Lahars can also dam rivers and which can lead to extensive flooding. Water and debris rushed down the slopes, picking up more debris along the way. A 5 metre wall of water and debris Nuée ardentes destroy life and property in their paths. slammed into the town of Amero, 72 km from the volcano. 60 people, thousands of animals and fish, and hundreds of acres of lumber were destroyed by ash flows from Mt. St. Helens. A Nuée Ardent killed 20,000 people when Mt. Vesuvius The lahar killed exploded and shed a pyroclastic flow across the village 28,700 people and of Pompeii in 79 AD. destroyed over 5,000 structures in the city. 3 Landslides People and animals Landslides can be generated when a volcano collapses died instantly from the during an eruption. rushing cloud of hot gas and ash. During the Mt. St. Helens eruption 2.3 km3 of debris slid down the mountain at speeds up to 240 km/hr. The slide traveled over 24 km and left a 45 m deep deposit. 350,000 years ago Mt. Shasta experienced a similar eruption and landslide that was 20 times greater than that of Mt. St. Helens. Volcanic Gases SO2 emissions can have direct effects on life in the vicinity of a volcano. In addition to making magma more explosive, volcanic eruptions also include gases that can be deadly to all life. An eruption in 1783 of Laki Crater (Iceland) produced a sulfurous haze that lasted for 9 months and killed 75% of all livestock and 24% of the Icelandic population. Volcanoes release more than 130 to 230 million tonnes of CO2 into the atmosphere every year Humans add CO2 at the rate of approximately 22 billion tonnes per year (150 times the rate of volcanic production) CO , SO and CO are the most abundant of harmful gases. 2 2 Human CO2 production is equal to that if 17,000 volcanoes like Kilauea were erupting every year. Mammoth Mountain is If the air that we breath has more than 10% CO2 it a relatively young becomes deadly because it displaces the Oxygen that we volcano that is emitting need for respiration. large volumes of CO2. Lake Nios, Cameroon, is a very deep lake within a volcanic crater. The lake is so deep that hydrostatic pressure forces CO2 to remain at the lake bottom. When the pressure of the CO2 exceeds a certain limit the Gas concentrations in the soil in gas rapidly bubbles up out of the lake and flows as an some areas near the mountain are invisible gas cloud down the adjacent slopes. high enough to kill trees and small animals. On August 61, 1986 such a gas release flowed 19 km suffocating 1,700 people along its route. 4 Tsunamis Lake Nyos 10 days after the 1986 eruption Caused by the displacement of seawater by eruptions of volcanic islands and submarine volcanoes. Krakatoa (1883 eruption) killed 36,000 people by the tsunami, alone (the most deadly outcome of the eruption). The fountain in the This is the newly forming background lifts CO 2 summit of Krakatoa, growing up to the surface so where the 1883 eruption blew that it no longer the top off of the original accumulates. volcano. Global Climate Change A series of eruptions of Tambora (Indonesia) extruded up to 150 km3 of magma (solid equivalent), much of it into the Due to ash and gas that may spend years in the upper atmosphere. atmosphere; reduces incoming solar radiation. SO2 from an eruption forms tiny droplets of sulfuric acid in the upper atmosphere. The droplets significantly increase global albedo…..a negative radiative forcing that leads to cooling. Tambora (1815 eruption) was followed in 1816 by the “year without a summer”. Mt. Pinatubo (1991) released 22 million metric tons of SO 2 Average global temperature is estimated to have been and reduced the Earth’s average temperature by 0.5 reduced by 3 degrees Celsius. degrees Celsius in the year following the eruption. In June of 1816 there was widespread snowfall throughout Approximately 260,000 people have been killed by volcanoes in the eastern United States. historic times…most by a handful of individual eruptions. The normal growing season experienced repeated frosts as cold air extended much more southerly than normal. Food shortages and starvation are attributed to the deaths of 80,000 people. The global population was about 1 billion people in 1816. Our current population is a little over 6 billion. The 1816 fatality rate would have resulted in a death toll of nearly 500,000 people due to starvation. 5 Volcanic Explosivity Index http://pubs.usgs.gov/publications/msh/comparisons.html Deadly Historic Volcanic Eruptions An eruption in 1902 following the growth of a lava dome on the side Mt. Pelée of the mountain. (West Indes) VEI = 4 Lava domes are constructed of A stratovolcano along viscous lava and are prone to the Caribbean trench. collapse, unleashing a violent pyroclastic flow. The nuée ardente that was generated when Mt. Pelée erupted swept 6 km downslope through the town of St. Vincent. 6 Tambora (1815) VEI = 7 Almost the entire population of 30,000 The largest eruption of historic time. people were killed within minutes of Greatest impacts from pyroclastic flows and inhaling the hot gases ash and gas eruptions. and ash. Approximately 150 km3 of ash was erupted with the explosions. There were only two survivors; one was in a 10,000 people were killed by bomb impacts, tephra falls and dungeon! pyroclastic flows. By far the largest impact was on the Earth’s atmosphere. The eruption plume reached 44 km above the earth, loading the stratosphere with ashes and gases. Krakatoa (1883) VEI = 6 The concentration mercury On the Island of Rakata, Krakatoa was one of in ice cores from glaciers in 130 active volcanoes in Indonesia (the country Wyoming record a peak in with the most active volcanoes in the world).
Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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).
    [Show full text]
  • Mars Frontier
    THE MARS FRONTIER Vol. 12 Voyage of Discovery Copyright © 2009 Robert H. Stockman All rights reserved Contents 1. Ball Game 2 2. Stamford 20 3. Washington 40 4. Houston 51 5. Beijing 73 6. Paris 81 7. Kourou 94 8. Outbreak 105 9. Tie Your Camel 126 10. Conflagration 142 11. Arrival 157 12. Welcomes 173 13. Looking to the Future 193 14. The Prize 208 15. Dawes 219 16. Trials 230 17. Crises 248 18. Uzboi 267 19. Dedication 287 20. Equinox 296 1 1. Ball Game early Jan. 2059 “La vostra partecipazione a Progetto del Nuovo Mondo porterà grandi benefici a tutta l'umanità. Grazzi.” Will Elliott repeated the last sentence of the Italian version of his “stump speech” slowly, carefully, deliberately. Reading the speech at about one third his usual speed, his accent really wasn’t bad. Computerized editing would take his ploddings, squeeze out the extra time, add rhythms and intonations from his English version, and produce something that made him sound almost like a native speaker. Such was the power of mid twenty-first century computer technology and the cultural expectations that drove it. He paused to look at the 3-d screen on the wall near his desk. It was set on “porthole” mode; he could see Earth in the middle, about a third the diameter of the moon as it appeared from Earth. They were still a million kilometers out, a day from aerocapture into an elliptical orbit around the home world. The image looked real; the half that was illumined by the sun was even so bright that it made his eyes water slightly.
    [Show full text]
  • Back Matter (PDF)
    Index Page numbers in italics refer to Figures and Tables martian classification 333-6 Aci San Antonio 182 deformation 336-7 Acicatena 182-3 flank structures 337-9 Aciplatani 183-4 gravitational collapse 340-3 Aeolian Islands regional studies Alicudi 12 Elysium 323-7 see also Stromboli Hellas 327-30 Alaska 1, 3, 11, 12, 17 Syrtis Major 330-2 Alba Patera 319-20, 334, 335, 336, 339 Tharsis 313-23 Albor Tholus 323, 324-5 334, 335, 336, 339 rift zones 339-40 Alicudi 12 sizes 332-3 Alpha Regio 352, 358 morphology classification 308 Amphitrites Patera 327-9, 334, 337 problems of interpretation 308-10 analogue modelling related slides 276-7 landslides 302-4 California 83 Andean volcanoes 1 Campi Flegri 83, 263 Antarctica see Deception Island Canarian Archipeligo (Canary Islands) 1, 5, 8, 12 Apollinaris Patera 325-6, 334, 335, 336, 337, 338 mass wasting 128 Arsia Mons 36, 37, 316-18, 334, 335, 336, 337, 338, 339 rift features 125-8 Arsia-type caldera 335-6 geometry 129 Ascraeus Mons 37, 38, 319, 334, 335, 336, 337, 338, stresses in 128-9 339, 341 setting 125 aseismic creep 179-80 slides 281 Etna study volcanic activity 125 measurement sites 181-6 volcanic hazard assessment 131-4 significance of results 186-90 see also E1 Hierro; Fuerteventura; Gran Canaria; Atla Regio 353, 356, 357, 364, 369 La Gomera; La Palma; Lanzarote; Tenerife Augustine Island (Alaska) 1, 3, 11, 12, 17 Caribbean Avalancha del Zarzo 366, 368 tsunami hazard 115 Ayacata Formation 86, 87 quantification 120-2 Cascades Range see Mount Adams; Mount Rainier; Bandai-type collapse 77-8 Mount St Helens basalt Casita 99 influence on stability 48-9 Cavoni 55, 60 shield volcano landslides 295 Ceraunius Tholus 321-2, 334, 335, 336, 339, 343 Basaltic Shield Formation (BSF) 255 Chilean volcanoes basement Hudson 245.
    [Show full text]
  • 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.
    [Show full text]
  • A Study of the Relative Ages of Olympus Mons, Uranius Tholus, Euripus Mons, and Hecates Tholus
    A Study of the Relative Ages of Olympus Mons, Uranius Tholus, Euripus Mons, and Hecates Tholus Supai Middle School 7th Grade Science Investigations Class May, 2011 Introduction & Hypotheses Science Question: What is the difference in the relative ages of Olympus Mons, Uranius Tholus, Euripus Mons, and Hecates Tholus and their respective cones, calderas, and flanks? Our science question is important because, by finding an answer, we will be able to piece together some of the history of the formation of Martian landscape, which could help us understand if there is a cycle in the formation of volcanoes over time, and if this would also apply to Earth, as well as Mars. This query intrigues us, because its answer will allow us to gain further knowledge of Mars and its geological properties, which will possibly aid further studies into this topic, or pertaining to, these four volcanoes. From previous research, we hypothesize that Uranius Tholus is the oldest volcano. Also, based on the amount of craters that we have found on its surface, we believe that Olympus Mons is the youngest. Background First, we will state all what we learned while we were collecting data for our experimental design. We learned that a volcano is a formation made of the planet’s crust which contains lava and releases out of a caldera (the top part of the volcano). The lava then flows down the cone, or the rising part between the caldera and flank. The flank would be the outer most rim where lava stopped flowing. Magma is lava that has yet to reach a planets surface and is in the mantle.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Volcanism on Mars
    Papers Presented to the NASA MEVI'V Program Working Group Meeting: Volcanism on Mars Oahu, Hawaii June 27-30, 1988 Sponsored by Lunar and Planetary Institute Hosted by University of Hawaii at Manoa LPI Contrihutinn No. 660 Material in this volume may be copied without restraint for library, abstract service, educational, or research purposes; however, republication of any paper or portion thereof requires written permission from the author as well as appropriate acknowledgment of this publication. Preface Welcome to Hawaii! Contained within are the abstracts that were received in response to our announcement of the working group meeting. As you know, the purpose of the MEVTV program is to further the understanding of volcanism, tectonism, and volatiles on Mars, and to explore the interactions among these processes. The purpose of this working group meeting is to focus predominantly on volcanism on Mars, prior to considering the more complex Issues of interactions between volcanism and tectonism or between volcanism and global or regional volatile evolution. We also hope to identify the topical areas of research that will aid the planetary geology community in understanding volcanism on Mars and its relationship to other physical processes. We wish you a stimulating and enjoyable stay in Hawaii! The Working Group Committee TABLE OF CONTENTS Eruptive Viscosity and Volcano Morphology S. B. Posin and R. Greeley ............................................................................. 1 Faulting and its Relation to Volcanism: Mars' Western Equatorial Region D. H. Scott and J. Dohm ................................................................................. 5 Lava Thicknesses: Implications for Rheological and Crustal Development C. R. J. Kilburn and R. M. C. Lopes ............................................................. 9 Mars: Volcanism in the Valles Marineris Overlooked? B.
    [Show full text]
  • 15. Volcanic Activity on Mars
    15. Volcanic Activity on Mars Martian volcanism, preserved at the surface, composition), (2) domes and composite cones, is extensive but not uniformly distributed (Fig. (3) highland paterae, and related (4) volcano- 15.1). It includes a diversity of volcanic land- tectonic features. Many plains units like Lu- forms such as central volcanoes, tholi, paterae, nae Planum and Hesperia Planum are thought small domes as well as vast volcanic plains. to be of volcanic origin, fed by clearly defined This diversity implies different eruption styles volcanoes or by huge fissure volcanism. Many and possible changes in the style of volcanism small volcanic cone fields in the northern plains with time as well as the interaction with the are interpreted as cinder cones (Wood, 1979), Martian cryosphere and atmosphere during the formed by lava and ice interaction (Allen, evolution of Mars. Many volcanic constructs 1979), or as the product of phreatic eruptions are associated with regional tectonic or local (Frey et al., 1979). deformational features. An overview of the temporal distribution of Two topographically dominating and mor- processes, including the volcanic activity as phologically distinct volcanic provinces on Mars well as the erosional processes manifested by are the Tharsis and Elysium regions. Both are large outflow channels ending in the northern situated close to the equator on the dichotomy lowlands and sculpting large units of the vol- boundary between the cratered (older) high- canic flood plains has been given by Neukum lands and the northern lowlands and are ap- and Hiller (1981). This will be discussed in proximately 120◦ apart. They are characterized this work together with new findings.
    [Show full text]
  • Mars Upside Down 14 December 2017
    Mars upside down 14 December 2017 1 / 4 This stunning image swath was taken by ESA’s Mars Express during camera calibration as the spacecraft flew over the north pole (bottom) towards the equator (top). Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO Which way is up in space? Planets are usually shown with the north pole at the top and the south pole at the bottom. In this remarkable image taken by ESA's Mars Express, the Red Planet is seen with north at the bottom, and the equator at the top. The image was taken on 19 June for calibrating the high-resolution stereo camera, while Mars Express was flying from north to south. The camera's nine channels – one downward-pointing, four colour and four stereo – panned over the surface to record a large area with the same illumination conditions. At This base map from NASA’s Viking mission shows the the same time, the camera was shifted to the context of an associated image release outlined by the horizon, instead of just pointing to the surface as in large highlighted central swath. A number of the routine imaging. volcanoes seen in the image are labelled, as well as Olympus Mons, which lies outside of the main image The result is this rare wide-angle view of the planet, release, for context. Credit: NASA/Viking, FU Berlin with the illuminated horizon near the equator at the top of the image, and the shadowed north pole at the bottom. Panning south, the view soaks up sights of some of the planet's largest volcanoes in the Tharsis region.
    [Show full text]