Wet-Based Glaciation in Phlegra Montes, Mars

Total Page：16

File Type：pdf, Size：1020Kb

Wet-Based Glaciation in Phlegra Montes, Mars

Geophysical Research Abstracts Vol. 18, EGU2016-1541, 2016 EGU General Assembly 2016 © Author(s) 2015. CC Attribution 3.0 License. Wet-based glaciation in Phlegra Montes, Mars. Colman Gallagher (1,2) and Matt Balme (3,4) (1) UCD School of Geography, University College Dublin, Ireland ([email protected]), (2) UCD Earth Institute, University College Dublin, Ireland, (3) Department of Physical Sciences, Open University, UK, (4) Planetary Science Institute, Tucson, USA Eskers are sinuous landforms composed of sediments deposited from meltwaters in ice-contact glacial conduits. This presentation describes the first definitive identification of eskers on Mars still physically linked with their parent system (1), a Late Amazonian-age glacier (∼150 Ma) in Phlegra Montes. Previously described Amazonian-age glaciers on Mars are generally considered to have been dry based, having moved by creep in the absence of subglacial water required for sliding, but our observations indicate significant sub-glacial meltwater routing. The confinement of the Phlegra Montes glacial system to a regionally extensive graben is evidence that the esker formed due to sub-glacial melting in response to an elevated, but spatially restricted, geothermal heat flux rather than climate-induced warming. Now, however, new observations reveal the presence of many assemblages of glacial abrasion forms and associated channels that could be evidence of more widespread wet-based glaciation in Phlegra Montes, including the collapse of several distinct ice domes. This landform assemblage has not been described in other glaciated, mid-latitude regions of the martian northern hemisphere. Moreover, Phlegra Montes are flanked by lowlands displaying evidence of extensive volcanism, including contact between plains lava and piedmont glacial ice. These observations provide a rationale for investigating non-climatic forcing of glacial melting and associated landscape development on Mars, and can build on insights from Earth into the importance of geothermally-induced destabilisation of glaciers as a key amplifier of climate change. (1) Gallagher, C. and Balme, M. (2015). Eskers in a complete, wet-based glacial system in the Phlegra Montes region, Mars, Earth and Planetary Science Letters, 431, 96-109..

Copy Link

Recommended publications

Eskers Associated with Extant Glaciers in Mid-Latitude Graben on Mars: Evidence for Geothermal Controls Upon Recent Basal Melting
Lunar and Planetary Science XLVIII (2017) 1234.pdf ESKERS ASSOCIATED WITH EXTANT GLACIERS IN MID-LATITUDE GRABEN ON MARS: EVIDENCE FOR GEOTHERMAL CONTROLS UPON RECENT BASAL MELTING. F.E.G. Butcher1, C. Gallagher2,3, N.S. Arnold4, M.R. Balme1, S.J. Conway5, S.R. Lewis1, A. Hagermann1. 1School of Physical Sciences, The Open University, UK ([email protected]), 2UCD School of Geography, University College Dublin, Ireland, 3UCD Earth Institute, University College Dublin, Ireland 4Scott Polar Research Institute, University of Cambridge, UK, 5CNRS, LPG Nantes, France. Introduction: Diagnostic evidence for past melting of putative debris-covered glaciers (DCGs) in Mars’ mid-latitudes [e.g. 1-2] is extremely rare. As such, it is widely believed that these DCGs have been perennially frozen to their beds in cold-based thermal regimes [e.g. 3] since their formation ~40 Ma to 1 Ga [4-8]. Here, we present a landsystem model that challenges this paradigm. We identify a sinuous ridge emerging from a DCG in the broad rift zone NE of the Tharsis volcanic province. We interpret this ridge as an esker formed by deposition of sediment within a subglacial meltwater conduit. This is only the second esker-like ridge to be identified in association with a mid-latitude DCG. Re- cent work [9] identified a complex of esker-like ridges on the foreland of an extant DCG in Phlegra Montes, for which high-resolution analysis is ongoing [10]. Significantly, both candidate eskers are located within graben. Graben are topographic troughs formed by crustal extension and are commonly associated with elevated geothermal heat (GH) flux [e.g.
[Show full text]
Eskers in a Complete, Wet-Based Glacial System in the Phlegra
Earth and Planetary Science Letters 431 (2015) 96–109 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Eskers in a complete, wet-based glacial system in the Phlegra Montes region, Mars ∗ Colman Gallagher a,b, , Matthew Balme c,d a UCD School of Geography, University College Dublin, Belfield, Dublin 4, Ireland b UCD Earth Institute, University College Dublin, Belfield, Dublin 4, Ireland c Dept. of Physical Sciences, Open University, Walton Hall, Milton Keynes MK7 6AA, UK d Planetary Science Institute Tucson, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States a r t i c l e i n f o a b s t r a c t Article history: Although glacial landsystems produced under warm/wet based conditions are very common on Earth, Received 30 April 2015 even here, observations of subglacial landforms such as eskers emerging from extant glaciers are rare. Received in revised form 9 September 2015 This paper describes a system of sinuous ridges emerging from the in situ but now degraded piedmont Accepted 14 September 2015 terminus of a Late Amazonian-aged (∼150 Ma) glacier-like form in the southern Phlegra Montes region Available online 29 September 2015 of Mars. We believe this to be the first identification of martian eskers that can be directly linked to their Editor: C. Sotin parent glacier. Together with their contextual landform assemblage, the eskers are indicative of significant Keywords: glacial meltwater production and subglacial routing. However, although the eskers are evidence of a Mars wet-based regime, the confinement of the glacial system to a well-defined, regionally significant graben, glacier and the absence of eskers elsewhere in the region, is interpreted as evidence of sub-glacial melting eskers as a response to locally enhanced geothermal heat flux rather than climate-induced warming.
[Show full text]
16. Ice in the Martian Regolith
16. ICE IN THE MARTIAN REGOLITH S. W. SQUYRES Cornell University S. M. CLIFFORD Lunar and Planetary Institute R. O. KUZMIN V.I. Vernadsky Institute J. R. ZIMBELMAN Smithsonian Institution and F. M. COSTARD Laboratoire de Geographie Physique Geologic evidence indicates that the Martian surface has been substantially modified by the action of liquid water, and that much of that water still resides beneath the surface as ground ice. The pore volume of the Martian regolith is substantial, and a large amount of this volume can be expected to be at tem- peratures cold enough for ice to be present. Calculations of the thermodynamic stability of ground ice on Mars suggest that it can exist very close to the surface at high latitudes, but can persist only at substantial depths near the equator. Impact craters with distinctive lobale ejecta deposits are common on Mars. These rampart craters apparently owe their morphology to fluidhation of sub- surface materials, perhaps by the melting of ground ice, during impact events. If this interpretation is correct, then the size frequency distribution of rampart 523 524 S. W. SQUYRES ET AL. craters is broadly consistent with the depth distribution of ice inferred from stability calculations. A variety of observed Martian landforms can be attrib- uted to creep of the Martian regolith abetted by deformation of ground ice. Global mapping of creep features also supports the idea that ice is present in near-surface materials at latitudes higher than ± 30°, and suggests that ice is largely absent from such materials at lower latitudes. Other morphologic fea- tures on Mars that may result from the present or former existence of ground ice include chaotic terrain, thermokarst and patterned ground.
[Show full text]
Hubbard B, Souness C, Brough S. Glacier-Like Forms on Mars
Hubbard B, Souness C, Brough S. Glacier-like forms on Mars. The Cryosphere 2014, 8, 2047-2061. Copyright: © Author(s) 2014. This work is distributed under the Creative Commons Attribution 3.0 License. DOI link to article: https://doi.org/10.5194/tc-8-2047-2014 Date deposited: 24/11/2017 This work is licensed under a Creative Commons Attribution 3.0 Unported License Newcastle University ePrints - eprint.ncl.ac.uk The Cryosphere, 8, 2047–2061, 2014 www.the-cryosphere.net/8/2047/2014/ doi:10.5194/tc-8-2047-2014 © Author(s) 2014. CC Attribution 3.0 License. Glacier-like forms on Mars B. Hubbard, C. Souness, and S. Brough Department of Geography and Earth Sciences, Aberystwyth University, Aberystwyth, UK Correspondence to: B. Hubbard ([email protected]) Received: 7 May 2014 – Published in The Cryosphere Discuss.: 5 June 2014 Revised: 15 September 2014 – Accepted: 26 September 2014 – Published: 5 November 2014 Abstract. More than 1300 glacier-like forms (GLFs) are lo- concerned and of broader planetary issues such as (i) how cated in Mars’ mid-latitudes. These GLFs are predominantly Mars’ present-day landscape was formed, (ii) the presence composed of ice–dust mixtures and are visually similar to and phase state of H2O on Mars’ surface, and (iii) how Mars’ terrestrial valley glaciers, showing signs of downhill viscous climate has changed in geologically recent times. The aim of deformation and an expanded former extent. However, sev- this paper is to summarize and develop our understanding of eral fundamental aspects of their behavior are virtually un- the fundamental physical glaciology of Mars’ GLFs.
[Show full text]
Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°.
[Show full text]
Solar-System-Wide Significance of Mars Polar Science
Solar-System-Wide Significance of Mars Polar Science A White Paper submitted to the Planetary Sciences Decadal Survey 2023-2032 Point of Contact: Isaac B. Smith ([email protected]) Phone: 647-233-3374 York University and Planetary Science Institute 4700 Keele St, Toronto, Ontario, Canada Acknowledgements: A portion of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). © 2020. All rights reserved. 1 This list includes many of the hundreds of current students and scientists who have made significant contributions to Mars Polar Science in the past decade. Every name listed represents a person who asked to join the white paper or agreed to be listed and provided some comments. Author List: I. B. Smith York University, PSI W. M. Calvin University of Nevada Reno D. E. Smith Massachusetts Institute of Technology C. Hansen Planetary Science Institute S. Diniega Jet Propulsion Laboratory, Caltech A. McEwen Lunar and Planetary Laboratory N. Thomas Universität Bern D. Banfield Cornell University T. N. Titus U.S. Geological Survey P. Becerra Universität Bern M. Kahre NASA Ames Research Center F. Forget Sorbonne Université M. Hecht MIT Haystack Observatory S. Byrne University of Arizona C. S. Hvidberg University of Copenhagen P. O. Hayne University of Colorado LASP J. W. Head III Brown University M. Mellon Cornell University B. Horgan Purdue University J. Mustard Brown University J. W. Holt Lunar and Planetary Laboratory A. Howard Planetary Science Institute D. McCleese Caltech C. Stoker NASA Ames Research Center P. James Space Science Institute N.
[Show full text]
MARTIAN GEOLOGIC "REVOLUTIONS": a TALE of TWO PROCESSES; Kenneth L
LPSC XXI 1237 MARTIAN GEOLOGIC "REVOLUTIONS": A TALE OF TWO PROCESSES; Kenneth L. Tanaka, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001 The antiquated geologic term "revolution" is defined as "A term formerly popular among geologists for a time of profound orogeny and other crustal movements, on a continentwide or even worldwide scale, the assumption being that such revolutions produced abrupt changes in geography, climate, and environment" [I]. The term is little used today because of changes in our definition of "orogeny" and in our understanding of Earth's geologic history. Herein, I informally resurrect the term for Mars, in modified form, because of its suitability to this planet. My definition is "a time of profound geologic activity resulting in global changes in physiography, climate, or environment." On Earth, most surface rocks (except the youngest) record a cumulatively complex geologic history, and their landscapes are largely molded by surficial processes. On Mars, however, structure and topography are more directly the results of volcanism and tectonism. Singular, major volcanic and tectonic events dominated in shaping the surface, and they strongly influenced the planet's environment. Impact cratering has also had a major role in the geology of Mars, and geologic revolutions related to cratering events may be proposed. However, here I examine only those revolutions apparently or possibly related to volcanism and tectonism, because I am reviewing the thrust of work from NASA's research project "Mars: Evolution of Volcanism, Tectonism, and Volatiles." Below I outline three possible revolutions on Mars that are based on geologic evidence. Each includes uncertainties in such fundamental aspects as origin, nature and sequence of events, and environmental significance.
[Show full text]
Phlegra Montes, Mars
46th Lunar and Planetary Science Conference (2015) 1371.pdf PHLEGRA MONTES, MARS: CHRONOLOGY AND DENUDATION RATES S. van Gasselt1, A.-P. Rossi2, C. Orgel1;3, J. Schulz1. 1Freie Universität Berlin, Department of Earth Sciences, D–12249 Berlin, Germany ([email protected]); 2Jacobs University Bremen, Earth and Space Sciences, D–28759 Bremen, Germany; 3Eötvös Loránd University, Department of Geology, Budapest, 1053 Hungary. Background: The Phlegra Montes are located north– MO THEMIS (VIS/IR) instruments [14]. Topography is east of the Elysium rise (165◦E, 29.5–51.0◦N) and form derived using (a) gridded MGS Mars Orbiter Laser Alti- a 1,250 km long topographically well-pronounced ar- meter (MOLA) data [15, 16], (b) photogrammetrically– cuate ridge composed of Hesperian to Noachian–aged derived stereo information from HRSC [17, 18] (abso- remnant massifs [1] with associated debris aprons and lute and regional scales) and (c) photoclinometrically- lineated valley fill features (fig. 1). Considered to be of derived information using observation– and illumination– endogenic tectonic origin in earlier work [2], the Phlegra geometries (relative and local scales). Montes have recently been interpreted as unit composed Our primary aim is the systematic assessment of repres- 0:04 of degraded Hesperian–aged (3.650:06 Gyr (eHt) and entative surface ages using impact–crater size–frequency 0:06 3.710:10 Gyr (lHt)), and Noachian- to Hesperian–aged statistics with recent chronology models and definition of 0:05 0:08 (3.770:07–3.910:18 Gyr HNt) material of potentially vol- the Martian impact-crater production function described canic origin pre–dating the Hesperian plains–forming in [19].
[Show full text]
Ali M. Bramson CV
Curriculum Vitae – Current as of September 14, 2021 Prof. Ali M. Bramson Purdue University [email protected] Dept. of Earth, Atmospheric, and Planetary Sciences (EAPS) +1 (765) 494-0279 550 Stadium Mall Dr. West Lafayette, IN 47907 www.eaps.purdue.edu/bramson EDUCATION University of Arizona, Tucson, AZ 2012–2018 Ph.D. Planetary Sciences, minor in Geosciences (Aug. 2018) M.S. Planetary Sciences (Dec. 2015) University of Wisconsin-Madison, Madison, WI 2007–2011 B.S. Physics and Astronomy-Physics, certificate (minor) in Computer Science (Dec. 2011) Graduated with distinction (honor’s thesis); named on UW’s Dean’s List 6 semesters PROFESSIONAL POSITIONS HELD Assistant Professor Aug. 2020–present Department of Earth, Atmospheric and Planetary Sciences (EAPS), Purdue University Postdoctoral Research Associate Sept. 2018–Aug. 2020 Lunar & Planetary Laboratory (LPL), University of Arizona Advisor: Prof. Lynn Carter Graduate Research Associate Aug. 2012–Aug. 2018 Lunar & Planetary Laboratory, University of Arizona Advisor: Prof. Shane Byrne Dissertation Title: “Radar Analysis and Theoretical Modeling of the Presence and Preservation of Ice on Mars” Undergraduate Research Assistant Dec. 2008–May 2012 Astronomy Department, University of Wisconsin-Madison Advisor: Prof. Eric M. Wilcots Senior Thesis Title: “Using networking algorithms to assess the environments of galaxy groups” REU Student June 2010–Aug. 2010 SETI Institute Advisor: Dr. Cynthia Phillips Searching for ongoing geologic activity on Jupiter’s satellites REU Student May 2009–Aug. 2009 Arecibo Observatory/Cornell University Advisors: Dr. Michael Nolan and Dr. Ellen Howell Modeling of 25143 Itokawa to improve radar-based shape estimation methods Undergraduate Research Assistant June 2007–May 2009 Nanoscale Science and Engineering Center (NSEC), University of Wisconsin-Madison 1 Ali M.
[Show full text]
Phlegra Montes: Candidate Landing Site with Shallow Ice for Human Exploration
Seventh Mars Polar Science Conf. 2020 (LPI Contrib. No. 2099) 6008.pdf PHLEGRA MONTES: CANDIDATE LANDING SITE WITH SHALLOW ICE FOR HUMAN EXPLORATION. A.S. McEwen1 S.S. Sutton1, A.M. Bramson1, S. Byrne1, E.I. Petersen1, J.S. Levy2, M.P. Golombek3, N.R. Williams3, N.E. Putzig4 1LPL, Univ. Arizona, 2Colgate Univ., 3JPL, Caltech, 4PSI. Introduction: Human exploration and settlement [4]. The hills are heavily modified by glacial flow of Mars is of interest to SpaceX [1] as well as NASA, landforms, some of which have radar-sounding re- ESA, and CNSA (China). H2O is essential for drink- turns interpreted as nearly pure ice under a debris ing, growing food, and producing oxygen and hydro- layer [5–8]. The bedrock composition is poorly gen, but avoiding polar regions is important to keep known because of Amazonian modification, but ba- temperatures moderate and for solar power. saltic compositions have been detected in nearby Ere- MRO/HiRISE working with JPL has been imaging bus Montes [9]. candidate landing sites for SpaceX. This effort is fo- cused on the northern mid-latitudes because of low altitudes, the known presence of shallow ice down to 39°N [2], and milder winters than the southern middle latitudes. Human Mars landers will likely target flat landing sites (slopes <5°) that are relatively free of large boulders and dust. Based on topographic data and HiRISE images, two regions stand out as most promising: Arcadia Planitia and Phlegra Montes (Fig. 1). Arcadia Planitia is especially flat and has extensive apparently boul- der-free areas. Phlegra Montes probably also has doz- Figure 2: HRSC perspective view of a portion of ens of acceptable areas (>200 m diameter) plus other southern Phlegra Montes.
[Show full text]
Martian Geomorphology and Its Relation to Subsurface Volatiles
MECA Special Session at LPSC XVII: MARTIAN GEOMORPHOLOGY AND ITS RELATION TO SUBSURFACE VOLATILES MECA MECA Special Session at LPSC XVII: MARTIAN GEOMORPHOLOGY AND ITS RELATION TO SUBSURFACE VOLATILES edited by Stephen M. Clifford, Lisa A. Rossbacher, and James R. Zimbelman Sponsored by The Lunar and Planetary Institute Hosted by The NASA/Johnson Space Center March 17, 1986 Lunar and Planetary Institute 3303 NASA Road 1 Houstot1, Texas 77058-4399 LPI Technical Report 87 -02 Compiled in 1987 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Clifford S. M., Rossbacher L. A., and Zimbelman J. R., eds. (1987) MECA Special Session at LPSC XVII: Martian Geomorphology and its Relation to SubsurJace Volatiles. LPI Tech. Rpt. 87-{)2. Lunar and Planetary Institute, Houston. 51 pp. Papers in this report may be cited as: Author A. A. (1986) Title of paper. In MECA Special Session at LPSC XVI!: Martian Geomorphology and its Relation to SubsurJace Volatiles (S. M. Clifford et aI., eds.), pp. XX- YY. LPI Tech Rpt. 87-{)2. Lunar and Planetary Institute, Houston. This report is distributed by: LIBRARY/ INFORMATION CENTER Lunar and Planetary Institute 3303 NASA Road I Houston, TX 77058-4399 Mail order requestors will be invoicedJor the cost oJpostage and handling.
[Show full text]
Recent Basal Melting of a Mid-Latitude Glacier on Mars Frances Butcher, M
Recent Basal Melting of a Mid-Latitude Glacier on Mars Frances Butcher, M. Balme, C. Gallagher, N. Arnold, S. Conway, A. Hagermann, S. Lewis To cite this version: Frances Butcher, M. Balme, C. Gallagher, N. Arnold, S. Conway, et al.. Recent Basal Melting of a Mid-Latitude Glacier on Mars. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2017, 122 (12), pp.2445-2468. 10.1002/2017JE005434. hal-02270617 HAL Id: hal-02270617 https://hal.archives-ouvertes.fr/hal-02270617 Submitted on 26 Aug 2019 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. PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Recent Basal Melting of a Mid-Latitude 10.1002/2017JE005434 Glacier on Mars Key Points: Frances E. G. Butcher1 , M. R. Balme1, C. Gallagher2,3, N. S. Arnold4, S. J. Conway5, • We identify a candidate esker 1 1 emerging from a late A. Hagermann , and S. R. Lewis Amazonian-aged (~110 Ma) 1 2 mid-latitude debris-covered glacier School of Physical Sciences, Open University, Milton Keynes, UK, UCD School of Geography, University College Dublin, 3 4 in Tempe Terra, Mars Dublin 4, Ireland, UCD Earth Institute, University College Dublin, Dublin 4, Ireland, Scott Polar Research Institute, • Eskers form in ice-contact meltwater University of Cambridge, Cambridge, UK, 5CNRS, UMR 6112 Laboratoire de Planétologie et Géodynamique, Université de conduits.
[Show full text]