Remarkable Geochemical Changes and Degassing at Voui Crater Lake, Ambae Volcano, Vanuatu
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Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Crater Gradation in Gusev Crater and Meridiani Planum, Mars J
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, E02S08, doi:10.1029/2005JE002465, 2006 Crater gradation in Gusev crater and Meridiani Planum, Mars J. A. Grant,1 R. E. Arvidson,2 L. S. Crumpler,3 M. P. Golombek,4 B. Hahn,5 A. F. C. Haldemann,4 R. Li,6 L. A. Soderblom,7 S. W. Squyres,8 S. P. Wright,9 and W. A. Watters10 Received 19 April 2005; revised 21 June 2005; accepted 27 June 2005; published 6 January 2006. [1] The Mars Exploration Rovers investigated numerous craters in Gusev crater and Meridiani Planum during the first 400 sols of their missions. Craters vary in size and preservation state but are mostly due to secondary impacts at Gusev and primary impacts at Meridiani. Craters at both locations are modified primarily by eolian erosion and infilling and lack evidence for modification by aqueous processes. Effects of gradation on crater form are dependent on size, local lithology, slopes, and availability of mobile sediments. At Gusev, impacts into basaltic rubble create shallow craters and ejecta composed of resistant rocks. Ejecta initially experience eolian stripping, which becomes weathering-limited as lags develop on ejecta surfaces and sediments are trapped within craters. Subsequent eolian gradation depends on the slow production of fines by weathering and impacts and is accompanied by minor mass wasting. At Meridiani the sulfate-rich bedrock is more susceptible to eolian erosion, and exposed crater rims, walls, and ejecta are eroded, while lower interiors and low-relief surfaces are increasingly infilled and buried by mostly basaltic sediments. Eolian processes outpace early mass wasting, often produce meters of erosion, and mantle some surfaces. -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Mars Science Laboratory: Curiosity Rover Curiosity’S Mission: Was Mars Ever Habitable? Acquires Rock, Soil, and Air Samples for Onboard Analysis
National Aeronautics and Space Administration Mars Science Laboratory: Curiosity Rover www.nasa.gov Curiosity’s Mission: Was Mars Ever Habitable? acquires rock, soil, and air samples for onboard analysis. Quick Facts Curiosity is about the size of a small car and about as Part of NASA’s Mars Science Laboratory mission, Launch — Nov. 26, 2011 from Cape Canaveral, tall as a basketball player. Its large size allows the rover Curiosity is the largest and most capable rover ever Florida, on an Atlas V-541 to carry an advanced kit of 10 science instruments. sent to Mars. Curiosity’s mission is to answer the Arrival — Aug. 6, 2012 (UTC) Among Curiosity’s tools are 17 cameras, a laser to question: did Mars ever have the right environmental Prime Mission — One Mars year, or about 687 Earth zap rocks, and a drill to collect rock samples. These all conditions to support small life forms called microbes? days (~98 weeks) help in the hunt for special rocks that formed in water Taking the next steps to understand Mars as a possible and/or have signs of organics. The rover also has Main Objectives place for life, Curiosity builds on an earlier “follow the three communications antennas. • Search for organics and determine if this area of Mars was water” strategy that guided Mars missions in NASA’s ever habitable for microbial life Mars Exploration Program. Besides looking for signs of • Characterize the chemical and mineral composition of Ultra-High-Frequency wet climate conditions and for rocks and minerals that ChemCam Antenna rocks and soil formed in water, Curiosity also seeks signs of carbon- Mastcam MMRTG • Study the role of water and changes in the Martian climate over time based molecules called organics. -
New Insights Into Crater Obliteration in the Noachian Highlands of Mars
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1649.pdf New Insights into Crater Obliteration in the Noachian Highlands of Mars. Samuel J. Holo and Edwin S. Kite University of Chicago, Department of Geophysical Sciences, Chicago, IL, 60637 – [email protected] Introduction: The Noachian highlands of Mars are Datasets and hypotheses: We used a global geo- heavily-cratered terrain that, in their geology, record logic map of Mars [10] and 2 pixel-per-degree (ppd) pre-valley-network Mars, the climate of which remains gridded MOLA data to generate a 2ppd map of Noa- enigmatic (e.g. [1]). The majority of craters on Noa- chian highland units (eNh, mNh and lNh) with their as- chian terrain are degraded (e.g. [2]), and several aspects sociated elevations (smoothed by nearest-neighbor av- of the Noachian highland landscape can be explained by eraging to avoid sampling crater bottoms). Combination the interplay of impact cratering and erosion of crater of this map with a global database of Martian craters rims by fluvial erosion [3,4]. Further, examination of the [11] enables us to ask four main questions: latitudinal/elevational trends in crater density and mor- • Is there a signal of a latitude control on crater phometric properties has prompted studies on the his- obliteration? tory of climatic forcing on crater modification and deg- • Is there a signal of an elevation control on radation (e.g. [2,5]). crater obliteration? The size-frequency distribution (SFD) of craters in • Does the degradation of equatorial craters on the Noachian highlands exhibits a paucity of craters < Noachian terrain leave a measurable signal of ~32 km in diameter, relative to extrapolation from spatial clustering relative to fresh craters? isochron fits to larger craters (e.g. -
Amphipod Newsletter 39 (2015)
AMPHIPOD NEWSLETTER 39 2015 Interviews BIBLIOGRAPHY THIS NEWSLETTER PAGE 19 FEATURES INTERVIEWS WITH ALICJA KONOPACKA AND KRZYSZTOF JAŻDŻEWSKI PAGE 2 MICHEL LEDOYER WORLD AMPHIPODA IN MEMORIAM DATABASE PAGE 14 PAGE 17 AMPHIPOD NEWSLETTER 39 Dear Amphipodologists, Statistics from We are delighted to present to you Amphipod Newsletter 39! this Newsletter This issue includes interviews with two members of our amphipod family – Alicja Konopacka and Krzysztof Jazdzewski. Both tell an amazing story of their lives and work 2 new subfamilies as amphipodologists. Sadly we lost a member of our amphipod 21 new genera family – Michel Ledoyer. Denise Bellan-Santini provides us with a fitting memorial to his life and career. Shortly many 145 new species members of the amphipod family will gather for the 16th ICA in 5 new subspecies Aveiro, Portugal. And plans are well underway for the 17th ICA in Turkey (see page 64 for more information). And, as always, we provide you with a Bibliography and index of amphipod publications that includes citations of 376 papers that were published in 2013-2015 (or after the publication of Amphipod Newsletter 38). Again, what an amazing amount of research that has been done by you! Please continue to notify us when your papers are published. We hope you enjoy your Amphipod Newsletter! Best wishes from your AN Editors, Wim, Adam, Miranda and Anne Helene !1 AMPHIPOD NEWSLETTER 39 2015 Interview with two prominent members of the “Polish group”. The group of amphipod workers in Poland has always been a visible and valued part of the amphipod society. They have organised two of the Amphipod Colloquia and have steadily provided important results in the world of amphipod science. -
Ancient Fluid Escape and Related Features in Equatorial Arabia Terra (Mars)
EPSC Abstracts Vol. 7 EPSC2012-132-3 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 Ancient fluid escape and related features in equatorial Arabia Terra (Mars) F. Franchi(1), A. P. Rossi(2), M. Pondrelli(3), B. Cavalazzi(1), R. Barbieri(1), Dipartimento di Scienze della Terra e Geologico Ambientali, Università di Bologna, via Zamboni 67, 40129 Bologna, Italy ([email protected]). 2Jacobs University, Bremen, Germany. 3IRSPS, Università D’Annunzio, Pescara, Italy. Abstract Noachian [1]. The ELDs are composed by light rocks showing a polygonal pattern, described elsewhere on Arabia Terra, in the equatorial region of Mars, is Mars [4], and is characterized by a high sinuosity of long-time studied area especially for the abundance the strata that locally follows a concentric trend of fluid related features. Detailed stratigraphic and informally called “pool and rim” structures (Fig. morphological study of the succession exposed in the 1A). Crommelin and Firsoff craters evidenced the occurrences of flow structures and spring deposits that endorse the presence of fluids circulation in the Late Noachian. All the morphologies in these two proto-basins occur within the Equatorial Layered Deposits (ELDs). 1. Introduction Martian layered spring deposits are of considerable interest for their supposed relationship with water and high potential of microbial signatures preservation. Their supposed fluid-related origin [1] makes the Equatorial Layered Deposits attractive targets for future missions with astrobiological purposes. In this study we report the occurrence of mounds fields and flow structures in Firsoff and Crommelin craters and summarize the result of a detailed study of the remote-sensing data sets available in this region. -
Terrestrial Planets
Terrestrial Planets First ever ‘whole Earth’ picture from deep space, taken by Bill Anders on Apollo 8 Apollo 8 crew, Bill Anders centre: The Earth is just a planet courtesy Nasa 1- 4 from the Sun Image courtesy: http://commons.wikimedia.org/wiki/Image:Terrestrial_planet_size_comparisons_edit.jpg Mercury, Venus, Earth and Mars are four astonishingly different planets Mercury and Venus have only been seen in any detail within the last 30 years Mercury in sight Courtesy NASA (Mariner 10) Mercury is visible only soon after the setting sun or shortly before dawn the Mariner 10 probe (1974/75) is the source of most information about Mercury – Messenger, launched 2004, first flypast in 2008 and orbit Mercury in 2011. ESA’s BepiColombo, to be launched in 2013 Mercury Mercury is like the Earth inside and the Moon outside Mercury has had a cooling and bombardment history similar to the moon It appears as cratered lava with scarps Its rocks are Earth-like Mariner 10 image Messenger images ↑ Double-ringed crater – a Mercury feature courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/S trom02.jpg ← Courtesy: http://messenger.jhuapl.edu/gal lery/sciencePhotos/pics/EN010 8828161M.jpg Messenger image Courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/Prockter06.jpg Mercury Close-up Mercury’s topography was formed under stronger gravity than on the Moon The Caloris basin is an impact crater ~1400 km across, beneath which is thought to be a dense mass 2 Mercury’s rotation period is exactly /3 of its orbital period -
FROM WET PLANET to RED PLANET Current and Future Exploration Is Shaping Our Understanding of How the Climate of Mars Changed
FROM WET PLANET TO RED PLANET Current and future exploration is shaping our understanding of how the climate of Mars changed. Joel Davis deciphers the planet’s ancient, drying climate 14 DECEMBER 2020 | WWW.GEOLSOC.ORG.UK/GEOSCIENTIST WWW.GEOLSOC.ORG.UK/GEOSCIENTIST | DECEMBER 2020 | 15 FEATURE GEOSCIENTIST t has been an exciting year for Mars exploration. 2020 saw three spacecraft launches to the Red Planet, each by diff erent space agencies—NASA, the Chinese INational Space Administration, and the United Arab Emirates (UAE) Space Agency. NASA’s latest rover, Perseverance, is the fi rst step in a decade-long campaign for the eventual return of samples from Mars, which has the potential to truly transform our understanding of the still scientifi cally elusive Red Planet. On this side of the Atlantic, UK, European and Russian scientists are also getting ready for the launch of the European Space Agency (ESA) and Roscosmos Rosalind Franklin rover mission in 2022. The last 20 years have been a golden era for Mars exploration, with ever increasing amounts of data being returned from a variety of landed and orbital spacecraft. Such data help planetary geologists like me to unravel the complicated yet fascinating history of our celestial neighbour. As planetary geologists, we can apply our understanding of Earth to decipher the geological history of Mars, which is key to guiding future exploration. But why is planetary exploration so focused on Mars in particular? Until recently, the mantra of Mars exploration has been to follow the water, which has played an important role in shaping the surface of Mars. -
John Joly (1857–1933)
Trinity College Memorial Discourse Monday 14th May 2007 JOHN JOLY (1857–1933) Patrick N. Wyse Jackson FTCD Department of Geology, Trinity College, Dublin 2, Ireland ([email protected]) Provost, Fellows, Scholars, Colleagues, Honoured Guests, and Friends It gives me great pleasure to be here today as we honour a Trinity scientist and life-long servant, and remember him close to the 150th anniversary of his birth in a small rural rectory in what is now County Offaly. I am also using the occasion to privately (and now that I mention it, publicly) remember another Trinity graduate, whose centenary his family will celebrate next year. On Trinity Monday, 67 years ago, my father Robert Wyse Jackson delivered the Memorial Discourse on Jonathan Swift. John Joly whom we honour today was a scientist with a vivid and clear imagination, and his research led him into many varied disciplines. He was a physicist, engineer, geophysicist, and educationalist, but also researched in botany, medicine and on photography. He was also closely associated with a number of Dublin organisations most notably the Royal Dublin Society of which he was President for a time, and with Alexandra College of which he was Warden for many years. This Discourse shall follow a broadly chronological sequence from his birth to death, and will examine various strands of his work and life either in depth to some degree, or else fleetingly. A bibliography of papers on Joly’s life and work is appended to the end of this Discourse. 1 John Joly in 1903 In adulthood Joly Joly was very distinctive. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
A Preliminary Report on Expeditions Monsoon And
A Preliminary Report on Expeditions Monsoon and Lusiad 1960 - 1963 University of California, San Diego Scripps Institution of Oceanography Cruises to the Indian Ocean By The Members of the Expedition Edited by Robert L. Fisher S. I. O. Reference 64-19 ― i ― FOREWORD Field participation in the International Indian Ocean Expedition by scientists and research vessels of the University of California's Scripps Institution of Oceanography comprises three multi- program investigations: MONSOON (1960-1), LUSIAD (1962-3) and DODO (1964). All three expeditions, though first broadly outlined in 1959, lie within the cooperative international exploration of the Indian Ocean being sponsored by the Scientific Committee on Oceanic Research and UNESCO. Therefore, though original schedules have to date been met, the programs have in fact been influenced and modified by the plans, interests and findings of other agencies and laboratories, and direct participation by marine scientists, students and trainees from other areas has been welcomed. Although the final SIO IIOE cruise, DODO, is just underway, a preliminary report on some generalized results of the first two expeditions seems appropriate now, with the clear understanding that many conclusions stated here may indeed be premature. Final analyses, syntheses and results will appear in more specialized formal publications and in the proposed SCOR-sponsored atlases which eventually will summarize Indian Ocean Expedition findings. At Scripps Institution, it is customary to give names, rather than number designations, to the major expeditions. The 1960-1 investigation, 3 ½ months in the Indian Ocean, embraced the first SIO field work in the "monsoon seas". It was funded primarily by the Office of Naval Research of the Navy Department, with auxiliary support for personnel and special equipment from the Bureau of Ships and the National Science Foundation.