Microbialites at Gusev Crater, Mars
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Legalizing Marijuana: California's Pot of Gold?
University of the Pacific Scholarly Commons McGeorge School of Law Scholarly Articles McGeorge School of Law Faculty Scholarship 2009 Legalizing Marijuana: California’s Pot of Gold? Michael Vitiello Pacific cGeM orge School of Law Follow this and additional works at: https://scholarlycommons.pacific.edu/facultyarticles Part of the Criminal Law Commons Recommended Citation Michael Vitiello, Legalizing Marijuana: California’s Pot of Gold?, 2009 Wis. L. Rev. 1349. This Article is brought to you for free and open access by the McGeorge School of Law Faculty Scholarship at Scholarly Commons. It has been accepted for inclusion in McGeorge School of Law Scholarly Articles by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. ESSAY LEGALIZING MARUUANA: CALIFORNIA'S POT OF GOLD? MICHAEL VITIELLO* In early 2009, a member of the California Assembly introduced a bill that would have legalized marijuana in an effort to raise tax revenue and reduce prison costs. While the bill's proponent withdrew the bill, he vowed to renew his efforts in the next term. Other prominent California officials, including Governor Schwarzenegger, have indicated their willingness to study legalization in light of California's budget shortfall. For the first time in over thirty years, politicians are giving serious consideration to a proposal to legalize marijuana. But already, the public debate has degenerated into traditional passionate advocacy, with ardent prohibitionists raising the specter of doom, and marijuana advocates promising billions of dollars in tax revenues and reduced prison costs. Rather than rehashing the old debate about legalizing marijuana, this Essay offers a balanced view of the proposal to legalize marijuana, specifically as a measure to raise revenue and to reduce prison costs. -
Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
NASA Mars Exploration Strategy: “Follow the Water”
Gullies on Mars -- Water or Not? Allan H. Treiman NASA Mars Exploration Strategy: “Follow the Water” Life W Climate A T Geology E Resources R Evidence of Water on Mars Distant Past Crater Degradation and Valley Networks ‘River’ Channels Flat Northern Lowlands Meteorites Carbonate in ALH84001 Clay in nakhlites MER Rover Sites Discoveries Hydrous minerals: jarosite! Fe2O3 from water (blueberries etc.) Silica & sulfate & phosphate deposits Recent Past (Any liquid?) Clouds & Polar Ice Ground Ice Valley Networks and Degraded Craters 1250 km River Channels - Giant Floods! 225 km 10 km craters River Channels - ‘Normal’ Flows 14 km 1 km River Channels from Rain? 700 km Science, July 2, 2004 19 km Ancient Martian Meteorite ALH84001 MER Opportunity - Heatshield and parachute. Jarosite - A Water-bearing Mineral Formed in Groundwater 3+ KFe3 (SO4)2(OH)6 2 Jarosite = K2SO4 + 3 Fe2O3 + 3 H2SO4 Hematite is in “Blueberries,” which still suggest water. Stone Mountain MER Spirit: Columbia Hills H2O Now: Clouds & Polar Caps Ground Ice – Mars Orbiter GRS Water abundances within a few meters depth of the Martian surface. Wm. Feldman. AAAS talk & Los Alamos Nat’l. Lab. Press Release, 15 Feb. 2003. (SPACE.com report, 16 Feb. 2003) So, Water on Mars !! So? Apparently, Mars has/had lots of water. Lots of evidence for ancient liquid water (> ~2 billion years ago), both surface and underground. Martian Gullies - Liquid Water or Not? Material flows down steep slopes, most commonly interpreted as water-bearing debris flows [Malin and Edgett (2000) Science 288, 2330]. Liquid water is difficult to produce and maintain near Mars’ surface, now. -
Open Research Online Oro.Open.Ac.Uk
Open Research Online The Open University’s repository of research publications and other research outputs Centimeter to decimeter hollow concretions and voids in Gale Crater sediments, Mars Journal Item How to cite: Wiens, Roger C.; Rubin, David M.; Goetz, Walter; Fairén, Alberto G.; Schwenzer, Susanne P.; Johnson, Jeffrey R.; Milliken, Ralph; Clark, Ben; Mangold, Nicolas; Stack, Kathryn M.; Oehler, Dorothy; Rowland, Scott; Chan, Marjorie; Vaniman, David; Maurice, Sylvestre; Gasnault, Olivier; Rapin, William; Schroeder, Susanne; Clegg, Sam; Forni, Olivier; Blaney, Diana; Cousin, Agnes; Payré, Valerie; Fabre, Cecile; Nachon, Marion; Le Mouelic, Stephane; Sautter, Violaine; Johnstone, Stephen; Calef, Fred; Vasavada, Ashwin R. and Grotzinger, John P. (2017). Centimeter to decimeter hollow concretions and voids in Gale Crater sediments, Mars. Icarus, 289 pp. 144–156. For guidance on citations see FAQs. c 2017 Elsevier Inc. https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Accepted Manuscript Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1016/j.icarus.2017.02.003 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Centimeter to Decimeter Hollow Concretions and Voids In Gale Crater Sediments, Mars Roger C. Wiens1, David M. Rubin2, Walter Goetz3, Alberto G. Fairén4, Susanne P. Schwenzer5, Jeffrey R. Johnson6, Ralph Milliken7, Ben Clark8, Nicolas Mangold9, Kathryn M. Stack10, Dorothy Oehler11, Scott Rowland12, Marjorie Chan13, David Vaniman14, Sylvestre Maurice15, Olivier Gasnault15, William Rapin15, Susanne Schroeder16, Sam Clegg1, Olivier Forni15, Diana Blaney10, Agnes Cousin15, Valerie Payré17, Cecile Fabre17, Marion Nachon18, Stephane Le Mouelic9, Violaine Sautter19, Stephen Johnstone1, Fred Calef10, Ashwin R. -
Downselection of Landing Sites Proposed for the Mars 2020 Rover Mission
47th Lunar and Planetary Science Conference (2016) 2324.pdf DOWNSELECTION OF LANDING SITES PROPOSED FOR THE MARS 2020 ROVER MISSION. M. P. Golombek1, J. A. Grant2, K. A. Farley3, K. Williford1, A. Chen1, R. E. Otero1, and J. W. Ashley1, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109; 2Smithsonian Institution, Center for Earth and Planetary Sciences, Washington, D.C. 20560, 3Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125. Introduction: The Mars 2020 mission would ex- suitable for addressing key planetary evolution ques- plore a site likely to have been habitable, seek signs of tions if and when they are returned to Earth. past life, prepare a returnable cache with the most Results of the voting were presented as the compelling samples, take the first steps towards in-situ weighted average (assigning 5 points to each green resource utilization on Mars, and demonstrate technol- vote, 3 to each yellow vote, and 1 to each red vote that ogy needed for future human and robotic exploration were then summed and divided by the total number of of Mars. The first landing site workshop identified and votes) and the mode (color receiving the most votes). prioritized 27 landing sites proposed by the science This ensured that participants could not skew the re- community according to science objectives that also sults by withholding votes from some sites. Both met the engineering constraints [1]. This abstract de- methods yield similar results and reveal a fall-off in scribes the downselection of landing sites that occurred support for sites ranked lower than the top nine or ten at the second landing site workshop and associated based on mode and average, respectively [2]. -
Evaluation of Pilot Summer Activities Programme for 16 Year Olds
RESEARCH Evaluation of Pilot Summer Activities Programme for 16 Year Olds Graham Thom SQW Ltd Research Report RR341 Research Report No 341 Evaluation of Pilot Summer Activities Programme for 16 Year Olds Graham Thom SQW Ltd The views expressed in this report are the authors' and do not necessarily reflect those of the Department for Education and Skills. © Queen’s Printer 2002. Published with the permission of DfES on behalf of the Controller of Her Majesty's Stationery Office. Applications for reproduction should be made in writing to The Crown Copyright Unit, Her Majesty's Stationery Office, St Clements House, 2-16 Colegate, Norwich NR3 1BQ. ISBN 1 84185 734 3 June 2002 Table of Contents Acknowledgements Executive Summary Chapter Page 1 Introduction 1 The role of Connexions 1 Methodology 2 Report structure 3 2 Characteristics of pilot projects 4 Describing the partnerships 4 Management structure 7 Other staff involved in the partnerships 11 Engaging young people 14 Delivering the project 19 Summary 29 3 Characteristics of participants 30 Personal characteristics 30 Academic performance 32 Levels of personal social development 35 Future plans 36 Comparing the profile of participants with the 2000 37 cohort Getting involved 38 Summary 41 4 The impact of the programme 42 Overall impact on future plans 42 Overall impact on personal and social characteristics 45 Overall satisfaction with the programme 46 Impact on different groups 46 Key influencing variables 49 Impact on young people – the longer term perspective 51 Summary 56 5 Conclusions -
Peculiarities of the Chemical Abundance Distribution in Galaxies NGC 3963 and NGC 7292
MNRAS 505, 2009–2019 (2021) https://doi.org/10.1093/mnras/stab1414 Advance Access publication 2021 May 19 Peculiarities of the chemical abundance distribution in galaxies NGC 3963 and NGC 7292 A. S. Gusev ‹ and A. V. Dodin Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia Downloaded from https://academic.oup.com/mnras/article/505/2/2009/6278202 by Lomonosov Moscow State University user on 09 June 2021 Accepted 2021 May 11. in original form 2021 April 27 ABSTRACT Spectroscopic observations of 32 H II regions in the spiral galaxy NGC 3963 and the barred irregular galaxy NGC 7292 were carried out with the 2.5-m telescope of the Caucasus Mountain Observatory of the Sternberg Astronomical Institute using the Transient Double-beam Spectrograph with a dispersion of ≈1Åpixel−1 and a spectral resolution of ≈3 Å. These observations were used to estimate the oxygen and nitrogen abundances and the electron temperatures in H II regions through modern strong- line methods. In general, the galaxies have oxygen and nitrogen abundances typical of stellar systems with similar luminosities, sizes, and morphology. However, we have found some peculiarities in chemical abundance distributions in both galaxies. The distorted outer segment of the southern arm of NGC 3963 shows an excess oxygen and nitrogen abundances. Chemical elements abundances in NGC 7292 are constant and do not depend on the galactocentric distance. These peculiarities can be explained in terms of external gas accretion in the case of NGC 3963 and major merging for NGC 7292. Key words: ISM: abundances – H II regions – galaxies: abundances – galaxies: individual: NGC 3963, NGC 7292. -
Possible Clastic Origin for Olivine-Rich Rocks in the Nili Fossae Region: Implications for NE Syrtis, Midway, and Jezero Landing Site Science
Possible Clastic Origin for Olivine-Rich Rocks in the Nili Fossae Region: Implications for NE Syrtis, Midway, and Jezero Landing Site Science Christopher H. Kremer, John F. Mustard, and Michael S. Bramble Brown University Mars 2020 4th LSW October 17, 2018 Circum-Isidis Olivine-Rich Unit Mustard et al. (2009) Ehlmann and Mustard (2012) Goudge et al. (2015) Exposed at NE Syrtis, Midway, Enriched in Fo68-91 olivine Diversely altered, with exposures (~10-30%), widely distributed of carbonate with local exposures and Jezero including olivine-rich (Hamilton and Christensen, 2005) of serpentine and talc/saponite analog(?) in Columbia Hills (70,000 km2; Kremer et al., In Review) Previous Hypotheses and Observations Basement Olivine-rich unit 30 km 50 km (Rogers et al., 2018) (after Goudge et al., 2015) (Mustard et al., 2009) Moderate thermal inertia, minimal Unit superposes crater that is regolith or craters, yardangs: unit may be Intrusive origin ruled out by younger than the ~1900 km friable, potentially inconsistent with most superposition of basement diameter Isidis impact basin melt rocks unit Previous Hypotheses and Observations Basement Olivine-rich unit 50 km 30 km Kremer et al. In Review (after Goudge et al., 2015) (Mustard et al., 2009) Moderate thermal inertia, minimal Unit superposes crater that is regolith or craters, yardangs: unit may be Intrusive origin ruled out by younger than the ~1900 km friable, potentially inconsistent with most superposition of basement diameter Isidis impact basin melt rocks unit Hypotheses for Origins of Olivine-Rich Unit ??? Intrusive complex? Lava? (Hamilton and Non-Isidis Impact Sand lag deposit, erg, Volcanic ash?? (Hoefen et al., 2003) Christensen, 2005; condensate or or other epiclastic Tornabene et al., 2008) ejecta? (Rogers et al. -
Mineralogy of the Martian Surface
EA42CH14-Ehlmann ARI 30 April 2014 7:21 Mineralogy of the Martian Surface Bethany L. Ehlmann1,2 and Christopher S. Edwards1 1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125; email: [email protected], [email protected] 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 Annu. Rev. Earth Planet. Sci. 2014. 42:291–315 Keywords First published online as a Review in Advance on Mars, composition, mineralogy, infrared spectroscopy, igneous processes, February 21, 2014 aqueous alteration The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: The past fifteen years of orbital infrared spectroscopy and in situ exploration 10.1146/annurev-earth-060313-055024 have led to a new understanding of the composition and history of Mars. Copyright c 2014 by Annual Reviews. Globally, Mars has a basaltic upper crust with regionally variable quanti- by California Institute of Technology on 06/09/14. For personal use only. All rights reserved ties of plagioclase, pyroxene, and olivine associated with distinctive terrains. Enrichments in olivine (>20%) are found around the largest basins and Annu. Rev. Earth Planet. Sci. 2014.42:291-315. Downloaded from www.annualreviews.org within late Noachian–early Hesperian lavas. Alkali volcanics are also locally present, pointing to regional differences in igneous processes. Many ma- terials from ancient Mars bear the mineralogic fingerprints of interaction with water. Clay minerals, found in exposures of Noachian crust across the globe, preserve widespread evidence for early weathering, hydrothermal, and diagenetic aqueous environments. Noachian and Hesperian sediments include paleolake deposits with clays, carbonates, sulfates, and chlorides that are more localized in extent. -
Open Research Online Oro.Open.Ac.Uk
Open Research Online The Open University’s repository of research publications and other research outputs Habitability of hydrothermal systems at Jezero and Gusev Craters as constrained by hydrothermal alteration of a terrestrial mafic dike Journal Item How to cite: Costello, Lacey J.; Filiberto, Justin; Crandall, Jake R.; Potter-McIntyre, Sally L.; Schwenzer, Susanne P.; Miller, Michael A.; Hummer, Daniel R.; Olsson-Francis, Karen and Perl, Scott (2020). Habitability of hydrothermal systems at Jezero and Gusev Craters as constrained by hydrothermal alteration of a terrestrial mafic dike. Geochemistry (Early access). For guidance on citations see FAQs. c 2020 The Authors https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1016/j.chemer.2020.125613 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Geochemistry xxx (xxxx) xxxx Contents lists available at ScienceDirect Geochemistry journal homepage: www.elsevier.com/locate/chemer Habitability of hydrothermal systems at Jezero and Gusev Craters as constrained by hydrothermal alteration of a terrestrial mafic dike Lacey J. Costelloa,1, Justin Filibertob,*, Jake R. Crandallc, Sally L. Potter-McIntyrea, Susanne P. Schwenzerd, Michael A. Millere, Daniel R. Hummera, Karen Olsson-Francisd, Scott Perlf a -
Spring 2019 Newsletter
Friends of the Columbia Gorge Protecting the Gorge Since 1980 Spring 2019 Newsletter Spring Brings Hope for the Gorge Friends of the Columbia Gorge Oil train fire and oil spill in Mosier, Board of Directors Oregon, 2016. Geoff Carr Chair Photo: Paloma Ayala Debbie Asakawa Vice Chair Kari Skedsvold Secretary/Treasurer Pat Campbell Greg Delwiche John Nelson* Gwen Farnham Carrie Nobles Donald Friedman Buck Parker* John Harrison Lisa Berkson Platt David Michalek* Mia Prickett Patty Mizutani Vince Ready* Annie Munch Meredith Savery Land Trust Board of Trustees John Nelson* President David Michalek* Secretary/Treasurer John Baugher Land Trust Advisor Pat Campbell Greg Delwiche Take Action Dustin Klinger Barbara Nelson Buck Parker* Rick Ray* Protect Oregon from Dangerous Oil Trains Staff riends of the Columbia Gorge and proposed bills. Especially in light of Sophia Aepfelbacher Membership Coordinator Frances Ambrose* Land Trust Assistant our allies are supporting legislation the Trump administration’s repeal of a Nathan Baker Senior Staff Attorney in Oregon that would improve 2015 Department of Transportation rule Mika Barrett Stewardship Volunteer Coord. Fprotections against crude oil derailments and requiring oil trains to use newer, safer, Dan Bell* Land Trust Director Elizabeth Brooke-Willbanks Development Manager oil spills. House Bill 2858 and Senate Bill 99 breaking technology, Oregon needs to Peter Cornelison* Field Representative would require: ensure it is doing all it can to reduce the Pam Davee Director of Philanthropy threat from -
Evolution of Mars As a Planet, Possible Life on Mars
EVOLUTION OF MARS LECTURE 18 NEEP 533 HARRISON H. SCHMITT NASA HST IMAGE N THARSIS HELLAS S ANDESITE OR WEATHERED SOIL DUST DUST DUST BASALT ~100 KM A C B THEMIS THERMAL IMAGING OF SPIRIT LANDING AREA IN GUSEV CRATER A. SPIRIT LANDING ELLIPSE B. CLOSER VIEW OF SPIRIT LANDING ELLIPSE C. NIGHT IR IMAGE: BRIGHT AREAS ARE MORE ROCKY. ARROW POINTS TO ROCKY SLOPE SPIRIT MOVED TO GUSEV CRATER POSSIBLE LAKE BED IN LARGE BASIN A C B THEMIS THERMAL IMAGING OF OPPORTUNITYLANDING AREA IN MERIDIANI PLANUM A. LANDING ELLIPSE ~120 KM LONG) B. CLOSER VIEW OF LANDING ELLIPSE C. NIGHT IR IMAGE: BRIGHT AREAS ARE MORE ROCKY. ARROW POINTS TO ROCKY SLOPE MAJOR STAGES OF MARS’ EVOLUTION 1 BEGINNING 2 MAGMA OCEAN / CONVECTIVE OVERTURN 3A ? ? CRATERED UPLANDS / VERY LARGE BASINS 3B ? CORE FORMATION/GLOBAL MAGNETIC FIELD 3C 4.5 - 1.3 GLOBAL MAFIC VOLCANISM DENSE WATER / CO2 ATMOSPHERE E ? G 3D EROSION / LAKES / NORTHERN OCEAN A T ? ? S 4 LARGE BASINS CATACLYSM ? THARSIS UPLIFT AND VOLCANISM ? 5 NORTHERN HEMISPHERE BASALTIC / ANDESITIC VOLCANISM ? 1.3 - 0.2 SUBSURFACE HYDROSPHERE / CRYOSPHERE 6 ? PRESENT SURFACE CONDITIONS LUNAR 4.6 4.2? 3.8 ? 5.0 4.0 3.0 2.0 1.0 BILLIONS OF YEARS BEFORE PRESENT ITALICS = SNC DATES RED = MAJOR UNCERTAINTY OLYMPUS TOPOGRAPHY OF MONS THARSIS REGION VALLES MARINERIS THARSIS REGION SHADED RELIEF DETAIL MARS GLOBAL SURVEYOR MOLA OLYMPUS MONS VALLES MARINERIS APOLLO MODEL OF MARS EVOLUTION ELYSIUM MONS ANDESITIC THARSIS EVENTS EXTRUSIONS <3.8 B.Y. THARSIS THICKENING ATMOSPHERE: MAFIC UPPER MANTLE WITH CO2, H20 CRYOSPHERE / INCREASING HYDROSPHERE SI AND FE UPWARDS OLIVINE/ NA- PYROXENE ? ANDESITIC CUMULATE INTRUSIONS? OLIVINE ? CUMULATE RELIC PROTO- GARNET / NA-CPX/ CORE ? NA-BIOTITE?/NA- HORNBLENDE/ ? FExNIySz “RUTILE” (TRANSITION? CORE CUMULATES ? ZONE) RELIC MAGNETIC STRIPING THICKENED SOUTHERN ©Harrison H.