DOCSLIB.ORG

Durangoko Azoka & Durango Da Azoka

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Durangoko Azoka & Durango Da Azoka egitaraua Durangoko azoka & Durango da azoka Durango uriaren hegaletik Mañarierreka bideratzen da Kantauri itsasoaren bila. Erreka-bazterrean, urtero, 1965az geroztik, gizaki-tantekin osatutako Durangoko azoka izeneko ur-putzua sortzen izan da. Baina… nahiz eta urtero ur berria izan putzuak, lau hamarkada luze igaro ondoren tanta, beste tanta batzuekin bilduz, putzu izateari utzi eta erreka izatearen beharra ikusi zuten. Putzua Kulturerreka bihurtzea. Errekaondoko bidezidorrean zehar, abenduko euri zaparradako tangadak bilduz, euskal kulturaren uholdea sortu eta bideratu. Landakotik Larizdorre kalera kokatzen diren azoka, saguganbara, ahotsenea, irudienea, szenatokia eta beste izen batzuetako ur-putzuak lotuz Errekaondoko kultur bidezidorra burutu. Tabirako Uriberri guztira AZOKA zabalduz. Durangoko azoka & Durango da azoka. Aurkibidea 04 Durangoko mapa 06 Landako erakustazoka 08 Artisau Azoka 09 Abenduaren 5ean 13 Abenduaren 6an 17 Abenduaren 7an 21 Abenduaren 8an Erretentxu K. Kurutziaga Kalea Matxinestarta Kalea Ibaizabal Auzunea Pablo Pedro Astarloa Kalea Murueta Torre A. Murueta Torre Komentukalea Kalea Andra Mari Kalea 1 2 3 Antso Estegiz Zumardia Aldapa Azoka Kabi@ Areto Nagusia Arandoño Torre K. Kalebarria K. Azoka K. Goienkalea Kalea Monago K. P Parkinga Hiribidea Montevideo Artisau Azoka Kanpatorrosteta K. Artekalea Kalea Uribarri Kalea Barrenkalea K. Oiz Kalea 4 5 6 7 Lariz Torre K. Saguganbara Plateruena Ahotsenea Irudienea Zeharkalea K. Andra Mari K. Oiz Kalea Oiz Zumalakarregi K. Zumalakarregi K. 8 Szenatokia Arkotxa K. Arkotxa Turismo Ermodo Kalea Bulegoa Bus Geltokia Ezkurdi Plaza Arte eta Historia Museoa Juan Antonio Abasolo K Geltoki Zaharra Argazki Erakusketa “Noctis Labyrinthus” Josemiel Barandiaran K, Tronperri Kalea Galtzareta K. Tren Landako Hiribidea Geltokia Bruno Mauricio Zabala K. Fray Juan de Zumarraga K. 4 2013ko abenduaren 5etik 8ra Erretentxu K. Kurutziaga Kalea BILBO DONOSTIA Matxinestarta Kalea Ibaizabal Auzunea IURRETA Pablo Pedro Astarloa Kalea Murueta Torre A. Murueta Torre Komentukalea Kalea Andra Mari Kalea Antso Estegiz Zumardia Aldapa 1 2 3 DURANGO Azoka Kabi@ Areto Nagusia Arandoño Torre K. Kalebarria K. ARRASATE GASTEIZ Azoka K. Goienkalea Kalea Monago K. P Parkinga Hiribidea Montevideo Artisau Azoka Kanpatorrosteta K. Artekalea Kalea Uribarri Kalea Barrenkalea K. Oiz Kalea 4 5 6 7 Lariz Torre K. Saguganbara Plateruena Ahotsenea Irudienea Zeharkalea K. Andra Mari K. Oiz Kalea Oiz Zumalakarregi K. Zumalakarregi K. 8 Szenatokia Arkotxa K. Arkotxa Turismo Ermodo Kalea Bulegoa Bus Geltokia Ezkurdi Plaza Arte eta Historia Museoa Juan Antonio Abasolo K Geltoki Zaharra Argazki Erakusketa “Noctis Labyrinthus” Josemiel Barandiaran K, Tronperri Kalea Galtzareta K. Tren Landako Hiribidea Geltokia Bruno Mauricio Zabala K. Fray Juan de Zumarraga K. www.durangokoazoka.com 5 48.DURANGOKO AZOKA kulturaren plaza 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 025 026 027 028 029 030 031 032 033 034 035 036 037 038 039 040 041 042 043 044 045 046 047 048 049 050 051 052 053 054 055 056 057 Goienkale Goienkale Goienkale 102 101 100 099 098 097 096 095 094 093 092 091 090 089 088 087 086 085 084 082 081 080 079 078 077 076 075 074 073 072 071 070 069 068 067 066 065 064 063 062 061 060 059 058 Turismo Gerediaga Bulegoa Elkartea Prentsa 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 025 026 027 028 029 030 031 032 033 034 035 036 037 038 039 040 041 042 043 Bulegoa EITB Artekale Informazioa Artekale Artekale 079 078 077 076 075 074 073 072 071 070 069 068 067 066 065 064 063 062 061 060 059 058 057 056 055 054 053 052 051 050 049 048 047 046 045 044 066 BIS 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 Azoka Barrenkale 3 Barrenkale Atseden Gunea Zuzendaritza Bulego Irrati 2 Areto Nagusia Teknikoa Estudioa Kabi@ 055 054 053 052 051 050 049 048 047 046 045 044 043 042 041 040 039 038 037 036 035 034 033 032 031 030 029 028 027 026 025 Literatura Erakundeak eta elkarteak Musika 1512-2022 NAFARROA BIZIRIK // BIZKAIKO MUSEOAK-BFA // EROSKI // Artekale 29-30 Barrenkale 40 Goienkale 81-82 ERRABAL JAZZ // Artekale 54 ADARMENDI EKE // Barrenkale 17 BONBERENEA EKINTZAK // EUSKAL DANTZARIEN BILTZARRA AFEDE // Goienkale 88-92 Artekale 43 // Goienkale 35 AGORILA // Goienkale 25 BRIXTON RECORDS // Goienkale 56 EUSKAL HERRIA ALDIZKARIA // AHOTSAK.COM // Goienkale 79 COAVN-EHAEO // Goienkale 80 Barrenkale 29 AIZKORRI // Goienkale 87 DAMBA KAMELUAK // Goienkale 57 EUSKAL HERRIKO UNIBERTSITATEA AIZU!-AEK // Goienkale 33 DENONARTEAN // Artekale 16 // Goienkale 69-71 ALTAFFAYLLA-ARABERA // DESCLÉE // Goienkale 94-95 EUSKAL MEMORIA // Barrenkale 11-12 Barrenkale 10 DEUSTUKO UNIBERTSITATEA // EUSKAL PAPERGINTZA // Goienkale 41 ARABAKO FORU ALDUNDIA // Goienkale 73 EUSKALTZAINDIA // Artekale 35 Artekale 60 DURANGALDEKO ARGITALPENAK EUSKO JAURLARITZA // Artekale 61-64 ARGIA // Goienkale 8 // Artekale 21 EUSKO LEGEBILTZARRA // Artekale 33 ARTEZ // Goienkale 40 DURANGOKO UDALA // Artekale 22 GAKOA // Artekale 15 ASKAPENA // Barrenkale 36 EFARANTZAZU // Artekale 36 GARA // Barrenkale 18-19 ASTERO // Barrenkale 20 EGUZKI BIDEOAK // Goienkale 44 GATUZAIN // Goienkale 27 ATARAMIÑE // Barrenkale 37-38 EHAZE // Goienkale 66 GAUMIN ARGITALETXEA // AZKUE FUNDAZIOA // Artekale 24-26 EL MUNDO DE LOS PIRINEOS // Goienkale 19 BADIHARDUGU // Goienkale 78 Barrenkale 28 GAZTE SORKUNTZA // Goienkale 42 BAGA BIGA MUSIKA IDEIAK // ELHUYAR // Artekale 28 GAZTELUPEKO HOTSAK // Goienkale 50-53 ELHUYAR HIZTEGIAK // Artekale 27 Artekale 52-53 BANIZU NIZUKE // Goienkale 65 ELKAR // Artekale 68-79 GAZTEZULO.COM // Goienkale 46 BBK // Artekale 31-32 ELKAR // Goienkale 60-64 GEREDIAGA ELKARTEA // Artekale 20 BERRIA // Barrenkale 21-22 ELKAR AZOKAK // Artekale 13-14 GIPUZKOAKO FORU ALDUNDIA // BERTSOLARI ALDIZKARIA // ELKAR BANAKETA // Artekale 7-9 Artekale 55-56 Artekale 67 ELKAR BANAKETA // Barrenkale 30-32 GITE-IPES AHAZTUAK // Barrenkale 34 BIDEHUTS // Artekale 48 ELKAR BANAKETA // Goienkale 47 GOR DISKOAK // Artekale 44-46 BITARTE // Artekale 17 ELKAR-ARGIAK // Goienkale 59 GURE LIBURUAK // Barrenkale 9 BIZKAIKO FORU ALDUNDIA // ENA // Artekale 19 HABE // Artekale 65-66 Artekale 57-59 EREIN // Goienkale 96-102 HALA DZIPO // Artekale 47 6 2013ko abenduaren 5etik 8ra Azoka ordutegia: 10:30-20:00 // Sarrera doan 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 025 026 027 028 029 030 031 032 033 034 035 036 037 038 039 040 041 042 043 044 045 046 047 048 049 050 051 052 053 054 055 056 057 Goienkale Goienkale Goienkale 102 101 100 099 098 097 096 095 094 093 092 091 090 089 088 087 086 085 084 082 081 080 079 078 077 076 075 074 073 072 071 070 069 068 067 066 065 064 063 062 061 060 059 058 Turismo Gerediaga Bulegoa Elkartea Prentsa 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 025 026 027 028 029 030 031 032 033 034 035 036 037 038 039 040 041 042 043 Bulegoa EITB Artekale Informazioa Artekale Artekale 079 078 077 076 075 074 073 072 071 070 069 068 067 066 065 064 063 062 061 060 059 058 057 056 055 054 053 052 051 050 049 048 047 046 045 044 066 BIS 001 002 003 004 005 006 007 008 009 010 011 012 013 014 015 016 017 018 019 020 021 022 023 024 Azoka Barrenkale 3 Barrenkale Atseden Gunea Zuzendaritza Bulego Irrati 2 Areto Nagusia Teknikoa Estudioa Kabi@ 055 054 053 052 051 050 049 048 047 046 045 044 043 042 041 040 039 038 037 036 035 034 033 032 031 030 029 028 027 026 025 Literatura Erakundeak eta elkarteak Musika HAMAIKA TELEBISTA // Artekale 66 MEZULARI // Goienkale 84-86 THE BALDE - ENTZUN! // BIS MKA/Adorez Hiztegiak XXI // Goienkale 45 HIK HASI - HAZI HEZI // Goienkale 9 Artekale 34 TMEO // Goienkale 43 IBAIZABAL // Goienkale 11-18 MONDRAGON UNIBERTSITATEA // TRAVEL BUG // Barrenkale 13-16 IBAIZABAL KULTUR ELKARTEA // Goienkale 68 TRIKITIXA-TXISTULARI ELK. // Goienkale 32 MUSIKA EKOIZLEAK (MEE) / Goienkale 34 IGELA // Barrenkale 44 SYNTORAMA // Artekale 40 TTARTTALO // Goienkale 1-7 IKAS // Goienkale 29 MUSIKARI // Goienkale 55 TURISMO DURANGO // Artekale 00 IKASELKAR // Artekale 1-6 MUSIKAZUZENEAN // Artekale 42 TXALAP.ART - ESNE BELTZA // INDEPENDENTISTAK // Barrenkale 35 NABARRALDE // Barrenkale 41-42 Artekale 50 INTXORTA 1937 KULTUR OIHUKA // Goienkale 48 TXALAPARTA // Barrenkale 1 ELKARTEA // Barrenkale 33 ONGD AFRIC’ FORUM // TXALAPARTA // Barrenkale 2-8 IRRIEN LAGUNAK // Goienkale 21 Goienkale 20 TXERTOA // Artekale 10-12 JAKIN // Goienkale 75 ORTZADAR-NOTICIAS TALDEA // UDAKO EUSKAL UNIBERTSITATEA JK. IRIZAR // Artekale 37 Barrenkale 23-24 - UEU // Goienkale 72 KATXIPORRETA // Goienkale 22 PAMIELA // Barrenkale 48-54 UDALBILTZA // Artekale 23 KLASIKART // Artekale 38-39 PAMIELA-KALANDRAKA // UNIVERSITY OF NEVADA PRESS // KONTSEILU EBANJELIKOA // Barrenkale 55 Goienkale 74 Goienkale 39 PIRRITX, PORROTX ETA MARI URTXINTXA ESKOLA-BIZKAIA // LA GALLINA VASCA // Barrenkale 39 MOTOTS // Goienkale 23 Goienkale 93 LABAYRU IKASTEGIA // SEASKA // Goienkale 30 WWW.KATXIPORRETA.COM // Goienkale 76-77 SILBOBERRI TXISTU ELKARTEA // Goienkale 24 LANKU - EHBE // Goienkale 67 Goienkale 36 ZE ESATEK! & LAGUNAK // LEMURIA // Artekale 18 SORTZEN ELKARTEA // Goienkale 54 MAIATZ // Goienkale 28 Goienkale 10 ZEA MAYS // Artekale 41 MAUKA MUSIKAGINTZA // SU TA GAR // Goienkale 58 ZENBAT GARA KULTUR ELKARTEA Artekale 51 SUA EDIZIOAK // Barrenkale 25-27 / GABRIEL ARESTI KULTURA MEETTOK // Barrenkale 43 SUSA-LITERATURA // ELKARTEA // Goienkale 31 METAK-ESAN OZENKI // Barrenkale 45-47 ZTK // Goienkale 26 Goienkale 49 TALKA - GOSE // Artekale 49 ZUTOIA // Goienkale 37-38 www.durangokoazoka.com 7 Artisau Azoka eta Plateruena Abenduak 5, osteguna 5 Goizean / Arratsaldean: 5 Haurrentzako tailerrak, Zura ezagutzeko ikastaro laburra. Gozoki tailerra eta Papiroflexia tailerra. www.plateruenasarrerak.eu Abenduak 6, ostirala 6 Txarteldegian 16.30-19.30 Goizean / Arratsaldean Suarekin lotutako lanbideen erakustaldia. Azaroak 29, ostirala • Burdinola artistikoa. Burdinolaren interpretazio 29 zentroa, Forjas Brun. 22:30 Ruper Ordorika.
Load more

Recommended publications
  • Plains Volcanism on Mars Revisited: the Topography and Morphology of Low Shields and Related Landforms
    Seventh International Conference on Mars 3287.pdf PLAINS VOLCANISM ON MARS REVISITED: THE TOPOGRAPHY AND MORPHOLOGY OF LOW SHIELDS AND RELATED LANDFORMS. E. Hauber1, 1Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, 12489 Berlin, Germany ([email protected]). Introduction: The morphometry of Martian vol- cent study [1] used MOLA topography to measure the canoes provides critical input to the investigation of morphometric properties of several large Martian vol- their tectonic setting and the rheology of their eruption canoes. However, images of the Viking Orbiter mis- products. It is also an important prerequisite for studies sion showed that there are also numerous small and of comparative planetology, e.g., the comparison be- low shield volcanoes on Mars [2-7]. Almost all of tween terrestrial and planetary surface features. A re- these low shields are located within Tharsis and Ely- sium, the major volcanic provinces on Mars. A com- prehensive description of low shields in Tempe Terra based on Viking Orbiter images is given by [5], who describes shield fields with broad, very low shields, often associated with linear fissure vents, and several steeper edifices (Fig. 1). Many of the low shields have one or more summit craters. The craters are relatively small as compared to the basal diameter, and their form may be circular or elongated along the dominant tectonic trend. Plescia [ref. 5] compared low shields in the Tempe Terra region with terrestrial volcanoes and found that they are similar in many aspects to low shields in the eastern Snake River Plains in Idaho (USA; hereafter referred to as ESRP).
    [Show full text]
  • The Role of Subsurface Volatiles in the Formational History of Noctis Labyrinthus, Mars
    51st Lunar and Planetary Science Conference (2020) 1997.pdf THE ROLE OF SUBSURFACE VOLATILES IN THE FORMATIONAL HISTORY OF NOCTIS LABYRINTHUS, MARS. Corbin L. Kling ([email protected])1, Paul K. Byrne1, and Karl W. Wegmann1, 1Depart- ment of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC, 27695. Introduction: Noctis Labyrinthus on Mars boasts Landforms of Noctis Labyrinthus: The region many interesting geomorphological signatures contains abundant normal faults, pit craters (collapse indicating a complex history (Figure 1). Situated pits with circular to elliptical/elongate shapes), and between the Tharsis Rise and Valles Marineris, Noctis rampart craters (impact craters with morphologies is understudied compared with its more famous indicating volatiles were mobilized in the ejecta) neighboring regions. Noctis Labyrinthus itself contains surrounding the deep troughs (Figure 1). The troughs abundant normal faults, pit craters, and deep troughs. contain many landforms indicating mass wasting The area was first mapped in 1977 on Mariner imagery processes and hint at the presence of ice. Landslides [1], and interpreted as akin to the East African Rift dominate trough slopes, whereas periglacial landforms system with respect to the large amount of faulting and are common along troughs floors. the orientations of those faults. The formational history The occurrence of landslides and periglacial features of Noctis Labyrinthus, however, is still debated, with in the large troughs of Noctis provide useful information explanations for its deep troughs ranging from lava tube regarding the final stages of formation, and potentially collapse [2] to groundwater release through faulting give clues to what process(es) contributed to the initial pathways and psuedokarst [3, 4].
    [Show full text]
  • NOCTIS LANDING: a Proposed Landing Site/Exploration Zone For
    NOCTIS LANDING: A Proposed Landing Site/Exploration Zone for Human Missions to the Surface of Mars Pascal Lee1,2,3, Shannen Acedillo1,2, Stephen Braham1, Adrian Brown2, Richard Elphic3, Terry Fong3, Brian Glass3, Christopher Hoftun1, Brage W. Johansen1, Kira Lorber1, David Mittlefehldt4, Yuta Tagaki1,2, Peter Thomas5, Mi- chael West1, Stephen West1, Michael Zolensky4. 1Mars Institute, NASA Research Park, Moffett Field, CA 94035, USA, [email protected]. 2SETI Institute, 3NASA Ames Research Center, 4NASAJohnson Space Center, 5Cornell University. Exploration Zone Name: Noctis Landing Landing Site Coordinates: 6o 29’ 38.33” S, 92o 27’ 12.34” W. The proposed Noctis Landing Landing Site/Exploration Zone (LS/EZ) is shown in Figure 1. Our preliminary study suggests that the proposed site meets all key Science and Resources (incl. Civil Engineering) requirements. The site is of significant interest, as the EZ not only offers a large number and wide range of regions of interest (ROIs) for short-term exploration, it is also located strategically at the crossroads between Tharsis and Valles Marineris, which are key for long-term exploration. Figure 1: Map of the Noctis Landing LS/EZ. The solid red circle marks the distance of 100 km radial range from the Landing Site (LS), defining the primary Exploration Zone (EZ). The dotted red circle marks 200 km radial range from the LS. Areas circled (or ellipsed) in blue are high value science targets located within the primary EZ. Areas outlined in yellow are high-value science targets located outside the EZ, but within 200 km radial range from the LS. White dotted lines represent potential paths for pressurized rover traverses.
    [Show full text]
  • Gypsum, Opal, and Fluvial Channels Within a Trough of Noctis
    Planetary and Space Science 87 (2013) 130–145 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Gypsum, opal, and fluvial channels within a trough of Noctis Labyrinthus, Mars: Implications for aqueous activity during the Late Hesperian to Amazonian Catherine M. Weitz a,n, Janice L. Bishop b, John A. Grant c a Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States b SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, United States c Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, 6th at Independence Ave. SW, Washington, DC 20560, United States article info abstract Article history: We investigate in detail the morphology, mineralogy, and stratigraphy of light-toned deposits within one Received 27 March 2013 trough of Noctis Labyrinthus, centered at À6.81N, 261.11E. CRISM spectra taken from light-toned layered Received in revised form deposits in the northern portion of the trough exhibit absorptions around 1.41, 1.92 and 2.21 μm, 3 July 2013 consistent with mixtures of opal and Al-clays that are exposed beneath younger lava flows and between Accepted 8 August 2013 high-standing mesas of chaotic terrain. In the southern portion of the trough, opal occurs as a patchy Available online 22 August 2013 surficial deposit along the southwestern lower wall. Gypsum appears to be present in the southern Keywords: portion of the trough where spectra show triplet absorptions at 1.44, 1.48, and 1.54 μm, and additional Mars absorptions at 1.20, 1.74, 1.95, 2.22, 2.27, and 2.49 μm.
    [Show full text]
  • Programme Book
    EPSC2018 European Planetary Science Congress 2018 16–21 September 2018 TU Berlin | Berlin | Germany Programme Book © TU Berlin/Dahl access to access to cafeteria area first floor area Information & registration Jupiter room Ground floor area H0104 Ground floor area EPSCEuropean Planetary Science Congress Mars Venus Saturn Uranus Neptune room room room room room H0112 H0111 H0110 H0107 H0106 access to ground floor area Cafeteria area Cafeteria area EPSCEuropean Planetary Science Congress Mercury Press conference Press room room room H2035 H2036 H2037 Second floor area Second floor area EPSCEuropean Planetary Science Congress EEuropeaPn PlanetarSy Science CCongress Table of contents 1 Welcome …………………………………2 General information …………………………………4 Exhibitors, Community events …………………………………6 Splinter meetings & workshops .………………………….….…7 Session overview ……………………………..….8 Monday – Oral programme ..……………………………….9 Tuesday – Oral programme ……………………………….19 Tuesday – Poster programme .………………………………30 Wednesday – Oral programme .……….…………………..…42 Wednesday – Poster programme .………………………………51 Thursday – Oral programme ……………………………….60 Thursday – Poster programme ……………………………….71 Friday – Oral programme ……………………………….81 Author index ……………………………….91 European Planetary Science Congress 2018 2 Welcome Message from the Organizers amateur astronomers, policy makers, the next generation of scientists and engineers, and On behalf of the Executive Committee, the planetary scientists around the world. Scientific Organizing Committee and the Local Organizing Committee, welcome
    [Show full text]
  • A Proposed Future Mars Landing Site in Noctis Labyrinthus
    42nd Lunar and Planetary Science Conference (2011) 1874.pdf A PROPOSED FUTURE MARS LANDING SITE IN NOCTIS LABYRINTHUS. C. M. Weitz1 and J. L. Bishop2, 1Planetary Science Institute, 1700 E Fort Lowell, Suite 106, Tucson, AZ 85719, [email protected]; 2The SETI Institute&NASA-Ames Research Center, Mountain View, CA 94043. Introduction: We have studied the geologic set- ting and identified candidate rover traverses and scien- Table 1: Noctis Labyrinthus Landing Site tific targets within a proposed landing ellipse in one of Site Name Noctis Labyrinthus the troughs of Noctis Labyrinthus (Figure 1). A stereo Center Coordinates 261.03E, -6.86N pair of HiRISE images covering a portion of the trough Latitude, longitude was used to produce a Digital Terrain Model (DTM). Elevation 2.22 km wrt MOLA CRISM spectral parameter maps were then co- Ellipse Size 15 km by 10 km registered and overlain on the DTM to aide in the in- Prime Science Tar- Smectites, Gypsum, Opal terpretation of stratigraphic relationships. The prime gets [Highest Priority], science targets are not within the 15x10 km landing Other light-toned units of ellipse but rather a few kms southwest of the ellipse uncertain composition, and include possible Al-smectites, Ca-sulfates (gyp- valleys, mesas, and Ama- sum or bassanite), and hydrated silica (opal) [1,2]. A zonian volcanics [Lower landing site within this trough could potentially ad- Priority] dress questions concerning the ages, setting, and for- Distance of Science Smectites – 8 km to SW mation of clays and sulfates, including the potential Targets from Ellipse Gypsum, Opal – 12 km to habitability of this region in the martian past.
    [Show full text]
  • Hirise Observations of Valles Marineris Layering Ross A
    Seventh International Conference on Mars 3310.pdf HiRISE Observations of Valles Marineris layering Ross A. Beyer1,2, Catherine M. Weitz3, Bradley J. Thompson4, Jeffrey M. Moore2, Alfred S. McEwen5, and the HiRISE Team; 1Carl Sagan Center at the SETI Institute ([email protected]), 2NASA Ames Research Center, 3Planetary Science Institute, 4NASA Jet Propulsion Laboratory, and 5The University of Arizona. The High Resolution Imaging Science Experiment (HiRISE) camera on the Mars Reconnaissance Orbiter (MRO) is providing spectacular images of Mars resolv- ing features at the sub-meter scale [1]. Color imag- ing and overlapping stereo images are also valuable for viewing topography and stratigraphy. We have used the HiRISE data to examine the layering observed in the chasma slopes, the interior mesas, the chasma floors, and layers observed on the surrounding plains. The high- resolution images show extensive layering with variable lithologies, and stunning new views of familiar land- scapes. Chasma Wall Layers HiRISE resolution of layers in the chasmata walls pro- vide better detail on the sub-meter texture of their out- crops. A talus cover dominates the low angle slopes and so layering is best observed on the spurs of the spur-and- gully morphology of the slopes and near the chasmata rims. The layers identifiable in lower-resolution data as dark-toned units resolve into rubbly outcrops of meter- scale boulders (Figure 1). A previous study [2] reasoned that since these layers were dark-toned even on sunlit- Figure 1: The north rim of Coprates Chasma showing facing slopes, that they must be inherently dark-toned more resistant layers cropping out and displaying a rub- material.
    [Show full text]
  • Evolution of Major Sedimentary Mounds on Mars: Build-Up Via Anticompensational Stacking Modulated by Climate Change
    Evolution of major sedimentary mounds on Mars: build-up via anticompensational stacking modulated by climate change Edwin S. Kite1,*, Jonathan Sneed1, David P. Mayer1, Kevin W. Lewis2, Timothy I. Michaels3, Alicia Hore4, Scot C.R. Rafkin5. 1. University of Chicago. 2. Johns Hopkins University. 3. SETI Institute. 4. Brock University. 5. Southwest Research Institute. (*[email protected]) Abstract. We present a new database of >300 layer-orientations from sedimentary mounds on Mars. These layer orientations, together with draped landslides, and draping of rocks over differentially- eroded paleo-domes, indicate that for the stratigraphically-uppermost ~1 km, the mounds formed by the accretion of draping strata in a mound-shape. The layer-orientation data further suggest that layers lower down in the stratigraphy also formed by the accretion of draping strata in a mound-shape. The data are consistent with terrain-influenced wind erosion, but inconsistent with tilting by flexure, differential compaction over basement, or viscoelastic rebound. We use a simple landscape evolution model to show how the erosion and deposition of mound strata can be modulated by shifts in obliquity. The model is driven by multi-Gyr calculations of Mars’ chaotic obliquity and a parameterization of terrain-influenced wind erosion that is derived from mesoscale modeling. Our results suggest that mound-spanning unconformities with kilometers of relief emerge as the result of chaotic obliquity shifts. Our results support the interpretation that Mars’ rocks record intermittent liquid-water runoff during a 108-yr interval of sedimentary rock emplacement. 1. Introduction. Understanding how sediment accumulated is central to interpreting the Earth’s geologic records (Allen & Allen 2013, Miall 2010).
    [Show full text]
  • Image: Jarosite in the Noctis Labyrinthus Region of Mars 22 February 2016, by Cathy Weitz
    Image: Jarosite in the Noctis Labyrinthus Region of Mars 22 February 2016, by Cathy Weitz indicate acidic aqueous conditions within a volcanic system in Noctis Labyrinthus. Above the light-toned jarosite deposit is a mantle of finely layered darker- toned material. CRISM spectra do not indicate this upper darker-toned mantle is hydrated. The deposit appears to drape over the pre-existing topography, suggesting it represents an airfall deposit from either atmospheric dust or volcanic ash. Provided by NASA Credit: NASA/JPL-Caltech/Univ. of Arizona This image, acquired on Nov. 24, 2015 by the High Resolution Imaging Science Experiment (HiRISE) camera aboard NASA's Mars Reconnaissance Orbiter, shows the western side of an elongated pit depression in the eastern Noctis Labyrinthus region of Mars. Along the pit's upper wall is a light- toned layered deposit. Noctis Labyrinthus is a huge region of tectonically controlled valleys located at the western end of the Valles Marineris canyon system. Spectra extracted from the light-toned deposit by the spacecraft's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument are consistent with the mineral jarosite, which is a potassium and iron hydrous sulfate. On Earth, jarosite can form in ore deposits or from alteration near volcanic vents, and indicates an oxidizing and acidic environment. The Opportunity rover discovered jarosite at the Meridiani Planum landing site, and jarosite has been found at several other locations on Mars, indicating that it is a common mineral on the Red Planet. The jarosite-bearing deposit observed here could 1 / 2 APA citation: Image: Jarosite in the Noctis Labyrinthus Region of Mars (2016, February 22) retrieved 29 September 2021 from https://phys.org/news/2016-02-image-jarosite-noctis-labyrinthus-region.html This document is subject to copyright.
    [Show full text]
  • Regional Hydrothermal Alteration in Noctis Labyrinthus: Scattered, Yet Pervasive
    EPSC Abstracts Vol. 10, EPSC2015-472, 2015 European Planetary Science Congress 2015 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2015 Regional hydrothermal alteration in Noctis Labyrinthus: scattered, yet pervasive. P. Thollot (1,2), N. Mangold (1) and S. Le Mouélic (1) (1) Laboratoire de Planétologie et Géodynamique de Nantes (LPGN), CNRS/Université Nantes, 44322 Nantes Cedex, France, (2) Laboratoire de Géologie de Lyon (LGL-TPE), CNRS/Université Lyon 1, 69622 Villeurbanne Cedex, France. ([email protected]) Abstract to-noise. Custom spectral criteria, based on the shape and combination of absorption bands, were then We analyzed 113 CRISM cubes in Noctis computed to look for various alteration minerals. Labyrinthus. We found 10 classes of alteration minerals including clays and sulfates, sometimes associated in the same setting. Fe and Al sulfates argue for acidic hydrothermal alteration. 1. Introduction The Valles Marineris (VM) region of Mars bears various alteration minerals, as initially revealed by km-scale data from OMEGA (Observatoire pour la Minéralogie, l’Eau, les Glaces et l’Activité) [1,2], and which diversity has been assessed by numerous local studies using finer resolution (tens of m) data from CRISM (Compact Reconnaissance Imaging Spectrometer for Mars). These minerals include Fe- oxides and sulfates in the chasmata and hydrated silica or phyllosilicates on the surrounding plateaus [3]. Figure 1: Extent of the area of study with CRISM footprints in yellow. Noctis Labyrinthus (NL) is an ensemble of depressions located at the western extremity of We found widespread occurrences of outcrops of ~10 Valles Marineris, where an unexpected diversity of classes of different hydrated minerals.
    [Show full text]
  • Noctis Landing, Mars: Concept Vehicular Traverse Paths from a Proposed Human Landing Site and Exploration Zone in West Valles Marineris
    50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 3272.pdf NOCTIS LANDING, MARS: CONCEPT VEHICULAR TRAVERSE PATHS FROM A PROPOSED HUMAN LANDING SITE AND EXPLORATION ZONE IN WEST VALLES MARINERIS. Brianne Visaya1,2,3 Brian Day2, and Pascal Lee1,2,4,1SETI Institute, e-mail: [email protected], 2NASA Ames Re- search Center, 3Los Medanos College, 4Mars Institute. Summary: Noctis Landing, a proposed landing volcanic – and by likely implication hydrothermal - site and exploration zone for human missions to the activity on Mars, and thus to key opportunities to surface of Mars, would allow access, via short and search for signs of extant life on Mars. long-range vehicular traverses, to an exceptionally Pressurized Rover Traverses. Vehicular traverses wide range possible of Science Regions of Interest. to SROIs will be a central activity in the exploration of Introduction: Noctis Landing is one of 47 sites Mars from any Landing Site. Dual or multiple pressur- proposed to NASA during the agency’s First Landing ized rovers working in tandem are essential to this ac- Site (LS) / Exploration Zone (EZ) Workshop for Hu- tivity, for both short-range traverses located well man Missions to the Surface of Mars held in Houston, within the primary 100 km-radius EZ and long-range TX, in October 2015 [1, 2, 3]. The Noctis Landing site traverses extending well beyond. The actual configura- o o is located at 6 29’ 38.3” S, 92 27’ 12.3” W, in a vast tion of an accessible EZ around a LS is in practice ~200 km-wide regional depression between the west- more complex than a circular access perimeter, de- ern end of Valles Marineris and the eastern end of pending in particular on terrain and topography [6].
    [Show full text]
  • 1 Controls on the Global Distribution of Martian Landsliding
    ESSOAr | https://doi.org/10.1002/essoar.10504190.1 | CC_BY_NC_4.0 | First posted online: Thu, 10 Sep 2020 06:23:21 | This content has not been peer reviewed. 1 Controls on the Global Distribution of Martian Landsliding 2 Kevin P. Roback1, Bethany L. Ehlmann1,2 3 1 – Division of Geological and Planetary Sciences, California Institute of Technology, 4 Pasadena, CA, USA 5 2 – Jet Propulsion Laboratory, California Institute of Technology, Pasadena, 6 California 91125, USA 7 8 9 Abstract 10 Recent acquisition of high-resolution satellite imagery of the Martian surface 11 has permitted landsliding to be studied on a global scale on Mars for the first time. 12 We apply the Scoops3D software package to compute slope stability for select 13 regions of the Martian surface, combining calculations of slope stability with 14 number of observed landslides, as reported in a recently published (Crosta et al., 15 2018a, b) inventory of Martian landslides, to understand controls on the global 16 distribution of landsliding on Mars. We find that the distribution of landsliding does 17 not simply follow the distribution of unstable slopes. In particular, there is an 18 increase in landsliding in the Tharsis Rise area, and especially in Valles Marineris 19 and Noctis Labyrinthus, that is not explained by an abundance of unstable 20 topography alone. We analyzed for but did not find a clear local lithologic or 21 stratigraphic control on landslide occurrence from subsurface heterogeneities. 22 Other possibilities to explain the increased occurrence of landslides in the Tharsis 23 Rise include (1) regionally widespread Tharsis weak unit(s), such as from 1 ESSOAr | https://doi.org/10.1002/essoar.10504190.1 | CC_BY_NC_4.0 | First posted online: Thu, 10 Sep 2020 06:23:21 | This content has not been peer reviewed.
    [Show full text]