Experiment Description Mission to Mars
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Quantitative High-Resolution Reexamination of a Hypothesized
RESEARCH ARTICLE Quantitative High‐Resolution Reexamination of a 10.1029/2018JE005837 Hypothesized Ocean Shoreline in Cydonia Key Points: • We apply a proposed Mensae on Mars ‐ fi paleoshoreline identi cation toolkit Steven F. Sholes1,2 , David R. Montgomery1, and David C. Catling1,2 to newer high‐resolution data of an exemplar site for paleoshorelines on 1Department of Earth and Space Sciences, University of Washington, Seattle, WA, USA, 2Astrobiology Program, Mars • Any wave‐generated University of Washington, Seattle, WA, USA paleoshorelines should exhibit expressions identifiable in the residual topography from an Abstract Primary support for ancient Martian oceans has relied on qualitative interpretations of idealized slope hypothesized shorelines on relatively low‐resolution images and data. We present a toolkit for • Our analysis of these curvilinear features does not support a quantitatively identifying paleoshorelines using topographic, morphological, and spectroscopic paleoshoreline interpretation and is evaluations. In particular, we apply the validated topographic expression analysis of Hare et al. (2001, more consistent with eroded https://doi.org/10.1029/2001JB000344) for the first time beyond Earth, focusing on a test case of putative lithologies shoreline features along the Arabia level in northeast Cydonia Mensae, as first described by Clifford and Supporting Information: Parker (2001, https://doi.org/10.1006/icar.2001.6671). Our results show these curvilinear features are • Supporting Information S1 inconsistent with a wave‐generated shoreline interpretation. The topographic expression analysis identifies a few potential shoreline terraces along the historically proposed contacts, but these tilt in different directions, do not follow an equipotential surface (even accounting for regional tilting), and are Correspondence to: not laterally continuous. -
Characterizing the Seasonal Cycle of Upper-Ocean Flows Under Multi-Year
Ocean Modelling 113 (2017) 115–130 Contents lists available at ScienceDirect Ocean Modelling journal homepage: www.elsevier.com/locate/ocemod Characterizing the seasonal cycle of upper-ocean flows under multi-year sea ice ∗ Jean A. Mensa , M.-L. Timmermans Department of Geology and Geophysics, Yale University, 210 Whitney Ave, New Haven CT 06511, USA a r t i c l e i n f o a b s t r a c t Article history: Observations in the Arctic Ocean suggest that upper-ocean dynamics under sea ice might be significantly Received 18 September 2016 weaker than in the temperate oceans. In particular, observational evidence suggests that currents devel- Revised 7 March 2017 oping under sea ice present weak or absent submesoscale ( O(1) Rossby number) dynamics, in contrast Accepted 18 March 2017 with midlatitude oceans typically characterized by more energetic dynamics at these scales. Idealized Available online 29 March 2017 numerical model results of the upper ocean under multi-year sea ice, subject to realistic forcing, are em- Keywords: ployed to describe the evolution of the submesoscale flow field. During both summer and winter under Mixed layer multi-year sea ice, the simulated submesoscale flow field is typically much less energetic than in the Arctic ocean midlatitude ice-free oceans. Rossby numbers under sea ice are generally consistent with geostrophic dy- Submesoscale namics ( Ro ∼ O(10 −3 ) ). During summer, ice melt generates a shallow mixed layer ( O(1) m) which isolates Sea ice the surface from deeper, warmer and saltier waters. The Ekman balance generally dominates the mixed layer, although inertial waves are present in the simulations during weakening and reversals of the ice- ocean stress. -
CYDONIA PYRAMID COMPLEX the SCARED PLANET Martian Motifs by Luis B
CYDONIA PYRAMID COMPLEX THE SCARED PLANET Martian Motifs by Luis B. Vega [email protected] www.PostScripts.org ‘…and with every wicked deception directed against those who are perishing, because they refused the love of the truth that would have saved them. For this reason, GOD will send them a powerful delusion so that they will believe The Lie, in order that judgment will come upon all who have disbelieved the truth and delighted in wickedness..’ -2 Thessalonians 2:10-12 The purpose of this study is to depict the various coordinates, approximate angles and measurements of the Cydonia pyramid complex anomaly on Mars. The depiction will be generated using Google Earth’s Mars coordinates, GPS calculations and figures. The illustration will show the entirety of the ‘Red Planet’, Mars from a frontal view that has the Valles Marineris featured very prominently. Although the rendition of the imagery is very low resolution, there is a general sense of where the Cydonia pyramid complex is situated on the planet. Although many in the past have composed a mathematical and Sacred Geometry association with the Cydonia ‘Pyramids’, this study will keep it simple and just touch on some elementary correlations. The study will only seek to highlight what is already known about the Cydonia, Mars pyramid anomaly but introduced new inferences and possible Biblical implications as to the Last Days coming deception. This study will delineate the Red Planet based on the concepts of Sacred Geometry. Depicted are 2 intersecting triangles that span the circle of the planet. These 2 triangles produce a hexagram centered on the Equator that is marked by Google and NASA. -
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. -
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180° 0° DODONA PLANUM 210° 330° 150° 30° 60° -60° . Bochica . Hatchawa Patera Patera . Nusku Patera . Hiruko Heno . Inti . Patera Patera Patera 70° -70° 240° 300° 60° 120° Tvashtar . Taranis Patera Iynx TARSUS Aramazd Mensa . Patera Tvashtar Paterae Haemus REGIO Montes Mensae LERNA REGIO 80° Echo -80°Mensa . Chors Nile Montes N Patera E M . Viracocha E Patera A 90° CHALYBES 270° 90° P 270° L A . Mithra N Patera U REGIO M . Vivasvant Patera . Crimea Mons 80° -80° Pyerun . Patera Dazhbog 120° 60° Patera . 300° 240° 70° -70° ILLYRIKON REGIO 60° -60° 30° 150° 330° 210° 0° 180° NORTH POLAR REGION SOUTH POLAR REGION 180° 170° 160° 150° 140° 130° 120° 110° 100° 90° 80° 70° 60° 50° 40° 30° 20° 10° 0° 350° 340° 330° 320° 310° 300° 290° 280° 270° 260° 250° 240° 230° 220° 210° 200° 190° 180° 57° 57° Nile Montes Dazhbog Patera CHALYBES REGIO 50° 50° . Kinich Ahau . Savitr Patera Patera Surt Zal Montes Lei-Kung Zal Fluctus . Fo Patera 40° 40° Patera Thor . Amaterasu . Dusura Patera Patera BULICAME . Manua Patera Shango REGIO Arinna . _ Patera Ukko . Atar Fluctus . Patera Patera Heiseb Isum 30° . 30° Fuchi Patera Patera Reshef Euxine . Patera Mons Patera Volund . Thomagata Amirani Patera . Shakuru Skythia Mons Girru . Mongibello . Tiermes Patera . Susanoo Donar Surya Estan Patera Patera . Patera Mons Patera Fluctus Patera Monan Daedalus 20° . Patera Loki . 20° Zamama Maui . Gish Bar Patera Mons Mulungu Steropes Maui . Patera . Patera Ruaumoko . Camaxtli Patera Gish Bar Sobo Patera . Patera Patera Fluctus Monan Loki Chaac . Ababinili Tien Mu Mons Llew . Balder Patera . Fjorgynn Patera . -
Participant List
Participant List 10/20/2019 8:45:44 AM Category First Name Last Name Position Organization Nationality CSO Jillian Abballe UN Advocacy Officer and Anglican Communion United States Head of Office Ramil Abbasov Chariman of the Managing Spektr Socio-Economic Azerbaijan Board Researches and Development Public Union Babak Abbaszadeh President and Chief Toronto Centre for Global Canada Executive Officer Leadership in Financial Supervision Amr Abdallah Director, Gulf Programs Educaiton for Employment - United States EFE HAGAR ABDELRAHM African affairs & SDGs Unit Maat for Peace, Development Egypt AN Manager and Human Rights Abukar Abdi CEO Juba Foundation Kenya Nabil Abdo MENA Senior Policy Oxfam International Lebanon Advisor Mala Abdulaziz Executive director Swift Relief Foundation Nigeria Maryati Abdullah Director/National Publish What You Pay Indonesia Coordinator Indonesia Yussuf Abdullahi Regional Team Lead Pact Kenya Abdulahi Abdulraheem Executive Director Initiative for Sound Education Nigeria Relationship & Health Muttaqa Abdulra'uf Research Fellow International Trade Union Nigeria Confederation (ITUC) Kehinde Abdulsalam Interfaith Minister Strength in Diversity Nigeria Development Centre, Nigeria Kassim Abdulsalam Zonal Coordinator/Field Strength in Diversity Nigeria Executive Development Centre, Nigeria and Farmers Advocacy and Support Initiative in Nig Shahlo Abdunabizoda Director Jahon Tajikistan Shontaye Abegaz Executive Director International Insitute for Human United States Security Subhashini Abeysinghe Research Director Verite -
Underlying Structural Control of Small-Scale Faults and Fractures in West Candor Chasma, Mars C
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E11001, doi:10.1029/2012JE004144, 2012 Underlying structural control of small-scale faults and fractures in West Candor Chasma, Mars C. Birnie,1 F. Fueten,1 R. Stesky,2 and E. Hauber3 Received 29 May 2012; revised 4 September 2012; accepted 18 September 2012; published 2 November 2012. [1] Orientations of small-scale faults and fractures within the interior layered deposits of West Candor Chasma were measured to investigate what information about the geologic history of Valles Marineris they can contribute. Deformational features were separated into six categories based on morphology and their orientations were analyzed. The elevations at which the deformational features formed are recorded, as a proxy for stratigraphic level. Deformational features occur over a continuous range of elevations and display regionally consistent preferred orientations, indicating their formation was controlled by a regional stress regime. The two most abundant preferred orientations of 35 and 110 are approximately parallel to the chasma walls and the inferred underlying normal faults. The alignment of three populations of small faults at 140, consistent with the morphology of release faults, indicates a large-scale fault underlying the southeastern border of Ceti Mensa. The preferred orientations imply these small-scale deformational features formed from a continuation of the same imposed stresses responsible for the formation of Valles Marineris, indicating these stresses existed past the formation of the interior layered deposits. The origins of a fourth preferred orientation of 70 is less clear but suggests the study area has undergone at least two periods of deformation. Citation: Birnie, C., F. -
Distribution, Morphology, and Morphometry of Circular Mounds in the Elongated Basin of Northern Terra Sirenum, Mars Ryodo Hemmi and Hideaki Miyamoto*
Hemmi and Miyamoto Progress in Earth and Planetary Science (2017) 4:26 Progress in Earth and DOI 10.1186/s40645-017-0141-x Planetary Science RESEARCH ARTICLE Open Access Distribution, morphology, and morphometry of circular mounds in the elongated basin of northern Terra Sirenum, Mars Ryodo Hemmi and Hideaki Miyamoto* Abstract An elongated, flat-floored basin, located in the northern part of Terra Sirenum on Mars, holds numerous enigmatic mounds (100 m wide) on the surface of its floor. We investigated their geological context, spatial distribution, morphological characteristics, and morphometric parameters by analyzing a variety of current remote sensing data sets of Mars. Over 700 mounds are identified; mapping of the mounds shows the spatial density of about 21 per 100 km2 and appearances of several clusters, coalescence, and/or alignment. Most of the mounds have smoother surface textures in contrast to the rugged surrounding terrain. Some of the mounds display depressions on their summits, meter-sized boulders on their flanks, and distinct lobate features. We also perform high-resolution topographic analysis on 50 isolated mounds, which reveals that their heights range from 6 to 43 m with a mean of 18 m and average flank slopes of most mounds are below 10°. These characteristics are consistent with the deposition and extension of mud slurries with mud breccia and gases extruded from subsurface, almost equivalent to terrestrial mud volcanism. If so, both abundance of groundwater and abrupt increase in pore fluid pressure are necessary for triggering mud eruption. Absolute crater retention ages suggest that the floor of the basin located among middle Noachian-aged highland terrains has been resurfaced during the Late Hesperian Epoch. -
Durham Research Online
Durham Research Online Deposited in DRO: 27 March 2019 Version of attached le: Published Version Peer-review status of attached le: Peer-reviewed Citation for published item: Orgel, Csilla and Hauber, Ernst and Gasselt, Stephan and Reiss, Dennis and Johnsson, Andreas and Ramsdale, Jason D. and Smith, Isaac and Swirad, Zuzanna M. and S¡ejourn¡e,Antoine and Wilson, Jack T. and Balme, Matthew R. and Conway, Susan J. and Costard, Francois and Eke, Vince R. and Gallagher, Colman and Kereszturi, Akos¡ and L osiak, Anna and Massey, Richard J. and Platz, Thomas and Skinner, James A. and Teodoro, Luis F. A. (2019) 'Grid mapping the Northern Plains of Mars : a new overview of recent water and icerelated landforms in Acidalia Planitia.', Journal of geophysical research : planets., 124 (2). pp. 454-482. Further information on publisher's website: https://doi.org/10.1029/2018JE005664 Publisher's copyright statement: Orgel, Csilla, Hauber, Ernst, Gasselt, Stephan, Reiss, Dennis, Johnsson, Andreas, Ramsdale, Jason D., Smith, Isaac, Swirad, Zuzanna M., S¡ejourn¡e,Antoine, Wilson, Jack T., Balme, Matthew R., Conway, Susan J., Costard, Francois, Eke, Vince R., Gallagher, Colman, Kereszturi, Akos,¡ L osiak, Anna, Massey, Richard J., Platz, Thomas, Skinner, James A. Teodoro, Luis F. A. (2019). Grid Mapping the Northern Plains of Mars: A New Overview of Recent Water and IceRelated Landforms in Acidalia Planitia. Journal of Geophysical Research: Planets 124(2): 454-482. 10.1029/2018JE005664. To view the published open abstract, go to https://doi.org/ and enter the DOI. Additional information: Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. -
History of Outflow Channel Flooding from an Integrated Basin System East of Valles Marineris, Mars
47th Lunar and Planetary Science Conference (2016) 2214.pdf History of Outflow Channel Flooding from an Integrated Basin System East of Valles Marineris, Mars. N. Wagner1, N.H. Warner1, and S. Gupta2, 1State University of New York at Geneseo, Department of Geological Sciences, 1 College Circle, Geneseo, NY 14454, USA. [email protected]. 2Earth Science and Engineering, Imperial College London, South Kensington Campus, London, SW7 2AZ, United Kingdom Introduction: The eastern end of Valles Marineris [6, 7], including all craters with diameters > 200 m in includes diverse terrain formed from extensional forces the count. and collapse due to groundwater release. Capri For the paleohydrology analysis, the topographic Chasma, Eos Chaos, Ganges Chasma, and Aurorae characteristics and dimensions of each channel were Chaos (Fig. 1) were all likely formed due to a measured using the HRSC DTM. Paleo-flow depths combination of these processes [1,2]. were determined based on the observation of trimlines Importantly, this region shows evidence that that mark the margins of individual bedrock terraces. significant volumes of overland water flow travelled These terraces were first identified by [4] and have through this integrated basin system [3,4,5]. been mapped here within every outlet channel that Furthermore, recent studies have suggested that liquid exits an upstream basin. The presence of multiple water was at least temporarily stable here [4]. The bedrock terraces and trimlines indicates that the topographic and temporal relationships between Eos channels were formed by progressively deeper incision Chaos and its associated outflow channels for example and also suggests that bankfull estimates of these demonstrate that the upstream chaotic terrains pre-date channels are gross over-estimates. -
Symmetry and Geometry of the Face on Mars Revealed a New Analysis Based on the April 2001 Image Mark J
© 2001 New Frontiers in Science (ISSN 1537-3169) newfrontiersinscience.com Symmetry and Geometry of the Face on Mars Revealed A New Analysis Based on the April 2001 Image Mark J. Carlotto, Ph. D. On April 8, 2001 Mars Global Surveyor (MGS) was able for the first time to obtain a fully illuminated high resolution image of the Face on Mars. Like previous MGS images the Face appears at first glance to be a highly eroded natural formation. However analysis of this new image shows the object to possess a very high degree of symmetry in two directions. Using repeatable geometrical constructions based on clearly resolved features the Face appears to fit a consistently expressed geometrical model based on rectangles having a long to short side ratio of 4/3, i.e., by rectangles diagonally bisected by 3-4-5 right triangles. Analysis of the new image reveals that the right (east) side of the Face is covered with sand. The depth of the sand appears to be sufficient to have covered over some of the detail on the east side and may account for its apparent lack of facial symmetry. 1. Introduction The Face on Mars is a mile long formation on the surface of Mars that resembles a humanoid face. First photographed by a Viking Orbiter spacecraft in July 1976, the Face was dismissed by NASA's Jet Propulsion Laboratory as an optical illusion -- a rock formation that happened to look like a face because of the way it was lit by the sun (JPL 1976). Several years later two engineers at the Goddard Space Flight Center (DiPietro and Molenaar 1986) found a second image of it taken at a different sun angle that also exhibited facial characteristics. -
Water Deficit Affects the Growth and Leaf Metabolite Composition Of
plants Article Water Deficit Affects the Growth and Leaf Metabolite Composition of Young Loquat Plants Giovanni Gugliuzza 1, Giuseppe Talluto 1, Federico Martinelli 2, Vittorio Farina 3 and Riccardo Lo Bianco 3,* 1 CREA—Research Centre for Plant Protection and Certification, SS 113 Km 245.500, 90011 Bagheria, Italy; [email protected] (G.G.); [email protected] (G.T.) 2 Department of Biology, University of Florence, via Madonna del Piano 6, 50019 Sesto Fiorentino, Italy; federico.martinelli@unifi.it 3 Department of Agricultural, Food and Forest Sciences, University of Palermo, Viale delle Scienze, Ed. 4, 90128 Palermo, Italy; [email protected] * Correspondence: [email protected]; Tel.: +39-091-238-96097 Received: 21 January 2020; Accepted: 17 February 2020; Published: 19 February 2020 Abstract: Water scarcity in the Mediterranean area is very common and understanding responses to drought is important for loquat management and production. The objective of this study was to evaluate the effect of drought on the growth and metabolism of loquat. Ninety two-year-old plants of ‘Marchetto’ loquat grafted on quince were grown in the greenhouse in 12-liter pots and three irrigation regimes were imposed starting on 11 May and lasting until 27 July, 2013. One-third of the plants was irrigated with 100% of the water consumed (well watered, WW), a second group of plants was irrigated with 66% of the water supplied to the WW plants (mild drought, MD), and a third group was irrigated with 33% of the water supplied to the WW plants (severe drought, SD). Minimum water potential levels of 2.0 MPa were recorded in SD plants at the end of May.