NASA ASTROBIOLOGY STRATEGY 2015 I
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Marina Galand
Thermosphere - Ionosphere - Magnetosphere Coupling! Canada M. Galand (1), I.C.F. Müller-Wodarg (1), L. Moore (2), M. Mendillo (2), S. Miller (3) , L.C. Ray (1) (1) Department of Physics, Imperial College London, London, U.K. (2) Center for Space Physics, Boston University, Boston, MA, USA (3) Department of Physics and Astronomy, University College London, U.K. 1." Energy crisis at giant planets Credit: NASA/JPL/Space Science Institute 2." TIM coupling Cassini/ISS (false color) 3." Modeling of IT system 4." Comparison with observaons Cassini/UVIS 5." Outstanding quesAons (Pryor et al., 2011) SATURN JUPITER (Gladstone et al., 2007) Cassini/UVIS [UVIS team] Cassini/VIMS (IR) Credit: J. Clarke (BU), NASA [VIMS team/JPL, NASA, ESA] 1. SETTING THE SCENE: THE ENERGY CRISIS AT THE GIANT PLANETS THERMAL PROFILE Exosphere (EARTH) Texo 500 km Key transiLon region Thermosphere between the space environment and the lower atmosphere Ionosphere 85 km Mesosphere 50 km Stratosphere ~ 15 km Troposphere SOLAR ENERGY DEPOSITION IN THE UPPER ATMOSPHERE Solar photons ion, e- Neutral Suprathermal electrons B ion, e- Thermal e- Ionospheric Thermosphere Ne, Nion e- heang Te P, H * + Airglow Neutral atmospheric Exothermic reacAons heang IS THE SUN THE MAIN ENERGY SOURCE OF PLANERATY THERMOSPHERES? W Main energy source: UV solar radiaon Main energy source? EartH Outer planets CO2 atmospHeres Exospheric temperature (K) [aer Mendillo et al., 2002] ENERGY CRISIS AT THE GIANT PLANETS Observed values at low to mid-latudes solsce equinox Modeled values (Sun only) [Aer -
Where Less May Be More: How the Rare Biosphere Pulls Ecosystems Strings
The ISME Journal (2017) 11, 853–862 OPEN © 2017 International Society for Microbial Ecology All rights reserved 1751-7362/17 www.nature.com/ismej MINI REVIEW Where less may be more: how the rare biosphere pulls ecosystems strings Alexandre Jousset1, Christina Bienhold2,3, Antonis Chatzinotas4,5, Laure Gallien6,7, Angélique Gobet8, Viola Kurm9, Kirsten Küsel10,5, Matthias C Rillig11,12, Damian W Rivett13, Joana F Salles14, Marcel GA van der Heijden15,16,17, Noha H Youssef18, Xiaowei Zhang19, Zhong Wei20 and WH Gera Hol9 1Utrecht University, Department of Biology, Institute of Environmental Biology, Ecology and Biodiversity Group, Utrecht, The Netherlands; 2Alfred Wegener Institute Helmholtz Centre for Polar and Marine Research, Bremerhaven, Germany; 3Max Planck Institute for Marine Microbiology, Bremen, Germany; 4Helmholtz Centre for Environmental Research – UFZ, Leipzig, Germany; 5German Centre for Integrative Biodiversity Research (iDiv), Halle-Jena-Leipzig, Leipzig, Germany; 6Swiss Federal Institute for Forest, Snow and Landscape Research WSL, Birmensdorf, Switzerland; 7Center for Invasion Biology, Department of Botany & Zoology, Stellenbosch University, Matieland, South Africa; 8Sorbonne Universités, UPMC Université Paris 06, CNRS, UMR 8227, Integrative Biology of Marine Models, Station Biologique de Roscoff, F-29688, Roscoff Cedex, France; 9Netherlands Institute of Ecology, Department of Terrestrial Ecology, Wageningen, The Netherlands; 10Friedrich Schiller University Jena, Institute of Ecology, Jena, Germany; 11Freie Universtät Berlin, -
A Future Mars Environment for Science and Exploration
Planetary Science Vision 2050 Workshop 2017 (LPI Contrib. No. 1989) 8250.pdf A FUTURE MARS ENVIRONMENT FOR SCIENCE AND EXPLORATION. J. L. Green1, J. Hol- lingsworth2, D. Brain3, V. Airapetian4, A. Glocer4, A. Pulkkinen4, C. Dong5 and R. Bamford6 (1NASA HQ, 2ARC, 3U of Colorado, 4GSFC, 5Princeton University, 6Rutherford Appleton Laboratory) Introduction: Today, Mars is an arid and cold world of existing simulation tools that reproduce the physics with a very thin atmosphere that has significant frozen of the processes that model today’s Martian climate. A and underground water resources. The thin atmosphere series of simulations can be used to assess how best to both prevents liquid water from residing permanently largely stop the solar wind stripping of the Martian on its surface and makes it difficult to land missions atmosphere and allow the atmosphere to come to a new since it is not thick enough to completely facilitate a equilibrium. soft landing. In its past, under the influence of a signif- Models hosted at the Coordinated Community icant greenhouse effect, Mars may have had a signifi- Modeling Center (CCMC) are used to simulate a mag- cant water ocean covering perhaps 30% of the northern netic shield, and an artificial magnetosphere, for Mars hemisphere. When Mars lost its protective magneto- by generating a magnetic dipole field at the Mars L1 sphere, three or more billion years ago, the solar wind Lagrange point within an average solar wind environ- was allowed to directly ravish its atmosphere.[1] The ment. The magnetic field will be increased until the lack of a magnetic field, its relatively small mass, and resulting magnetotail of the artificial magnetosphere its atmospheric photochemistry, all would have con- encompasses the entire planet as shown in Figure 1. -
Bayesian Analysis of the Astrobiological Implications of Life's
Bayesian analysis of the astrobiological implications of life's early emergence on Earth David S. Spiegel ∗ y, Edwin L. Turner y z ∗Institute for Advanced Study, Princeton, NJ 08540,yDept. of Astrophysical Sciences, Princeton Univ., Princeton, NJ 08544, USA, and zInstitute for the Physics and Mathematics of the Universe, The Univ. of Tokyo, Kashiwa 227-8568, Japan Submitted to Proceedings of the National Academy of Sciences of the United States of America Life arose on Earth sometime in the first few hundred million years Any inferences about the probability of life arising (given after the young planet had cooled to the point that it could support the conditions present on the early Earth) must be informed water-based organisms on its surface. The early emergence of life by how long it took for the first living creatures to evolve. By on Earth has been taken as evidence that the probability of abiogen- definition, improbable events generally happen infrequently. esis is high, if starting from young-Earth-like conditions. We revisit It follows that the duration between events provides a metric this argument quantitatively in a Bayesian statistical framework. By (however imperfect) of the probability or rate of the events. constructing a simple model of the probability of abiogenesis, we calculate a Bayesian estimate of its posterior probability, given the The time-span between when Earth achieved pre-biotic condi- data that life emerged fairly early in Earth's history and that, billions tions suitable for abiogenesis plus generally habitable climatic of years later, curious creatures noted this fact and considered its conditions [5, 6, 7] and when life first arose, therefore, seems implications. -
Comparative Saturn-Versus-Jupiter Tether Operation
Journal of Geophysical Research: Space Physics Comparative Saturn-Versus-Jupiter Tether Operation J. R. Sanmartin1 ©, J. Pelaez1 ©, and I. Carrera-Calvo1 Abstract Saturn, Uranus, and Neptune, among the four Giant Outer planets, have magnetic field B about 20 times weaker than Jupiter. This could suggest, in principle, that planetary capture and operation using tethers, which involve B effects twice, might be much less effective at Saturn, in particular, than at Jupiter. It was recently found, however, that the very high Jovian B itself strongly limits conditions for tether use, maximum captured spacecraft-to-tether mass ratio only reaching to about 3.5. Further, it is here shown that planetary parameters and low magnetic field might make tether operation at Saturn more effective than at Jupiter. Operation analysis involves electron plasma density in a limited radial range, about 1-1.5 times Saturn radius, and is weakly requiring as regards density modeling. 1. Introduction All Giant Outer planets have magnetic field B and corotating plasma, allowing nonconventional exploration. Electrodynamic tethers, which are thermodynamic (dissipative) in character, can 1. provide propellantless drag both for deorbiting spacecraft in Low Earth Orbit at end of mission and for planetary spacecraft capture and operation down the gravitational well, and 2. generate accompanying, useful electrical power, or store it to later invert tether current (Sanmartin et al., 1993; Sanmartin & Estes, 1999). At Jupiter, tethers could be effective because its field B is high (Sanmartin et al., 2008). Tethers would allow a variety of science applications (Sanchez-Torres & Sanmartin, 2011). The Saturn field is 20 times smaller, however, and tether operation involves field B twice, which makes that thermodynamic character manifest: 1. -
Amplification by PCR Artificially Reduces the Proportion of the Rare Biosphere in Microbial Communities
Amplification by PCR Artificially Reduces the Proportion of the Rare Biosphere in Microbial Communities Juan M. Gonzalez1*, Maria C. Portillo1, Pedro Belda-Ferre2, Alex Mira2 1 Institute of Natural Resources and Agrobiology, Spanish Council for Research, IRNAS-CSIC, Sevilla, Spain, 2 Genomics and Health Department, Center for Advanced Research in Public Health (CSISP), Valencia, Spain Abstract The microbial world has been shown to hold an unimaginable diversity. The use of rRNA genes and PCR amplification to assess microbial community structure and diversity present biases that need to be analyzed in order to understand the risks involved in those estimates. Herein, we show that PCR amplification of specific sequence targets within a community depends on the fractions that those sequences represent to the total DNA template. Using quantitative, real-time, multiplex PCR and specific Taqman probes, the amplification of 16S rRNA genes from four bacterial species within a laboratory community were monitored. Results indicate that the relative amplification efficiency for each bacterial species is a nonlinear function of the fraction that each of those taxa represent within a community or multispecies DNA template. Consequently, the low-proportion taxa in a community are under-represented during PCR-based surveys and a large number of sequences might need to be processed to detect some of the bacterial taxa within the ‘rare biosphere’. The structure of microbial communities from PCR-based surveys is clearly biased against low abundant taxa which are required to decipher the complete extent of microbial diversity in nature. Citation: Gonzalez JM, Portillo MC, Belda-Ferre P, Mira A (2012) Amplification by PCR Artificially Reduces the Proportion of the Rare Biosphere in Microbial Communities. -
Geobiology of the Late Paleoproterozoic Duck Creek Formation, Western Australia
Precambrian Research 179 (2010) 135–149 Contents lists available at ScienceDirect Precambrian Research journal homepage: www.elsevier.com/locate/precamres Geobiology of the late Paleoproterozoic Duck Creek Formation, Western Australia Jonathan P. Wilson a,b,∗, Woodward W. Fischer b, David T. Johnston a, Andrew H. Knoll c, John P. Grotzinger b, Malcolm R. Walter e, Neal J. McNaughton i, Mel Simon d, John Abelson d, Daniel P. Schrag a, Roger Summons f, Abigail Allwood g, Miriam Andres h, Crystal Gammon b, Jessica Garvin j, Sky Rashby b, Maia Schweizer b, Wesley A. Watters f a Department of Earth and Planetary Sciences, Harvard University, USA b Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA c Department of Organismic and Evolutionary Biology, Harvard University, USA d The Agouron Institute, USA e Australian Centre for Astrobiology, University of New South Wales, Australia f Massachusetts Institute of Technology, USA g Jet Propulsion Laboratory, USA h Chevron Corp., USA i Curtin University of Technology, Australia j University of Washington, USA article info abstract Article history: The ca. 1.8 Ga Duck Creek Formation, Western Australia, preserves 1000 m of carbonates and minor Received 25 August 2009 iron formation that accumulated along a late Paleoproterozoic ocean margin. Two upward-deepening Received in revised form 12 February 2010 stratigraphic packages are preserved, each characterized by peritidal precipitates at the base and iron Accepted 15 February 2010 formation and carbonate turbidites in its upper part. Consistent with recent studies of Neoarchean basins, carbon isotope ratios of Duck Creek carbonates show no evidence for a strong isotopic depth gradient, but carbonate minerals in iron formations can be markedly depleted in 13C. -
The Cyclical Influence of Society and Music
Conspectus Borealis Volume 6 Issue 1 Article 15 3-13-2020 The Cyclical Influence of Society and Music Bailey Gomes Northern Michigan University, [email protected] Follow this and additional works at: https://commons.nmu.edu/conspectus_borealis Part of the Music Commons, Politics and Social Change Commons, Social Influence and oliticalP Communication Commons, Social Justice Commons, and the Social Media Commons Recommended Citation Gomes, Bailey (2020) "The Cyclical Influence of Society and Music," Conspectus Borealis: Vol. 6 : Iss. 1 , Article 15. Available at: https://commons.nmu.edu/conspectus_borealis/vol6/iss1/15 This Scholarly Article is brought to you for free and open access by the Journals and Peer-Reviewed Series at NMU Commons. It has been accepted for inclusion in Conspectus Borealis by an authorized administrator of NMU Commons. For more information, please contact Kevin McDonough. The Cyclical Influence of Society and Music Throughout time, there have been discussions over the age-old question: ‘which came first, the chicken or the egg?’ This type of question applies to many other areas of life and it is the basis for this paper. The question that this paper explores is ‘does society change music, or does music change society?’ This paper will show that neither came first, but rather they exist simultaneously in a never-ending cycle. By discussing the influences of two musical icons, Pearl Jam and Lady Gaga, this paper will show the perpetual cycle of how society and music influence each other. Society is constantly changing and there are always movements that gain public attention. Whether that attention is positive or negative does not matter; it is attention nonetheless. -
Diving Deep for Knowledge Stars in Our Solar System
The Daring Journey “ The exhilaration of seeing first- ’m an explorer at heart. As a child I was al- ways drawn to the ocean and the mysterious hand previously unexplored areas of Ianimal life below its surface. As an adult I’m the deep ocean and the promise for still captivated by the ocean’s vast and powerful life-sustaining role on Earth, but I’ve turned my new discoveries remains as strong attention away from the charismatic tropical fish, a motivator for me today as on my coral reefs and marine mammals that captured my imagination in my youth to a vibrant ocean first dive well over a decade ago.” world of microbes that often goes unnoticed. This world is invisible to our unaided eye — teeming with single-celled bacteria, archaea, protists and viruses, the smallest life forms and among the most difficult to study. They number among the million trillion trillions in ocean waters and deep sediments, far surpassing the total number of Diving Deep for Knowledge stars in our solar system. Researchers in the relatively young field known as geobiology are just beginning to understand the intricacies of this complex microbial world closely with organic and isotope geochemists, pe- associated with each of our respective methodolog- and how it has changed over the course of Earth’s troleum geologists and earth scientists. From this ical approaches was a challenge. I still remember history. However, what is clear is that the col- experience, I gained a deep appreciation for the my dismay after discussing the details of the SIMS lective metabolic activity of microorganisms in benefits and challenges of cross-disciplinary col- instrument with Chris over the phone, having real- terrestrial and marine environments continues to laborations. -
Monday, November 13, 2017 WHAT DOES IT MEAN to BE HABITABLE? 8:15 A.M. MHRGC Salons ABCD 8:15 A.M. Jang-Condell H. * Welcome C
Monday, November 13, 2017 WHAT DOES IT MEAN TO BE HABITABLE? 8:15 a.m. MHRGC Salons ABCD 8:15 a.m. Jang-Condell H. * Welcome Chair: Stephen Kane 8:30 a.m. Forget F. * Turbet M. Selsis F. Leconte J. Definition and Characterization of the Habitable Zone [#4057] We review the concept of habitable zone (HZ), why it is useful, and how to characterize it. The HZ could be nicknamed the “Hunting Zone” because its primary objective is now to help astronomers plan observations. This has interesting consequences. 9:00 a.m. Rushby A. J. Johnson M. Mills B. J. W. Watson A. J. Claire M. W. Long Term Planetary Habitability and the Carbonate-Silicate Cycle [#4026] We develop a coupled carbonate-silicate and stellar evolution model to investigate the effect of planet size on the operation of the long-term carbon cycle, and determine that larger planets are generally warmer for a given incident flux. 9:20 a.m. Dong C. F. * Huang Z. G. Jin M. Lingam M. Ma Y. J. Toth G. van der Holst B. Airapetian V. Cohen O. Gombosi T. Are “Habitable” Exoplanets Really Habitable? A Perspective from Atmospheric Loss [#4021] We will discuss the impact of exoplanetary space weather on the climate and habitability, which offers fresh insights concerning the habitability of exoplanets, especially those orbiting M-dwarfs, such as Proxima b and the TRAPPIST-1 system. 9:40 a.m. Fisher T. M. * Walker S. I. Desch S. J. Hartnett H. E. Glaser S. Limitations of Primary Productivity on “Aqua Planets:” Implications for Detectability [#4109] While ocean-covered planets have been considered a strong candidate for the search for life, the lack of surface weathering may lead to phosphorus scarcity and low primary productivity, making aqua planet biospheres difficult to detect. -
CURRICULUM VITAE Edward Francis Delong, Professor Department Of
CURRICULUM VITAE Edward Francis DeLong, Professor Department of Oceanography, School of Ocean and Earth Science and Technology Center for Microbial Oceanography: Research and Education Co-Director, Simons Collaboration on Ocean Processes and Ecology University of Hawaii, Manoa, Honolulu, 96822 Ph: 808-956-0563 Fax: 808-956-5059 email: [email protected]; [email protected] http://en.wikipedia.org/wiki/Edward_DeLong http://scholar.google.com/citations?user=wEkWbTQAAAAJ&hl=en http://scope.soest.hawaii.edu http://www.soest.hawaii.edu/oceanography/faculty/DeLong.html Education: A. S., Biology, Santa Rosa Junior College, 1980 B. S., Bacteriology, University of California Davis, 1982 Ph. D., Marine Biology, Scripps Institute of Oceanography, 1986 Thesis title: Adaptations of deep-sea bacteria to the abyssal environment Professional Experience: 2014- Professor of Oceanography, SOEST, University of Hawaii, Manoa 2014- co-Director, Simons Collaboration on Ocean Processes and Ecology (SCOPE) 2006-2016 co-Director, Center for Microbial Oceanography: Research and Education 2004-2015 Professor, Massachusetts Institute of Technology 1998-2004 Senior Scientist V, Monterey Bay Aquarium Research Inst. 1997-2002 Science Dept. Chair, Monterey Bay Aquarium Research Inst. 1997-1999 Associate Scientist III, Monterey Bay Aquarium Research Inst. 1996-1998 Associate Professor, Ecology, Evolution Marine Biol. Dept., UCSB 1992-1996 Assistant Professor, Biology Dept., UC Santa Barbara 1989-1991 Assistant Scientist, Woods Hole Oceanographic Inst. 1986-1989 Post-doctoral Research Assoc., Indiana U., Bloomington, Indiana 1984-1986 Teaching Assistant, Biology Dept., UC San Diego 1982-1986 Research Assistant, Scripps Inst. of Oceanography, UC San Diego 1981-1982 Research Assistant, University of California, Davis, Ca. Professional interests: Physiology, biochemistry, ecology, and evolution of microbes. -
Jet Propulsion Laboratory, Digital Converters
Jet JUNE Propulsion 2014 Laboratory VOLUME 43 NUMBER 6 JPL 2025 What will JPL be like in 2025? What kind of missions will it be building and flying? How different will the lab be from the JPL of today? Those were the questions on the minds of Executive Council members in early May when they held their annual planning retreat. Over three days they laid out the broad strokes of strategies to make each of the lab’s major program areas robust a decade or more from now. “JPL is currently in good shape, but to remain that way we have to focus on where we are going across the next decade,” JPL Director Charles Elachi said follow- ing the off-site meeting. Among the strategies planned for JPL’s major units, in coming years the Solar System Exploration Director- ate hopes to create missions across a broad spectrum of scales—from flagships to miniature spacecraft. One major focus is to explore the ocean worlds in the outer solar system. The first step for this goal is to continue the development of what is hoped will be the next outer planet mission, Europa Clipper. Thanks to the power of NASA’s new Space Launch System, missions to the outer planets may become more frequent. JPL would also like to execute the first interplanetary mission using a pair of miniature cube- sat spacecraft. The Asteroid Redirect Mission in which JPL has a key role may serve as a model for future Clockwise: 1) Europa Clipper; 2) Mars; 3) Mars Sample Return lander; 4) solar system; 5) Earth satellites; 6) the pulsar planets PSR B1257+12 b, c, and d; 7) spiral closer collaborations with other NASA centers.