The Astrobiology Primer V2.0
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Lecture-29 (PDF)
Life in the Universe Orin Harris and Greg Anderson Department of Physics & Astronomy Northeastern Illinois University Spring 2021 c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 1 / 95 Overview Dating Rocks Life on Earth How Did Life Arise? Life in the Solar System Life Around Other Stars Interstellar Travel SETI Review c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 2 / 95 Dating Rocks Zircon Dating Sedimentary Grand Canyon Life on Earth How Did Life Arise? Life in the Solar System Life Around Dating Rocks Other Stars Interstellar Travel SETI Review c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 3 / 95 Zircon Dating Zircon, (ZrSiO4), minerals incorporate trace amounts of uranium but reject lead. Naturally occuring uranium: • U-238: 99.27% • U-235: 0.72% Decay chains: • 238U −→ 206Pb, τ =4.47 Gyrs. • 235U −→ 207Pb, τ = 704 Myrs. 1956, Clair Camron Patterson dated the Canyon Diablo meteorite: τ =4.55 Gyrs. c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 4 / 95 Dating Sedimentary Rocks • Relative ages: Deeper layers were deposited earlier • Absolute ages: Decay of radioactive isotopes old (deposited last) oldest (depositedolder first) c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 5 / 95 Grand Canyon: Earth History from 200 million - 2 billion yrs ago. Dating Rocks Life on Earth Earth History Timeline Late Heavy Bombardment Hadean Shark Bay Stromatolites Cyanobacteria Q: Earliest Fossils? Life on Earth O2 History Q: Life on Earth How Did Life Arise? Life in the Solar System Life Around Other Stars Interstellar Travel SETI Review c 2012-2021 G. -
JUICE Red Book
ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat. -
LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned
Space Sci Rev DOI 10.1007/s11214-011-9759-y LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned Jennifer L. Heldmann · Anthony Colaprete · Diane H. Wooden · Robert F. Ackermann · David D. Acton · Peter R. Backus · Vanessa Bailey · Jesse G. Ball · William C. Barott · Samantha K. Blair · Marc W. Buie · Shawn Callahan · Nancy J. Chanover · Young-Jun Choi · Al Conrad · Dolores M. Coulson · Kirk B. Crawford · Russell DeHart · Imke de Pater · Michael Disanti · James R. Forster · Reiko Furusho · Tetsuharu Fuse · Tom Geballe · J. Duane Gibson · David Goldstein · Stephen A. Gregory · David J. Gutierrez · Ryan T. Hamilton · Taiga Hamura · David E. Harker · Gerry R. Harp · Junichi Haruyama · Morag Hastie · Yutaka Hayano · Phillip Hinz · Peng K. Hong · Steven P. James · Toshihiko Kadono · Hideyo Kawakita · Michael S. Kelley · Daryl L. Kim · Kosuke Kurosawa · Duk-Hang Lee · Michael Long · Paul G. Lucey · Keith Marach · Anthony C. Matulonis · Richard M. McDermid · Russet McMillan · Charles Miller · Hong-Kyu Moon · Ryosuke Nakamura · Hirotomo Noda · Natsuko Okamura · Lawrence Ong · Dallan Porter · Jeffery J. Puschell · John T. Rayner · J. Jedadiah Rembold · Katherine C. Roth · Richard J. Rudy · Ray W. Russell · Eileen V. Ryan · William H. Ryan · Tomohiko Sekiguchi · Yasuhito Sekine · Mark A. Skinner · Mitsuru Sôma · Andrew W. Stephens · Alex Storrs · Robert M. Suggs · Seiji Sugita · Eon-Chang Sung · Naruhisa Takatoh · Jill C. Tarter · Scott M. Taylor · Hiroshi Terada · Chadwick J. Trujillo · Vidhya Vaitheeswaran · Faith Vilas · Brian D. Walls · Jun-ihi Watanabe · William J. Welch · Charles E. Woodward · Hong-Suh Yim · Eliot F. Young Received: 9 October 2010 / Accepted: 8 February 2011 © The Author(s) 2011. -
USGS Open-File Report 2005-1190, Table 1
TABLE 1 GEOLOGIC FIELD-TRAINING OF NASA ASTRONAUTS BETWEEN JANUARY 1963 AND NOVEMBER 1972 The following is a year-by-year listing of the astronaut geologic field training trips planned and led by personnel from the U.S. Geological Survey’s Branches of Astrogeology and Surface Planetary Exploration, in collaboration with the Geology Group at the Manned Spacecraft Center, Houston, Texas at the request of NASA between January 1963 and November 1972. Regional geologic experts from the U.S. Geological Survey and other governmental organizations and universities s also played vital roles in these exercises. [The early training (between 1963 and 1967) involved a rather large contingent of astronauts from NASA groups 1, 2, and 3. For another listing of the astronaut geologic training trips and exercises, including all attending and the general purposed of the exercise, the reader is referred to the following website containing a contribution by William Phinney (Phinney, book submitted to NASA/JSC; also http://www.hq.nasa.gov/office/pao/History/alsj/ap-geotrips.pdf).] 1963 16-18 January 1963: Meteor Crater and San Francisco Volcanic Field near Flagstaff, Arizona (9 astronauts). Among the nine astronaut trainees in Flagstaff for that initial astronaut geologic training exercise was Neil Armstrong--who would become the first man to step foot on the Moon during the historic Apollo 11 mission in July 1969! The other astronauts present included Frank Borman (Apollo 8), Charles "Pete" Conrad (Apollo 12), James Lovell (Apollo 8 and the near-tragic Apollo 13), James McDivitt, Elliot See (killed later in a plane crash), Thomas Stafford (Apollo 10), Edward White (later killed in the tragic Apollo 1 fire at Cape Canaveral), and John Young (Apollo 16). -
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. -
Evidence for Impact-Generated Deposition
EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS (Under the direction of Michael F. Roden) ABSTRACT Modeling demonstrates that the Late Eocene Chesapeake Bay impact would have been capable of depositing ejecta in east-central Georgia with thicknesses exceeding thirty centimeters. A coarse sand layer at the base of the Upper Eocene Dry Branch Formation was examined for shocked minerals. Universal stage measurements demonstrate that planar fabrics in some fine to medium sand-size quartz grains are parallel to planes commonly exploited by planar deformation features (PDF’s) in shocked quartz. Possible PDF’s are observed parallel to {10-13}, {10-11}, {10-12}, {11-22} and {51-61}. Petrographic identification of shocked quartz is supported by line broadening in X-ray diffraction experiments. Other impact ejecta recognized include possible ballen quartz, maskelynite, and reidite-bearing zircon grains. The layer is correlative with an unusual diamictite that contains goethite spherules similar to altered microkrystites. It may represent an impact-generated debris flow. These discoveries suggest that the Chesapeake Bay impact horizon is preserved in Georgia. The horizon also should be the source stratum for Georgia tektites. INDEX WORDS: Chesapeake Bay impact, Upper Eocene, Shocked quartz, Impact shock, Shocked zircon, Impact, Impact ejecta, North American tektites, Tektites, Georgiaites, Georgia Tektites, Planar deformation features, PDF’s, Georgia, Geology, Coastal Plain, Stratigraphy, Impact stratigraphy, Impact spherules, Goethite spherules, Diamictite, Twiggs Clay, Dry Branch Formation, Clinchfield Sand, Irwinton Sand, Reidite, Microkrystite, Cpx Spherules, Impact debris flow EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS B. -
Astrobiology and the Search for Life Beyond Earth in the Next Decade
Astrobiology and the Search for Life Beyond Earth in the Next Decade Statement of Dr. Andrew Siemion Berkeley SETI Research Center, University of California, Berkeley ASTRON − Netherlands Institute for Radio Astronomy, Dwingeloo, Netherlands Radboud University, Nijmegen, Netherlands to the Committee on Science, Space and Technology United States House of Representatives 114th United States Congress September 29, 2015 Chairman Smith, Ranking Member Johnson and Members of the Committee, thank you for the opportunity to testify today. Overview Nearly 14 billion years ago, our universe was born from a swirling quantum soup, in a spectacular and dynamic event known as the \big bang." After several hundred million years, the first stars lit up the cosmos, and many hundreds of millions of years later, the remnants of countless stellar explosions coalesced into the first planetary systems. Somehow, through a process still not understood, the laws of physics guiding the unfolding of our universe gave rise to self-replicating organisms − life. Yet more perplexing, this life eventually evolved a capacity to know its universe, to study it, and to question its own existence. Did this happen many times? If it did, how? If it didn't, why? SETI (Search for ExtraTerrestrial Intelligence) experiments seek to determine the dis- tribution of advanced life in the universe through detecting the presence of technology, usually by searching for electromagnetic emission from communication technology, but also by searching for evidence of large scale energy usage or interstellar propulsion. Technology is thus used as a proxy for intelligence − if an advanced technology exists, so to does the ad- vanced life that created it. -
Livre-Ovni.Pdf
UN MONDE BIZARRE Le livre des étranges Objets Volants Non Identifiés Chapitre 1 Paranormal Le paranormal est un terme utilisé pour qualifier un en- mé n'est pas considéré comme paranormal par les semble de phénomènes dont les causes ou mécanismes neuroscientifiques) ; ne sont apparemment pas explicables par des lois scien- tifiques établies. Le préfixe « para » désignant quelque • Les différents moyens de communication avec les chose qui est à côté de la norme, la norme étant ici le morts : naturels (médiumnité, nécromancie) ou ar- consensus scientifique d'une époque. Un phénomène est tificiels (la transcommunication instrumentale telle qualifié de paranormal lorsqu'il ne semble pas pouvoir que les voix électroniques); être expliqué par les lois naturelles connues, laissant ain- si le champ libre à de nouvelles recherches empiriques, à • Les apparitions de l'au-delà (fantômes, revenants, des interprétations, à des suppositions et à l'imaginaire. ectoplasmes, poltergeists, etc.) ; Les initiateurs de la parapsychologie se sont donné comme objectif d'étudier d'une manière scientifique • la cryptozoologie (qui étudie l'existence d'espèce in- ce qu'ils considèrent comme des perceptions extra- connues) : classification assez injuste, car l'objet de sensorielles et de la psychokinèse. Malgré l'existence de la cryptozoologie est moins de cultiver les mythes laboratoires de parapsychologie dans certaines universi- que de chercher s’il y a ou non une espèce animale tés, notamment en Grande-Bretagne, le paranormal est inconnue réelle derrière une légende ; généralement considéré comme un sujet d'étude peu sé- rieux. Il est en revanche parfois associé a des activités • Le phénomène ovni et ses dérivés (cercle de culture). -
CASKAR: a CASPER Concept for the SKA Phase 1 Signal Processing Sub-System
CASKAR: A CASPER concept for the SKA phase 1 Signal Processing Sub-system Francois Kapp, SKA SA Outline • Background • Technical – Architecture – Power • Cost • Schedule • Challenges/Risks • Conclusions Background CASPER Technology MeerKAT Who is CASPER? • Berkeley Wireless Research Center • Nancay Observatory • UC Berkeley Radio Astronomy Lab • Oxford University Astrophysics • UC Berkeley Space Sciences Lab • Metsähovi Radio Observatory, Helsinki University of • Karoo Array Telescope / SKA - SA Technology • NRAO - Green Bank • New Jersey Institute of Technology • NRAO - Socorro • West Virginia University Department of Physics • Allen Telescope Array • University of Iowa Department of Astronomy and • MIT Haystack Observatory Physics • Harvard-Smithsonian Center for Astrophysics • Ohio State University Electroscience Lab • Caltech • Hong Kong University Department of Electrical and Electronic Engineering • Cornell University • Hartebeesthoek Radio Astronomy Observatory • NAIC - Arecibo Observatory • INAF - Istituto di Radioastronomia, Northern Cross • UC Berkeley - Leuschner Observatory Radiotelescope • Giant Metrewave Radio Telescope • University of Manchester, Jodrell Bank Centre for • Institute of Astronomy and Astrophysics, Academia Sinica Astrophysics • National Astronomical Observatories, Chinese Academy of • Submillimeter Array Sciences • NRAO - Tucson / University of Arizona Department of • CSIRO - Australia Telescope National Facility Astronomy • Parkes Observatory • Center for Astrophysics and Supercomputing, Swinburne University -
James A. Mccloskey, Jr
CHEMICAL HERITAGE FOUNDATION JAMES A. MCCLOSKEY, JR. Transcript of Interviews Conducted by Michael A. Grayson at the McCloskeys’ Home Helotes, Texas on 19 and 20 March 2012 (With Subsequent Corrections and Additions) James A. McCloskey, Jr. ACKNOWLEDGMENT This oral history is one in a series initiated by the Chemical Heritage Foundation on behalf of the American Society for Mass Spectrometry. The series documents the personal perspectives of individuals related to the advancement of mass spectrometric instrumentation, and records the human dimensions of the growth of mass spectrometry in academic, industrial, and governmental laboratories during the twentieth century. This project is made possible through the generous support of the American Society for Mass Spectrometry. This oral history is designated Free Access. Please note: Users citing this interview for purposes of publication are obliged under the terms of the Chemical Heritage Foundation (CHF) Center for Oral History to credit CHF using the format below: James A. McCloskey, Jr., interview by Michael A. Grayson at the McCloskeys’ home, Helotes, Texas, 19-20 March 2012 (Philadelphia: Chemical Heritage Foundation, Oral History Transcript # 0702). Chemical Heritage Foundation Center for Oral History 315 Chestnut Street Philadelphia, Pennsylvania 19106 The Chemical Heritage Foundation (CHF) serves the community of the chemical and molecular sciences, and the wider public, by treasuring the past, educating the present, and inspiring the future. CHF maintains a world-class collection of materials that document the history and heritage of the chemical and molecular sciences, technologies, and industries; encourages research in CHF collections; and carries out a program of outreach and interpretation in order to advance an understanding of the role of the chemical and molecular sciences, technologies, and industries in shaping society. -
Exep Science Plan Appendix (SPA) (This Document)
ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 1 of 61 Created By: David A. Breda Date Program TDEM System Engineer Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Nick Siegler Date Program Chief Technologist Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Concurred By: Dr. Gary Blackwood Date Program Manager Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology EXOPDr.LANET Douglas Hudgins E XPLORATION PROGRAMDate Program Scientist Exoplanet Exploration Program ScienceScience Plan Mission DirectorateAppendix NASA Headquarters Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#19-0790 JPL Document No: 1735632 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 2 of 61 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters Created by: Dr. Karl Stapelfeldt Chief Program Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Eric Mamajek Deputy Program Chief Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. © 2018 California Institute of Technology. Government sponsorship acknowledged. Exoplanet Exploration Program JPL CL#19-0790 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 3 of 61 Table of Contents 1. -
WATER – Overview
WATER – Overview Contents Introduction ............................1 Module Matrix ........................2 FOSS Conceptual Framework...4 Background for the Conceptual Framework in Water ................6 FOSS Components ................ 16 FOSS Instructional Design ..... 18 FOSSweb and Technology ...... 26 Universal Design for Learning ................................ 30 Working in Collaborative INTRODUCTION Groups .................................. 32 Safety in the Classroom Water is the most important substance on Earth. Water dominates and Outdoors ........................ 34 the surface of our planet, changes the face of the land, and defi nes life. These powerful pervasive ideas are introduced here. The Scheduling the Module .......... 35 Water Module provides students with experiences to explore the FOSS K–8 Scope properties of water, changes in water, interactions between water and Sequence ....................... 36 and other earth materials, and how humans use water as a natural resource. In this module, students will • Conduct surface-tension experiments. • Observe and explain the interaction between masses of water at diff erent temperatures and masses of water in liquid and solid states. • Construct a thermometer to observe that water expands as it warms and contracts as it cools. • Investigate the eff ect of surface area and air temperature on evaporation, and the eff ect of temperature on condensation. • Investigate what happens when water is poured through two earth materials—soil and gravel. • Design and construct a waterwheel and use it to lift or pull objects. • Use fi eld techniques to compare how well several soils drain. © Copyright The Regents of the University California. Not for resale, redistribution, or use other than classroom without further permission. www.fossweb.com Full Option Science System 1 WATER – Overview Module Summary Focus Questions Students investigate properties of water.