Returning Samples from Enceladus for Life Detection
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Dustin M. Schroeder
Dustin M. Schroeder Assistant Professor of Geophysics Department of Geophysics, School of Earth, Energy, and Environmental Sciences 397 Panama Mall, Mitchell Building 361, Stanford University, Stanford, CA 94305 [email protected], 440.567.8343 EDUCATION 2014 Jackson School of Geosciences, University of Texas, Austin, TX Doctor of Philosophy (Ph.D.) in Geophysics 2007 Bucknell University, Lewisburg, PA Bachelor of Science in Electrical Engineering (B.S.E.E.), departmental honors, magna cum laude Bachelor of Arts (B.A.) in Physics, magna cum laude, minors in Mathematics and Philosophy PROFESSIONAL EXPERIENCE 2016 – present Assistant Professor of Geophysics, Stanford University 2017 – present Assistant Professor (by courtesy) of Electrical Engineering, Stanford University 2020 – present Center Fellow (by courtesy), Stanford Woods Institute for the Environment 2020 – present Faculty Affiliate, Stanford Institute for Human-Centered Artificial Intelligence 2021 – present Senior Member, Kavli Institute for Particle Astrophysics and Cosmology 2016 – 2020 Faculty Affiliate, Stanford Woods Institute for the Environment 2014 – 2016 Radar Systems Engineer, Jet Propulsion Laboratory, California Institute of Technology 2012 Graduate Researcher, Applied Physics Laboratory, Johns Hopkins University 2008 – 2014 Graduate Researcher, University of Texas Institute for Geophysics 2007 – 2008 Platform Hardware Engineer, Freescale Semiconductor SELECTED AWARDS 2021 Symposium Prize Paper Award, IEEE Geoscience and Remote Sensing Society 2020 Excellence in Teaching Award, Stanford School of Earth, Energy, and Environmental Sciences 2019 Senior Member, Institute of Electrical and Electronics Engineers 2018 CAREER Award, National Science Foundation 2018 LInC Fellow, Woods Institute, Stanford University 2016 Frederick E. Terman Fellow, Stanford University 2015 JPL Team Award, Europa Mission Instrument Proposal 2014 Best Graduate Student Paper, Jackson School of Geosciences 2014 National Science Olympiad Heart of Gold Award for Service to Science Education 2013 Best Ph.D. -
From Hayabusa to Hayabusa2: Present Status and Plans for Sample Curations of Asteroidal Sample Return Missions by Jaxa
81st Annual Meeting of The Meteoritical Society 2018 (LPI Contrib. No. 2067) 6117.pdf FROM HAYABUSA TO HAYABUSA2: PRESENT STATUS AND PLANS FOR SAMPLE CURATIONS OF ASTEROIDAL SAMPLE RETURN MISSIONS BY JAXA. T. Yada1, K. Sakamoto1, M. Yoshitake1, K. Kumagai2, M. Nishimura2, Y. Nakano1, S. Furuya1, M. Abe1, T. Okada1, S. Tachibana3, H. Yurimoto1,4, and M. Fujimoto1,5, 1Astromat. Sci. Res. Group, Inst. Space Astronaut. Sci., Japan Aerosp. Explor. Agnecy, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan ([email protected]), 2 Marine Works Japan Ltd., 3-54-1 Oppamahigashi, Yokosuka 237-0063 Japan, 3Dept. Earth Planet. Sci., Grad. Sch. Science, Univ. Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan, 4Dept. Earth Science, Grad. Sch. Science, Hokkaido Univ., Kita 8, Nishi 5, Kita, Sapporo, Hokkaido 060-0808, Japan, 5Earth-Life Sci. Inst., Tokyo Inst. Tech., 2-12-1-1E-1 Ookayama, Meguro, Tokyo 152-8550, Japan. Introduction: The new era of sample return missions had started since the Stardust returned samples from com- et 81P/Wild 2 in 2006 [1], followed by the Hayabusa spacecraft from the near-Earth S-type asteroid 25143 Itokawa in 2010 [2,3]. In this year, Hayabusa2 will reach its target body, the near-Earth C-type asteroid 162173 Ryugu [4], and also OSIRIS-REx toward the near-Earth B-type asteroid 101955 Bennu [5]. Additionally, several other sample return missions have been planned recently, such as the Martian Moons eXplorer (MMX) for the Phobos and/or Deimos [6], the CAESAR for 67P/Churyumov-Gerasimenko [7], and the HELACLES for the the Moon [8]. -
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7'tie;T;e ~;&H ~ t,#t1tMftllSieotOg, UCLA VOLUME 3 1986 EDITORIAL BOARD Mark E. Forry Anne Rasmussen Daniel Atesh Sonneborn Jane Sugarman Elizabeth Tolbert The Pacific Review of Ethnomusicology is an annual publication of the UCLA Ethnomusicology Students Association and is funded in part by the UCLA Graduate Student Association. Single issues are available for $6.00 (individuals) or $8.00 (institutions). Please address correspondence to: Pacific Review of Ethnomusicology Department of Music Schoenberg Hall University of California Los Angeles, CA 90024 USA Standing orders and agencies receive a 20% discount. Subscribers residing outside the U.S.A., Canada, and Mexico, please add $2.00 per order. Orders are payable in US dollars. Copyright © 1986 by the Regents of the University of California VOLUME 3 1986 CONTENTS Articles Ethnomusicologists Vis-a-Vis the Fallacies of Contemporary Musical Life ........................................ Stephen Blum 1 Responses to Blum................. ....................................... 20 The Construction, Technique, and Image of the Central Javanese Rebab in Relation to its Role in the Gamelan ... ................... Colin Quigley 42 Research Models in Ethnomusicology Applied to the RadifPhenomenon in Iranian Classical Music........................ Hafez Modir 63 New Theory for Traditional Music in Banyumas, West Central Java ......... R. Anderson Sutton 79 An Ethnomusicological Index to The New Grove Dictionary of Music and Musicians, Part Two ............ Kenneth Culley 102 Review Irene V. Jackson. More Than Drumming: Essays on African and Afro-Latin American Music and Musicians ....................... Norman Weinstein 126 Briefly Noted Echology ..................................................................... 129 Contributors to this Issue From the Editors The third issue of the Pacific Review of Ethnomusicology continues the tradition of representing the diversity inherent in our field. -
CAROL PATY [email protected] 1 Associate Professor Robert D. Clark
CAROL PATY [email protected] Associate Professor Robert D. Clark Honors College & Department of Earth Sciences 1293 University of Oregon Eugene, OR 97403-1293 Educational Background: B.A. Physics & Astronomy 2001 Bryn Mawr College Ph.D. Earth & Space Sciences 2006 University of Washington (Advisor: R. Winglee) Employment History: Undergraduate Teaching Assistant, Bryn Mawr College, Physics 1998-2001 Graduate Teaching Assistant, University of Washington, Earth & Space Sciences 2002-2005 Graduate Research Assistant, University of Washington, Earth & Space Sciences 2001-2006 Instructor, Chautauqua Course on Space Weather & Planetary Magnetospheres 2006 (Summer) Postdoctoral Researcher, Southwest Research Institute, Space Science & Engineering 2006-2008 Assistant Professor, Georgia Institute of Technology, Earth & Atmospheric Science 2008-2014 Associate Professor, Georgia Institute of Technology, Earth & Atmospheric Science 2014-2018 Associate Professor, University of Oregon, Clark Honors College & Earth Sciences 2018-present Current Research Interests: Space Plasma Physics, Planetary Magnetospheres, Planetary Upper Atmospheres/Ionospheres, Icy Satellites, Dusty Plasmas, Mars Atmospheric Evolution, Astrobiology, Mission Planning Activities (Cassini, Jupiter Icy Moon Explorer: JUICE, Europa Clipper Mission, Trident, Odyssey PMCS) Synergistic Activities: National Academy of Sciences – Ocean Worlds and Dwarf Planets Panel for the ‘Planetary Science and Astrobiology Decadal Survey 2023-2032’ October 2020 – present Icarus Editor 2017-present Outer -
Mars Pathfinder
NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mars Pathfinder Mars Pathfinder was the first completed mission events, ending in a touchdown which left all systems in NASAs Discovery Program of low-cost, rapidly intact. developed planetary missions with highly focused sci- The landing site, an ancient flood plain in Mars ence goals. With a development time of only three northern hemisphere known as Ares Vallis, is among years and a total cost of $265 million, Pathfinder was the rockiest parts of Mars. It was chosen because sci- originally designed entists believed it to as a technology be a relatively safe demonstration of a surface to land on way to deliver an and one which con- instrumented lander tained a wide vari- and a free-ranging ety of rocks robotic rover to the deposited during a surface of the red catastrophic flood. planet. Pathfinder In the event early in not only accom- Mars history, sci- plished this goal but entists believe that also returned an the flood plain was unprecedented cut by a volume of amount of data and water the size of outlived its primary North Americas design life. Great Lakes in Pathfinder used about two weeks. an innovative The lander, for- method of directly mally named the entering the Carl Sagan Martian atmos- Memorial Station phere, assisted by a following its suc- parachute to slow cessful touchdown, its descent through and the rover, the thin Martian atmosphere and a giant system of named Sojourner after American civil rights crusader airbags to cushion the impact. -
The Strength of Regolith and Rubble Pile Asteroids Arxiv:1306.1622V2 [Astro-Ph.EP] 5 Mar 2014
The Strength of Regolith and Rubble Pile Asteroids∗ P. S´anchez and D.J. Scheeres The University of Colorado at Boulder Abstract We explore the hypothesis that, due to small van der Waals forces between constituent grains, small rubble pile asteroids have a small but non-zero cohesive strength. The nature of this model predicts that the cohesive strength should be constant independent of aster- oid size, which creates a scale dependence with relative strength in- creasing as size decreases. This model counters classical theory that rubble pile asteroids should behave as scale-independent cohesionless collections of rocks. We explore a simple model for asteroid strength that is based on these weak forces, validate it through granular me- chanics simulations and comparisons with properties of lunar regolith, and then explore its implications and ability to explain and predict observed properties of small asteroids in the NEA and Main Belt pop- ulations, and in particular of asteroid 2008 TC3. One conclusion is that the population of rapidly rotating asteroids could consist of both distributions of smaller grains (i.e., rubble piles) and of monolithic boulders. arXiv:1306.1622v2 [astro-ph.EP] 5 Mar 2014 1 Introduction The strength and morphology of small asteroids in the solar system remains an open and fundamentally interesting scientific issue. The strength of a rubble pile body will control how fast it can rotate before shedding mass or disrupting, influence the process by which binary asteroids are created, and ∗Accepted in Meteoritics and Planetary Science, 2/2014. 1 could have significance for the mitigation of hazardous near-Earth asteroids (NEA) should this be necessary in the future. -
Planetary Science Update
Planetary Science Division Status Report Jim Green NASA, Planetary Science Division October 11, 2017 Presentation at LEAG Planetary Science Missions Events 2016 March – Launch of ESA’s ExoMars Trace Gas Orbiter July 4 – Juno inserted in Jupiter orbit * Completed September 8 – Launch of Asteroid mission OSIRIS – REx to asteroid Bennu September 30 – Landing Rosetta on comet CG October 19 – ExoMars EDM landing and TGO orbit insertion 2017 January 4 – Discovery Mission selection announced February 9-20 - OSIRIS-REx began Earth-Trojan search April 22 – Cassini begins plane change maneuver for the “Grand Finale” August 22 – Solar Eclipse across America September 15 – Cassini end of mission at Saturn September 22 – OSIRIS-REx Earth flyby October 28 – International Observe the Moon night (1st quarter) 2018 May 5 - Launch InSight mission to Mars August – OSIRIS-REx arrival at Bennu October – Launch of ESA’s BepiColombo to Mercury November 26 – InSight landing on Mars 2019 January 1 – New Horizons flyby of Kuiper Belt object 2014MU69 Formulation Implementation Primary Ops BepiColombo Lunar Extended Ops (ESA) Reconnaissance Orbiter Lucy New Horizons Psyche Juno Dawn JUICE (ESA) ExoMars 2016 MMX MAVEN MRO (ESA) (JAXA) Mars Express Mars (ESA) Odyssey OSIRIS-REx ExoMars 2020 (ESA) Mars Rover Opportunity Curiosity InSight 2020 Rover Rover NEOWISE Europa Clipper Discovery Program Discovery Program NEO characteristics: Mars evolution: Lunar formation: Nature of dust/coma: Solar wind sampling: NEAR (1996-1999) Mars Pathfinder (1996-1997) Lunar Prospector -
The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 18 - Fall 1991 © 1991, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific "Having finally penetrated below the clouds of Venus, we find its surface to be naked [not hidden], revealing the history of hundreds of millions of years of geological activity. Venus is a geologist's dream planet.'' —Astronomer David Morrison This fall, the brightest star-like object you can see in the eastern skies before dawn isn't a star at all — it's Venus, the second closest planet to the Sun. Because Venus is so similar in diameter and mass to our world, and also has a gaseous atmosphere, it has been called the Earth's "sister planet''. Many years ago, scientists expected its surface, which is perpetually hidden beneath a thick cloud layer, to look like Earth's as well. Earlier this century, some people even imagined that Venus was a hot, humid, swampy world populated by prehistoric creatures! But we now know Venus is very, very different. New radar images of Venus, just returned from NASA's Magellan spacecraft orbiting the planet, have provided astronomers the clearest view ever of its surface, revealing unique geological features, meteor impact craters, and evidence of volcanic eruptions different from any others found in the solar system. This issue of The Universe in the Classroom is devoted to what Magellan is teaching us today about our nearest neighbor, Venus. Where is Venus, and what is it like? Spacecraft exploration of Venus's surface Magellan — a "recycled'' spacecraft How does Magellan take pictures through the clouds? What has Magellan revealed about Venus? How does Venus' surface compare with Earth's? What is the next step in Magellan's mission? If Venus is such an uninviting place, why are we interested in it? Reading List Why is it so hot on Venus? Where is Venus, and what is it like? Venus orbits the Sun in a nearly circular path between Mercury and the Earth, about 3/4 as far from our star as the Earth is. -
Krista Marie Soderlund the University of Texas at Austin Institute for Geophysics, John A
Krista Marie Soderlund The University of Texas at Austin Institute for Geophysics, John A. & Katherine G. Jackson School of Geosciences J.J. Pickle Research Campus, Bldg. 196 (ROC), 10100 Burnet Rd. (R2200), Austin, TX 78758-4445 [email protected], Office: 512-471-0449, Cell: 218-349-3006, FAX: 512-471-8844 Research Interests Geophysical Fluid Dynamics, Magnetohydrodynamics, Planetary Science, Cryosphere Education University of California, Los Angeles Ph.D., Geophysics and Space Physics, 2011 M.S., Geophysics and Space Physics, 2009 Florida Institute of Technology B.S., Double major in Physics & Space Science, 2005, Summa Cum Laude Employment University of Texas at Austin, Institute for Geophysics Research Associate, September 2014-Present UTIG Postdoctoral Fellow, October 2011-September 2014 University of California, Los Angeles, Department of Earth and Space Sciences Graduate Student Researcher, Advisor: Dr. Jonathan M. Aurnou, 2006-2011 California Institute of Technology, Division of Geological and Planetary Sciences Summer Undergraduate Research Fellow, Dr. Joann M. Stock, 2005 NASA Jet Propulsion Laboratory, CA Consultant, Dr. Bonnie J. Buratti, 2006 Planetary Geology & Geophysics Undergrad Research Program, Dr. B.J. Buratti, 2004 Florida Institute of Technology, Department of Physics and Space Science Undergraduate Researcher, Dr. Niescja E. Turner, 2004-2005 Naval Oceanographic Office, Hydrology Code, Stennis Space Center, MS Physical science aid, 2003 Mission Experience Saturn Probe Interior and aTmosphere Explorer (SPRITE) -
Strategic Investments in Instrumentation and Facilities for Extraterrestrial Sample Curation and Analysis
PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION Strategic Investments in Instrumentation and Facilities for Extraterrestrial Sample Curation and Analysis ADVANCE COPY NOT FOR PUBLIC RELEASE BEFORE Thursday, December 20, 2018 at 11:00 a.m. ___________________________________________________________________________________ PLEASE CITE AS A REPORT OF THE NATIONAL ACADEMIES OF SCIENCES, ENGINEERING, AND MEDICINE Committee on Extraterrestrial Sample Analysis Facilities Space Studies Board Division on Engineering and Physical Sciences A Consensus Study Report of PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION THE NATIONAL ACADEMIES PRESS 500 Fifth Street, NW Washington, DC 20001 This activity was supported by Grant/Contract No. XXXX with XXXXX. Any opinions, findings, conclusions, or recommendations expressed in this publication do not necessarily reflect the views of any organization or agency that provided support for the project. International Standard Book Number-13: 978-0-309-XXXXX-X International Standard Book Number-10: 0-309-XXXXX-X Digital Object Identifier: https://doi.org/10.17226/25312 Additional copies of this publication are available for sale from the National Academies Press, 500 Fifth Street, NW, Keck 360, Washington, DC 20001; (800) 624-6242 or (202) 334-3313; http://www.nap.edu. Copyright 2018 by the National Academy of Sciences. All rights reserved. Printed in the United States of America Suggested citation: National Academies of Sciences, Engineering, and Medicine. 2018. Strategic Investments in Instrumentation and Facilities for Extraterrestrial Sample Curation and Analysis. Washington, DC: The National Academies Press. https://doi.org/10.17226/25312. PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION The National Academy of Sciences was established in 1863 by an Act of Congress, signed by President Lincoln, as a private, nongovernmental institution to advise the nation on issues related to science and technology. -
The Comet Astrobiology Exploration Sample Return (CAESAR)
Project Overview Michael Amato NASA GSFC CAESAR Project and GSFC, Cornell, and other partner proprietary and copyright Information CAESAR The CAESAR (Comet Astrobiology Exploration SAmple Return) mission is one of two New Frontiers missions selected for Phase A. CAESAR will acquire a sample from the nucleus of comet Churyumov-Gerasimenko, returning it safely to Earth. Comets are made up of materials from ancient stars, interstellar clouds, and the birth of our solar system. The CAESAR sample will reveal how these materials contributed to the early Earth, including the origins of the Earth's oceans, and of life The CAESAR mission seeks to return this sample from 67P/Churyumov-Gerasimenko, a comet that was successfully explored by the European Space Agency’s Rosetta spacecraft, to determine its origin and history. • PI Steve Squyres of Cornell University • CAESAR would be managed by NASA’s Goddard Space Flight Center CAESAR Project and GSFC, Cornell, and other partner proprietary and copyright Information CAESAR Sample Science CAESAR Project and GSFC, Cornell, and other partner proprietary and copyright Information Churyumov-Gerasimenko CAESAR Project and GSFC, Cornell, and other partner proprietary and copyright Information The CAESAR Spacecraft GSFC Restore-L EDU arm NEXT-C Ion Thruster CAESAR Project and GSFC, Cornell, and other partner proprietary and copyright Information Mission Timeline 2024 2026 2028 2030 2032 2034 2036 2038 Comet Ops SEP Cruise to 67P SEP Return to Earth Launch August 2024 Launch Arrive at Comet March 2029 Depart -
Bare-Tether Missions Paradigm for Exploration of Oceanworlds in Plumes of Icy Moons Enceladus, Europa, and Triton
Bare-Tether Missions Paradigm for Exploration of OceanWorlds in Plumes of Icy Moons Enceladus, Europa, and Triton Juan R. Sanmartin 34 + 910675922 Universidad Politécnica de Madrid / Emerito Real Academia de Ingeniería [email protected] I.- Introduction The case of Ice Giants, which only received flyby missions, is of particular interest as regards exploration. There are multiple issues of interest in exploring Uranus and Neptune as different from Gas Giants: Composition is definitely different; rocky mass-percent is much larger; both planetary dynamics and magnetic structures present striking differences (quite relevant for tether interaction); exoplanet statistics suggests Ice types are well more abundant than Gas types. This raises questions about exomoons and exomagnetics… As regards considering tethers for a Neptune mission, beyond just a flyby, there would seem to exist a basic problem with standard methods. The Introduction section of NASA’s “Ice Giants” Pre-Decadal Mission Study Report, JPL D-100520, June 2017 (529 pp), in Sec.2.3.3, recalls the multiple studies, over the last half-century, on mission design options for exploration of Uranus and Neptune, ranging from just chemical propulsion to electric propulsion, both with and without gravity assists, and a variety of mission architectural concepts. First, such faraway missions appear quite costly. In the Report the estimated cost of a Flagship Neptune mission was $1.972B, $300M less for Uranus, whereas total budget for both planets was $2B. Secondly, available solar power is practically nil in a large part of the trip, spacecraft capture by chemical propulsion leading to high wet-mass, with scientific load limited to a small mass fraction, and orbital maneuvers quite reduced after capture.