DOCSLIB.ORG

Report 2017 Research, Education and Public Outreach Annual Report 2017 Research, Education and Public Outreach

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Report 2017 Research, Education and Public Outreach Annual Report 2017 Research, Education and Public Outreach Annual Report 2017 Research, Education and Public Outreach Annual Report 2017 Research, Education and Public Outreach Nathalie A. Cabrol Director, Carl Sagan Center, Pamela Harman, Acting Director, Center for Education Rebecca Mcdonald Director, Center for Outreach Bill Diamond President & CEO The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach TABLE OF CONTENTS Peer-reviewed publications 10 Conferences: Abstracts & Proceedings 18 Technical Reports & Data Releases 29 Outreach, Media Coverage, Web Stories & Interviews 31 Invited Talks (Professional & Public) 39 Highlights, Significant Events & Activities 46 Fieldwork 52 Honors & Awards 54 Missions, Observations & Strategic Planning 56 Acknowledgements 60 The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach FROM THE SETI INSTITUTE President and CEO Dear friends, The scientists, educators and outreach professionals of the SETI Institute had yet another banner year of productivity in 2017. We are delighted to present our 2nd annual report, cataloging the research and education programs of the Institute, as well as the myriad of mainstream media stories about our people and our work. Among the highlights from this year’s report are 147 peer-reviewed articles in scientific journals, 225 conference proceedings and abstracts, 172 media stories and interviews, and 177 invited talks. The report also highlights 16 of our researchers and educators who were honored with more than twenty different committee chair positions, fellowships and NASA achievement awards for their extraordinary work. Honors and recognitions included: • Edna DeVore was selected as a fellow of the American Association for the Advance- ment of Science • Doug Caldwell was cited among the “World’s Most Impactful Researchers” by Clari- vate Analytics • Fergal Mullally received the NASA 2017 Exceptional Public Achievement Medal for revolutionary Kepler Object of Interest Vetting. • Mark Showalter received a NASA Group Achievement Award, granted to the New Horizons team • Margaret Race was appointed Senior Scientific Editor of the Astrobiology Journal • Driss Takir received a NASA Silver Achievement Medal for contributions to the char- acterization of asteroid Bennu with the OSIRIS-Rex team In addition, The SETI Institute was recognized as a “Top 100 NASA Contractor” for 2016 and we received the Alliance Award from the Girl Scouts of Northern California in The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach recognition of outstanding support. Lastly, Mark Showalter, Edna DeVore and Seth Shostak were named as the first Fellows of the Institute. We’ve added new sections to this year’s report highlighting our contributions to planned and ongoing NASA missions, submission of mission planning concepts, participation on official committees and working groups, and time allocations on major observational platforms, including Arecibo, Greenbank, the Very Large Array (VLA), the Spitzer Space Telescope, SOFIA, Hubble and more. Sharing our work with the public is a core element of our mission as a world-class research institution. I encourage you to peruse the following pages and get better acquainted with our amazing team and the compelling and impactful work they do. Sincerely, Bill Diamond President and CEO February 20, 2018 The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach CARL SAGAN CENTER for the study of life in the universe Taking Flight! This year was a very successful year for the Carl Sagan Center (CSC), and this impres- sive report is a reflection of your commitment to excellence: We are publishing in high profile journals; we are recognized leaders in our fields, and our work is being acknowl- edged regularly by our peers through prestigious honors and awards. We also share our passion of exploration and discovery with the public, and I am always amazed to see how the number of our public lectures often times surpass our professional presentations. That speaks volume about dedication. You are the best advocates of the Institute, and in a world where education is facing so many challenges, you are the voice of science and the keepers of the flame for the next generation. This year also marked Cassini’s Grand Finale. Many of you were involved with this prestigious mission, For all of us, the day Cassini plunged into Saturn’s atmosphere was bittersweet. However, as one mission ends, new ones are being readied (e.g., JWST, TESS, Mars 2020, ExoMars, and others), and the SETI Institute is already present at various levels in these missions, and will be directly involved with these exciting new chapters of exploration. When it comes to the inner workings of the CSC, this year brought a real improvement in our proposal success rate. During the retreat at Asilomar, I shared with you my con- cerns about the 2016 numbers, and together, we took a hard look at what could be im- proved. The Science Council took charge and went through a deep review and some soul searching to understand how to be more successful. As a result, there is now a process to help you with grant writing and proposal submission, and we will make sure to provide you all the support we can to keep the momentum going. Meanwhile, you took charge too. I was delighted to see how you started to communicate with each other, review each other’s proposals whenever possible, asked for advice and for collaboration, and sometimes for instruments as well, within the SETI Institute The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach community. This is really what it is all about: team work. Yes, we do sometimes compete against each other for the same grant money, and will continue to do so; but we are also learning to work together whenever possible, and in doing so, we are becoming stronger. The success of one is the success of all, and this is starting to pay dividend, literally. Since the retreat, we have received now over two third of the results for the 2017 proposal season. At this point in time, our success rate is above national average by a good margin. It is an average over all programs, and success is program-depen- dent. There are still areas that will require serious work but, overall, 2017 is turning out to be a very successful year, and you should be extremely proud of this. Your engagement in the process is key to this success. It will be even more important in the coming months, as we are de- fining the strategic vision for the years to come, creating new opportunities for us all through new collaborations, and new ways of doing business. Your engagement with your Research Group Chairs and the Science Council will be key. Remem- ber, this is your Institute, and by being involved, you are making your voice heard, and help shape your own future. While I am here to steer and suggest, I am also – and more importantly – here to listen and help, and to implement your ideas to the best of my abilities. As I always say: My door is always open, and I am also only one email away. Indeed, there is a lot to be proud of this year, and we will celebrate all these successes together. While there is always prog- ress to be made, I certainly can say that this year saw us all starting to think as a unit, and working more with, and for, each other. Embarking on that path was critical, and you are making it happen. I would like to end this letter by thanking all of those who are working behind the scene to make it all happen every single day in all departments of the Institute. Thank you! Nathalie A. Cabrol Director, SETI Institute Carl Sagan Center January 19, 2018 The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach CENTER FOR EDUCATION The 2017 Activity Report, a copious compendium of events and publications, is just the tip of the iceberg of the undertakings and efforts of the SETI Institute in the name of education and public engagement. Our day to day efforts, and incremental milestones are a significant part of our 2017 report. The Center for Education pillar programs, NASA Airborne Astronomy Ambassadors (AAA) and Reaching for the Stars: NASA Science for Girl Scouts progressed through the kick-off, professional development, flight week experiences, and evaluation of the Cycle 6 AAA; and rounds of testing and revising Girl Scout Space Science Badges, as well as holding astronomy camps. Unique in 2017, Girl Scout Destination Camps on the path of eclipse totality, and Girl Scout Eclipse Boxes & Activity Guides were successful due to great collaboration with our Co-Investigators. We were fortunate to have the REU and FDL programs on site, and look forward to the energy those programs bring to us. I offer my sincere gratitude to my Institute colleagues that embraced communication and collaboration across centers, that mentor students and life-long learners, that give public talks and that visit classrooms and libraries. Pamela Harman Acting Director, SETI Institute Center for Education The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Annual Report 2017 Research, Education and Public Outreach CENTER FOR OUTREACH 2017 was an amazing year in so many ways. At the SETI Institute, our more than 75 sci- entists and researchers have continued to advance the SETI Institute’s mission to explore, understand and explain the origin and nature of life in the universe, and the evolution of intelligence.
Load more

Recommended publications
  • Railway Employee Records for Colorado Volume Iii
    RAILWAY EMPLOYEE RECORDS FOR COLORADO VOLUME III By Gerald E. Sherard (2005) When Denver’s Union Station opened in 1881, it saw 88 trains a day during its gold-rush peak. When passenger trains were a popular way to travel, Union Station regularly saw sixty to eighty daily arrivals and departures and as many as a million passengers a year. Many freight trains also passed through the area. In the early 1900s, there were 2.25 million railroad workers in America. After World War II the popularity and frequency of train travel began to wane. The first railroad line to be completed in Colorado was in 1871 and was the Denver and Rio Grande Railroad line between Denver and Colorado Springs. A question we often hear is: “My father used to work for the railroad. How can I get information on Him?” Most railroad historical societies have no records on employees. Most employment records are owned today by the surviving railroad companies and the Railroad Retirement Board. For example, most such records for the Union Pacific Railroad are in storage in Hutchinson, Kansas salt mines, off limits to all but the lawyers. The Union Pacific currently declines to help with former employee genealogy requests. However, if you are looking for railroad employee records for early Colorado railroads, you may have some success. The Colorado Railroad Museum Library currently has 11,368 employee personnel records. These Colorado employee records are primarily for the following railroads which are not longer operating. Atchison, Topeka & Santa Fe Railroad (AT&SF) Atchison, Topeka and Santa Fe Railroad employee records of employment are recorded in a bound ledger book (record number 736) and box numbers 766 and 1287 for the years 1883 through 1939 for the joint line from Denver to Pueblo.
    [Show full text]
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • Trans-Neptunian Objects a Brief History, Dynamical Structure, and Characteristics of Its Inhabitants
    Trans-Neptunian Objects A Brief history, Dynamical Structure, and Characteristics of its Inhabitants John Stansberry Space Telescope Science Institute IAC Winter School 2016 IAC Winter School 2016 -- Kuiper Belt Overview -- J. Stansberry 1 The Solar System beyond Neptune: History • 1930: Pluto discovered – Photographic survey for Planet X • Directed by Percival Lowell (Lowell Observatory, Flagstaff, Arizona) • Efforts from 1905 – 1929 were fruitless • discovered by Clyde Tombaugh, Feb. 1930 (33 cm refractor) – Survey continued into 1943 • Kuiper, or Edgeworth-Kuiper, Belt? – 1950’s: Pluto represented (K.E.), or had scattered (G.K.) a primordial, population of small bodies – thus KBOs or EKBOs – J. Fernandez (1980, MNRAS 192) did pretty clearly predict something similar to the trans-Neptunian belt of objects – Trans-Neptunian Objects (TNOs), trans-Neptunian region best? – See http://www2.ess.ucla.edu/~jewitt/kb/gerard.html IAC Winter School 2016 -- Kuiper Belt Overview -- J. Stansberry 2 The Solar System beyond Neptune: History • 1978: Pluto’s moon, Charon, discovered – Photographic astrometry survey • 61” (155 cm) reflector • James Christy (Naval Observatory, Flagstaff) – Technologically, discovery was possible decades earlier • Saturation of Pluto images masked the presence of Charon • 1988: Discovery of Pluto’s atmosphere – Stellar occultation • Kuiper airborne observatory (KAO: 90 cm) + 7 sites • Measured atmospheric refractivity vs. height • Spectroscopy suggested N2 would dominate P(z), T(z) • 1992: Pluto’s orbit explained • Outward migration by Neptune results in capture into 3:2 resonance • Pluto’s inclination implies Neptune migrated outward ~5 AU IAC Winter School 2016 -- Kuiper Belt Overview -- J. Stansberry 3 The Solar System beyond Neptune: History • 1992: Discovery of 2nd TNO • 1976 – 92: Multiple dedicated surveys for small (mV > 20) TNOs • Fall 1992: Jewitt and Luu discover 1992 QB1 – Orbit confirmed as ~circular, trans-Neptunian in 1993 • 1993 – 4: 5 more TNOs discovered • c.
    [Show full text]
  • CNC/IUGG: 2019 Quadrennial Report
    CNC/IUGG: 2019 Quadrennial Report Geodesy and Geophysics in Canada 2015-2019 Quadrennial Report of the Canadian National Committee for the International Union of Geodesy and Geophysics Prepared on the Occasion of the 27th General Assembly of the IUGG Montreal, Canada July 2019 INTRODUCTION This report summarizes the research carried out in Canada in the fields of geodesy and geophysics during the quadrennial 2015-2019. It was prepared under the direction of the Canadian National Committee for the International Union of Geodesy and Geophysics (CNC/IUGG). The CNC/IUGG is administered by the Canadian Geophysical Union, in consultation with the Canadian Meteorological and Oceanographic Society and other Canadian scientific organizations, including the Canadian Association of Physicists, the Geological Association of Canada, and the Canadian Institute of Geomatics. The IUGG adhering organization for Canada is the National Research Council of Canada. Among other duties, the CNC/IUGG is responsible for: • collecting and reconciling the many views of the constituent Canadian scientific community on relevant issues • identifying, representing, and promoting the capabilities and distinctive competence of the community on the international stage • enhancing the depth and breadth of the participation of the community in the activities and events of the IUGG and related organizations • establishing the mechanisms for communicating to the community the views of the IUGG and information about the activities of the IUGG. The aim of this report is to communicate to both the Canadian and international scientific communities the research areas and research progress that has been achieved in geodesy and geophysics over the last four years. The main body of this report is divided into eight sections: one for each of the eight major scientific disciplines as represented by the eight sister societies of the IUGG.
    [Show full text]
  • EPSC2017-260, 2017 European Planetary Science Congress 2017 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2017
    EPSC Abstracts Vol. 11, EPSC2017-260, 2017 European Planetary Science Congress 2017 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2017 Formation of recurring slope lineae on Mars by rarefied gas-triggered granular flows F. Schmidt (1), F. Andrieu (1), F. Costard (1), M. Kocifaj (2,3) and A. G. Meresescu (1) (1) GEOPS, Univ. Paris-Sud, CNRS, Université Paris-Saclay, Rue du Belvédère, Bât. 504-509, 91405 Orsay, France (2) ICA, Slovak Academy of Sciences, Dubravska Road 9, 845 03 Bratislava, Slovak Republic (3) Faculty of Mathematics, Physics, and Informatics, Comenius University, Mlynska dolina, 842 48 Bratislava, Slovak Republic (frederic.schmidt@@u-psud.fr) Abstract been excluded near the crater rim [3]. In addition, the actual amount of atmospheric water required to re- Recurring Slope Linae or RSL are seasonal dark charge the RSL's source each year seems not features appearing when the soil reaches its sufficient. The precise thermal calculations using maximum temperature. They appear on various THEMIS measurement instrument show no evidence slopes at the equator of Mars, in orientation of liquid water [6] and there is no direct evidence of depending on the season. Today, liquid water related liquid water from CRISM, but only indirect detection processes have been promoted, such as deliquescence [4]. of salts. Nevertheless external atmospheric source of water is inconsistent with the observations. Internal We propose here a re-interpretation of the RSL source is also very unlikely. We take into features and a new process to explain the RSL consideration here the force occurring when the sun activity without involving any volatiles.
    [Show full text]
  • October 2003 SOCIETY
    ISSN 0739-4934 NEWSLETTER HISTORY OF SCIENCE VOLUME 32 NUMBER 4 October 2003 SOCIETY those with no interest in botany, the simple beauty of the glass is enough. Natural History Delights in Cambridge From modern-life in glass to long-ago life, it’s only a short walk. The museum houses ant to discuss dinosaurs, explore microfossils of some of the Earth’s earliest life Wancient civilizations, learn wild- forms, as well as fossil fish and dinosaurs – flower gardening, or study endangered such as the second ever described Triceratops, species? If variety is the spice of life, then and the world’s only mounted Kronosaurus, a the twenty-one million specimens at the 42-foot-long prehistoric marine reptile. Harvard Museum of Natural History show a Among its 90,000 zoological specimens the museum bursting with life, much of it unnat- museum also has the pheasants once owned urally natural. by George Washington. And many of the The museum will be the site of the opening mammal collections were put together in the reception for the 2003 HSS annual meeting. 19th century by “lions” in the history of sci- The reception begins at 7 p.m. Thursday, 20 ence, like Louis Agassiz. November, and tickets will be available at the Much of the museum’s collection of rocks and meeting registration desk. Buses will run from ores is the result of field work, but the museum the host hotel to the museum. houses not only that which has been dug up, but The Harvard MNH is an ideal spot for his- also that which has fallen out of the sky.
    [Show full text]
  • Cover No Spine
    2006 VOL 44, NO. 4 Special Issue: The Hans Christian Andersen Awards 2006 The Journal of IBBY,the International Board on Books for Young People Editors: Valerie Coghlan and Siobhán Parkinson Address for submissions and other editorial correspondence: [email protected] and [email protected] Bookbird’s editorial office is supported by the Church of Ireland College of Education, Dublin, Ireland. Editorial Review Board: Sandra Beckett (Canada), Nina Christensen (Denmark), Penni Cotton (UK), Hans-Heino Ewers (Germany), Jeffrey Garrett (USA), Elwyn Jenkins (South Africa),Ariko Kawabata (Japan), Kerry Mallan (Australia), Maria Nikolajeva (Sweden), Jean Perrot (France), Kimberley Reynolds (UK), Mary Shine Thompson (Ireland), Victor Watson (UK), Jochen Weber (Germany) Board of Bookbird, Inc.: Joan Glazer (USA), President; Ellis Vance (USA),Treasurer;Alida Cutts (USA), Secretary;Ann Lazim (UK); Elda Nogueira (Brazil) Cover image:The cover illustration is from Frau Meier, Die Amsel by Wolf Erlbruch, published by Peter Hammer Verlag,Wuppertal 1995 (see page 11) Production: Design and layout by Oldtown Design, Dublin ([email protected]) Proofread by Antoinette Walker Printed in Canada by Transcontinental Bookbird:A Journal of International Children’s Literature (ISSN 0006-7377) is a refereed journal published quarterly by IBBY,the International Board on Books for Young People, Nonnenweg 12 Postfach, CH-4003 Basel, Switzerland tel. +4161 272 29 17 fax: +4161 272 27 57 email: [email protected] <www.ibby.org>. Copyright © 2006 by Bookbird, Inc., an Indiana not-for-profit corporation. Reproduction of articles in Bookbird requires permission in writing from the editor. Items from Focus IBBY may be reprinted freely to disseminate the work of IBBY.
    [Show full text]
  • Abstracts of the 50Th DDA Meeting (Boulder, CO)
    Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011).
    [Show full text]
  • Impact Melt Emplacement on Mercury
    Western University Scholarship@Western Electronic Thesis and Dissertation Repository 7-24-2018 2:00 PM Impact Melt Emplacement on Mercury Jeffrey Daniels The University of Western Ontario Supervisor Neish, Catherine D. The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Jeffrey Daniels 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons, Physical Processes Commons, and the The Sun and the Solar System Commons Recommended Citation Daniels, Jeffrey, "Impact Melt Emplacement on Mercury" (2018). Electronic Thesis and Dissertation Repository. 5657. https://ir.lib.uwo.ca/etd/5657 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract Impact cratering is an abrupt, spectacular process that occurs on any world with a solid surface. On Earth, these craters are easily eroded or destroyed through endogenic processes. The Moon and Mercury, however, lack a significant atmosphere, meaning craters on these worlds remain intact longer, geologically. In this thesis, remote-sensing techniques were used to investigate impact melt emplacement about Mercury’s fresh, complex craters. For complex lunar craters, impact melt is preferentially ejected from the lowest rim elevation, implying topographic control. On Venus, impact melt is preferentially ejected downrange from the impact site, implying impactor-direction control. Mercury, despite its heavily-cratered surface, trends more like Venus than like the Moon.
    [Show full text]
  • 9–22–00 Vol. 65 No. 185 Friday Sept. 22, 2000 Pages 57277–57536
    9±22±00 Friday Vol. 65 No. 185 Sept. 22, 2000 Pages 57277±57536 VerDate 11-MAY-2000 19:36 Sep 21, 2000 Jkt 190000 PO 00000 Frm 00001 Fmt 4710 Sfmt 4710 E:\FR\FM\22SEWS.LOC pfrm11 PsN: 22SEWS 1 II Federal Register / Vol. 65, No. 185 / Friday, September 22, 2000 The FEDERAL REGISTER is published daily, Monday through SUBSCRIPTIONS AND COPIES Friday, except official holidays, by the Office of the Federal Register, National Archives and Records Administration, PUBLIC Washington, DC 20408, under the Federal Register Act (44 U.S.C. Subscriptions: Ch. 15) and the regulations of the Administrative Committee of Paper or fiche 202±512±1800 the Federal Register (1 CFR Ch. I). The Superintendent of Assistance with public subscriptions 512±1806 Documents, U.S. Government Printing Office, Washington, DC 20402 is the exclusive distributor of the official edition. General online information 202±512±1530; 1±888±293±6498 Single copies/back copies: The Federal Register provides a uniform system for making available to the public regulations and legal notices issued by Paper or fiche 512±1800 Federal agencies. These include Presidential proclamations and Assistance with public single copies 512±1803 Executive Orders, Federal agency documents having general FEDERAL AGENCIES applicability and legal effect, documents required to be published Subscriptions: by act of Congress, and other Federal agency documents of public interest. Paper or fiche 523±5243 Assistance with Federal agency subscriptions 523±5243 Documents are on file for public inspection in the Office of the Federal Register the day before they are published, unless the issuing agency requests earlier filing.
    [Show full text]
  • The Fate of Debris in the Pluto-Charon System
    MNRAS 000,1{13 (2016) Preprint 6 August 2018 Compiled using MNRAS LATEX style file v3.0 The Fate of Debris in the Pluto-Charon System Rachel A. Smullen,1? Kaitlin M. Kratter,1 1Steward Observatory, University of Arizona, Tucson, AZ 85721, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Pluto-Charon system has come into sharper focus following the fly by of New Horizons. We use N-body simulations to probe the unique dynamical history of this binary dwarf planet system. We follow the evolution of the debris disc that might have formed during the Charon-forming giant impact. First, we note that in-situ formation of the four circumbinary moons is extremely difficult if Charon undergoes eccentric tidal evolution. We track collisions of disc debris with Charon, estimating that hundreds to hundreds of thousands of visible craters might arise from 0.3{5 km radius bodies. New Horizons data suggesting a dearth of these small craters may place constraints on the disc properties. While tidal heating will erase some of the cratering history, both tidal and radiogenic heating may also make it possible to differentiate disc debris craters from Kuiper belt object craters. We also track the debris ejected from the Pluto-Charon system into the Solar System; while most of this debris is ultimately lost from the Solar System, a few tens of 10{30 km radius bodies could survive as a Pluto-Charon collisional family. Most are plutinos in the 3:2 resonance with Neptune, while a small number populate nearby resonances. We show that migration of the giant planets early in the Solar System's history would not destroy this collisional family.
    [Show full text]
  • 1 on the Origin of the Pluto System Robin M. Canup Southwest Research Institute Kaitlin M. Kratter University of Arizona Marc Ne
    On the Origin of the Pluto System Robin M. Canup Southwest Research Institute Kaitlin M. Kratter University of Arizona Marc Neveu NASA Goddard Space Flight Center / University of Maryland The goal of this chapter is to review hypotheses for the origin of the Pluto system in light of observational constraints that have been considerably refined over the 85-year interval between the discovery of Pluto and its exploration by spacecraft. We focus on the giant impact hypothesis currently understood as the likeliest origin for the Pluto-Charon binary, and devote particular attention to new models of planet formation and migration in the outer Solar System. We discuss the origins conundrum posed by the system’s four small moons. We also elaborate on implications of these scenarios for the dynamical environment of the early transneptunian disk, the likelihood of finding a Pluto collisional family, and the origin of other binary systems in the Kuiper belt. Finally, we highlight outstanding open issues regarding the origin of the Pluto system and suggest areas of future progress. 1. INTRODUCTION For six decades following its discovery, Pluto was the only known Sun-orbiting world in the dynamical vicinity of Neptune. An early origin concept postulated that Neptune originally had two large moons – Pluto and Neptune’s current moon, Triton – and that a dynamical event had both reversed the sense of Triton’s orbit relative to Neptune’s rotation and ejected Pluto onto its current heliocentric orbit (Lyttleton, 1936). This scenario remained in contention following the discovery of Charon, as it was then established that Pluto’s mass was similar to that of a large giant planet moon (Christy and Harrington, 1978).
    [Show full text]