David E. Trilling Curriculum Vitae (13 September 2011)
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Review Section
CSIRO PUBLISHING www.publish.csiro.au/journals/hras Historical Records of Australian Science, 2004, 15, 121–138 Review Section Compiled by Libby Robin Centre for Resource and Environmental Studies (CRES), Australian National University, Canberra, ACT, 0200, Australia. Email: [email protected] Tom Frame and Don Faulkner: Stromlo: loss of what he described as a ‘national an Australian observatory. Allen & Unwin: icon’. Sydney, 2003. xix + 363 pp., illus., ISBN 1 Institutional histories are often suffused 86508 659 2 (PB), $35. with a sense of inevitability. Looking back from the security of a firmly grounded present, the road seems straight and well marked. The journey that is reconstructed is one where the end point is always known, where uncertainties and diversions are forgotten — a journey that lands neatly on the institution’s front doorstep. Institu- tional histories are often burdened, too, by the expectation that they will not merely tell a story, but provide a record of achieve- ment. Written for the institution’s staff, as well as broader public, they can become bogged down in the details of personnel and projects. In this case, the fires of January 2003 add an unexpected final act Few institutional histories could boast such to what is a fairly traditional story of a dramatic conclusion as Stromlo: an Aus- growth and success. The force of nature tralian observatory. The manuscript was intervenes to remind us of the limits of substantially complete when a savage fire- inevitability, to fashion from the end point storm swept through the pine plantations another beginning. flanking Mount Stromlo, destroying all the The book is roughly divided into halves. -
William Liller (1927–2021)
Bulletin of the AAS • Vol. 53, Issue 2 William Liller (1927–2021) Alan Hirshfeld1, Christine Jones2, William Forman2 1UMass Dartmouth, 2Center for Astrophysics | Harvard & Smithsonian Published on: Apr 07, 2021 DOI: 10.3847/25c2cfeb.97f3253d License: Creative Commons Attribution 4.0 International License (CC-BY 4.0) Bulletin of the AAS • Vol. 53, Issue 2 William Liller (1927–2021) William Liller died on Sunday the 28th of February 2021. William (“Bill”) Liller, research mentor and major contributor to the study of planetary nebulae, comets, asteroids, magnetic activity in cool stars, the optical identification of X-ray sources, and astro-archaeology, died peacefully in his sleep on 28 February 2021, after a brief illness. He was 93 years old. Born on 1 April 1927 in Philadelphia to Carroll Kalbaugh “Pete” Liller, an advertising executive, and his wife, Catherine Dellinger Liller, Bill noted in the book “Asteroids to Quasars” that he became “obsessed with astronomy” in Photo courtesy Clive Grainger. August 1932, when his uncle drove up from West Virginia in a Model A Ford to view a solar eclipse from New York, near where Bill’s family was living at the time. At age 13, Bill’s report on the Quadrantid meteor shower was cited in an article in Popular Astronomy from the American Meteor Society. In his letter to the society, Bill had misspelled the name of the society’s director, C. P. Olivier, which Bill believed led to an intentional misspelling of his own name in the published article as “Billy Lillier.” In the February 2018 issue of the alumni magazine of Harvard’s Adams House, Bill recalled the years leading up to his matriculation in 1944: “After attending public schools in my home town of Atlanta, I was shipped off ‘to finish,’ and I spent my last two high school years at Mercersburg Academy in Pennsylvania. -
Ira Sprague Bowen Papers, 1940-1973
http://oac.cdlib.org/findaid/ark:/13030/tf2p300278 No online items Inventory of the Ira Sprague Bowen Papers, 1940-1973 Processed by Ronald S. Brashear; machine-readable finding aid created by Gabriela A. Montoya Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 © 1998 The Huntington Library. All rights reserved. Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague 1 Bowen Papers, 1940-1973 Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague Bowen Paper, 1940-1973 The Huntington Library San Marino, California Contact Information Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 Processed by: Ronald S. Brashear Encoded by: Gabriela A. Montoya © 1998 The Huntington Library. All rights reserved. Descriptive Summary Title: Ira Sprague Bowen Papers, Date (inclusive): 1940-1973 Creator: Bowen, Ira Sprague Extent: Approximately 29,000 pieces in 88 boxes Repository: The Huntington Library San Marino, California 91108 Language: English. Provenance Placed on permanent deposit in the Huntington Library by the Observatories of the Carnegie Institution of Washington Collection. This was done in 1989 as part of a letter of agreement (dated November 5, 1987) between the Huntington and the Carnegie Observatories. The papers have yet to be officially accessioned. Cataloging of the papers was completed in 1989 prior to their transfer to the Huntington. -
Pos(Westerbork)002 Historical Introduction Historical S 4.0 International License (CC BY-NC-ND 4.0)
Historical Introduction PoS(Westerbork)002 Richard Strom ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] 50 Years Westerbork Radio Observatory, A Continuing Journey to Discoveries and Innovations Richard Strom, Arnold van Ardenne, Steve Torchinsky (eds) Published with permission of the Netherlands Institute for Radio Astronomy (ASTRON) under the terms of the Creative CommonsAttribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Chapter 1 Historical introduction Richard Strom* rom the English longbows at the battle of Crécy (1346) to Winston Chur- chill’s world war I mobilized cannon (its true identity hidden behind the Fpseudonym “[water] tank”), warfare has always pushed technological innovation to new fronts. The second world war (WWII) was no exception. It gave us technology ranging from the dynamo-powered flashlight (a Philips invention) to jet engines, and space-capable rockets (Germany’s V2), not to mention (in a completely different realm) the mass production of Penicillin. In fact, it could be argued that WWII inventions marked the inception of the modern technological era1. In the field of electronics, the war led to innovations such as radio navigation, aircraft landing systems, and radar. It was these developments which were to * ASTRON, Univer- sity of Amsterdam, have a revolutionary impact on astronomy, initially in Britain, Australia and the The Netherlands United States. But the story begins in the US, with the electronics of the 1920s and ‘30s. Figure 1. Karl G. Jansky (c. 1933) Around 1930, there was increasing interest in the use of radio frequencies for communication. One of the main players, the Bell Telephone Laboratories in New Jersey, asked their research engineer, Karl Jansky (Figure 1), to investigate the inter- ference environment in the “short-wave” band around 20 MHz. -
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. -
The Kuiper Belt Luminosity Function from Mr = 22 to 25 Jean-Marc Petit, M
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Archive Ouverte en Sciences de l'Information et de la Communication The Kuiper Belt luminosity function from mR = 22 to 25 Jean-Marc Petit, M. Holman, B. Gladman, J. Kavelaars, H. Scholl, T. Loredo To cite this version: Jean-Marc Petit, M. Holman, B. Gladman, J. Kavelaars, H. Scholl, et al.. The Kuiper Belt lu- minosity function from mR = 22 to 25. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2006, 365 (2), pp.429-438. 10.1111/j.1365- 2966.2005.09661.x. hal-02374819 HAL Id: hal-02374819 https://hal.archives-ouvertes.fr/hal-02374819 Submitted on 21 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 000, 1{11 (2005) Printed 7 September 2005 (MN LATEX style file v2.2) The Kuiper Belt's luminosity function from mR=22{25. J-M. Petit1;7?, M.J. Holman2;7, B.J. Gladman3;5;7, J.J. Kavelaars4;7 H. Scholl3 and T.J. -
Mass of the Kuiper Belt · 9Th Planet PACS 95.10.Ce · 96.12.De · 96.12.Fe · 96.20.-N · 96.30.-T
Celestial Mechanics and Dynamical Astronomy manuscript No. (will be inserted by the editor) Mass of the Kuiper Belt E. V. Pitjeva · N. P. Pitjev Received: 13 December 2017 / Accepted: 24 August 2018 The final publication ia available at Springer via http://doi.org/10.1007/s10569-018-9853-5 Abstract The Kuiper belt includes tens of thousands of large bodies and millions of smaller objects. The main part of the belt objects is located in the annular zone between 39.4 au and 47.8 au from the Sun, the boundaries correspond to the average distances for orbital resonances 3:2 and 2:1 with the motion of Neptune. One-dimensional, two-dimensional, and discrete rings to model the total gravitational attraction of numerous belt objects are consid- ered. The discrete rotating model most correctly reflects the real interaction of bodies in the Solar system. The masses of the model rings were determined within EPM2017—the new version of ephemerides of planets and the Moon at IAA RAS—by fitting spacecraft ranging observations. The total mass of the Kuiper belt was calculated as the sum of the masses of the 31 largest trans-neptunian objects directly included in the simultaneous integration and the estimated mass of the model of the discrete ring of TNO. The total mass −2 is (1.97 ± 0.30) · 10 m⊕. The gravitational influence of the Kuiper belt on Jupiter, Saturn, Uranus and Neptune exceeds at times the attraction of the hypothetical 9th planet with a mass of ∼ 10 m⊕ at the distances assumed for it. -
Planetarian Index
Planetarian Cumulative Index 1972 – 2008 Vol. 1, #1 through Vol. 37, #3 John Mosley [email protected] The PLANETARIAN (ISSN 0090-3213) is published quarterly by the International Planetarium Society under the auspices of the Publications Committee. ©International Planetarium Society, Inc. From the Compiler I compiled the first edition of this index 25 years ago after a frustrating search to find an article that I knew existed and that I really needed. It was a long search without even annual indices to help. By the time I found it, I had run across a dozen other articles that I’d forgotten about but was glad to see again. It was clear that there are a lot of good articles buried in back issues, but that without some sort of index they’d stay lost. I had recently bought an Apple II computer and was receptive to projects that would let me become more familiar with its word processing program. A cumulative index seemed a reasonable project that would be instructive while not consuming too much time. Hah! I did learn some useful solutions to word-processing problems I hadn’t previously known exist, but it certainly did consume more time than I’d imagined by a factor of a dozen or so. You too have probably reached the point where you’ve invested so much time in a project that it’s psychologically easier to finish it than admit defeat. That’s how the first index came to be, and that’s why I’ve kept it up to date. -
Anton Pannekoek: Ways of Viewing Science and Society
STUDIES IN THE HISTORY OF KNOWLEDGE Tai, Van der Steen & Van Dongen (eds) Dongen & Van Steen der Van Tai, Edited by Chaokang Tai, Bart van der Steen, and Jeroen van Dongen Anton Pannekoek: Ways of Viewing Science and Society Ways of Viewing ScienceWays and Society Anton Pannekoek: Anton Pannekoek: Ways of Viewing Science and Society Studies in the History of Knowledge This book series publishes leading volumes that study the history of knowledge in its cultural context. It aspires to offer accounts that cut across disciplinary and geographical boundaries, while being sensitive to how institutional circumstances and different scales of time shape the making of knowledge. Series Editors Klaas van Berkel, University of Groningen Jeroen van Dongen, University of Amsterdam Anton Pannekoek: Ways of Viewing Science and Society Edited by Chaokang Tai, Bart van der Steen, and Jeroen van Dongen Amsterdam University Press Cover illustration: (Background) Fisheye lens photo of the Zeiss Planetarium Projector of Artis Amsterdam Royal Zoo in action. (Foreground) Fisheye lens photo of a portrait of Anton Pannekoek displayed in the common room of the Anton Pannekoek Institute for Astronomy. Source: Jeronimo Voss Cover design: Coördesign, Leiden Lay-out: Crius Group, Hulshout isbn 978 94 6298 434 9 e-isbn 978 90 4853 500 2 (pdf) doi 10.5117/9789462984349 nur 686 Creative Commons License CC BY NC ND (http://creativecommons.org/licenses/by-nc-nd/3.0) The authors / Amsterdam University Press B.V., Amsterdam 2019 Some rights reserved. Without limiting the rights under copyright reserved above, any part of this book may be reproduced, stored in or introduced into a retrieval system, or transmitted, in any form or by any means (electronic, mechanical, photocopying, recording or otherwise). -
Journal Pre-Proof
Journal Pre-proof A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt Mark R. Showalter, Susan D. Benecchi, Marc W. Buie, William M. Grundy, James T. Keane, Carey M. Lisse, Cathy B. Olkin, Simon B. Porter, Stuart J. Robbins, Kelsi N. Singer, Anne J. Verbiscer, Harold A. Weaver, Amanda M. Zangari, Douglas P. Hamilton, David E. Kaufmann, Tod R. Lauer, D.S. Mehoke, T.S. Mehoke, J.R. Spencer, H.B. Throop, J.W. Parker, S. Alan Stern, the New Horizons Geology, Geophysics, and Imaging Team PII: S0019-1035(20)30444-9 DOI: https://doi.org/10.1016/j.icarus.2020.114098 Reference: YICAR 114098 To appear in: Icarus Received date: 25 November 2019 Revised date: 30 August 2020 Accepted date: 1 September 2020 Please cite this article as: M.R. Showalter, S.D. Benecchi, M.W. Buie, et al., A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt, Icarus (2020), https://doi.org/10.1016/j.icarus.2020.114098 This is a PDF file of an article that has undergone enhancements after acceptance, such as the addition of a cover page and metadata, and formatting for readability, but it is not yet the definitive version of record. This version will undergo additional copyediting, typesetting and review before it is published in its final form, but we are providing this version to give early visibility of the article. Please note that, during the production process, errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. -
Collision Probabilities in the Edgeworth-Kuiper Belt
Draft version April 30, 2021 Typeset using LATEX default style in AASTeX63 Collision Probabilities in the Edgeworth-Kuiper belt Abedin Y. Abedin,1 JJ Kavelaars,1 Sarah Greenstreet,2, 3 Jean-Marc Petit,4 Brett Gladman,5 Samantha Lawler,6 Michele Bannister,7 Mike Alexandersen,8 Ying-Tung Chen,9 Stephen Gwyn,1 and Kathryn Volk10 1National Research Council of Canada, Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 2B612 Asteroid Institute, 20 Sunnyside Avenue, Suite 427, Mill Valley, CA 94941, USA 3DIRAC Center, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USA 4Institut UTINAM, CNRS-UMR 6213, Universit´eBourgogne Franche Comt´eBP 1615, 25010 Besan¸conCedex, France 5Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, British Columbia, Canada 6Campion College and the Department of Physics, University of Regina, Regina SK, S4S 0A2, Canada 7University of Canterbury, Christchurch, New Zealand 8Minor Planet Center, Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, US 9Academia Sinica Institute of Astronomy and Astrophysics, Taiwan 10Lunar and Planetary Laboratory, University of Arizona: Tucson, AZ, USA Submitted to AJ ABSTRACT Here, we present results on the intrinsic collision probabilities, PI , and range of collision speeds, VI , as a function of the heliocentric distance, r, in the trans-Neptunian region. The collision speed is one of the parameters, that serves as a proxy to a collisional outcome e.g., complete disruption and scattering of fragments, or formation of crater, where both processes are directly related to the impact energy. We utilize an improved and de-biased model of the trans-Neptunian object (TNO) region from the \Outer Solar System Origins Survey" (OSSOS). -
Outer Solar System Perihelion Gap Formation Through Interactions with a Hypothetical Distant Giant Planet
Draft version July 15, 2021 Typeset using LATEX twocolumn style in AASTeX63 Outer Solar System Perihelion Gap Formation Through Interactions with a Hypothetical Distant Giant Planet William J. Oldroyd 1 and Chadwick A. Trujillo 1 1Department of Astronomy & Planetary Science Northern Arizona University PO Box 6010, Flagstaff, AZ 86011, USA (Received 2021 February 10; Revised 2021 April 13; Accepted 2021 April 22; Published 2021 July 1) Submitted to AJ ABSTRACT Among the outer solar system minor planet orbits there is an observed gap in perihelion between roughly 50 and 65 au at eccentricities e & 0:65. Through a suite of observational simulations, we show that the gap arises from two separate populations, the Extreme Trans-Neptunian Objects (ETNOs; perihelia q & 40 au and semimajor axes a & 150 au) and the Inner Oort Cloud objects (IOCs; q & 65 au and a & 250 au), and is very unlikely to result from a realistic single, continuous distribution of objects. We also explore the connection between the perihelion gap and a hypothetical distant giant planet, often referred to as Planet 9 or Planet X, using dynamical simulations. Some simulations containing Planet X produce the ETNOs, the IOCs, and the perihelion gap from a simple Kuiper-Belt-like initial particle distribution over the age of the solar system. The gap forms as particles scattered to high eccentricity by Neptune are captured into secular resonances with Planet X where they cross the gap and oscillate in perihelion and eccentricity over hundreds of kiloyears. Many of these objects reach a minimum perihelia in their oscillation cycle within the IOC region increasing the mean residence time of the IOC region by a factor of approximately five over the gap region.