Something STRANGE Is Flying Around
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CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S. -
Elements of Astronomy
^ ELEMENTS ASTRONOMY: DESIGNED AS A TEXT-BOOK uabemws, Btminwcus, anb families. BY Rev. JOHN DAVIS, A.M. FORMERLY PROFESSOR OF MATHEMATICS AND ASTRONOMY IN ALLEGHENY CITY COLLEGE, AND LATE PRINCIPAL OF THE ACADEMY OF SCIENCE, ALLEGHENY CITY, PA. PHILADELPHIA: PRINTED BY SHERMAN & CO.^ S. W. COB. OF SEVENTH AND CHERRY STREETS. 1868. Entered, according to Act of Congress, in the year 1867, by JOHN DAVIS, in the Clerk's OlBce of the District Court of the United States for the Western District of Pennsylvania. STEREOTYPED BY MACKELLAR, SMITHS & JORDAN, PHILADELPHIA. CAXTON PRESS OF SHERMAN & CO., PHILADELPHIA- PREFACE. This work is designed to fill a vacuum in academies, seminaries, and families. With the advancement of science there should be a corresponding advancement in the facilities for acquiring a knowledge of it. To economize time and expense in this department is of as much importance to the student as frugality and in- dustry are to the success of the manufacturer or the mechanic. Impressed with the importance of these facts, and having a desire to aid in the general diffusion of useful knowledge by giving them some practical form, this work has been prepared. Its language is level to the comprehension of the youthful mind, and by an easy and familiar method it illustrates and explains all of the principal topics that are contained in the science of astronomy. It treats first of the sun and those heavenly bodies with which we are by observation most familiar, and advances consecutively in the investigation of other worlds and systems which the telescope has revealed to our view. -
Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Origin of the Near-Earth Asteroid Phaethon and the Geminids Meteor Shower
University of Central Florida STARS Faculty Bibliography 2010s Faculty Bibliography 1-1-2010 Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León H. Campins University of Central Florida K. Tsiganis A. Morbidelli J. Licandro Find similar works at: https://stars.library.ucf.edu/facultybib2010 University of Central Florida Libraries http://library.ucf.edu This Article is brought to you for free and open access by the Faculty Bibliography at STARS. It has been accepted for inclusion in Faculty Bibliography 2010s by an authorized administrator of STARS. For more information, please contact [email protected]. Recommended Citation de León, J.; Campins, H.; Tsiganis, K.; Morbidelli, A.; and Licandro, J., "Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower" (2010). Faculty Bibliography 2010s. 92. https://stars.library.ucf.edu/facultybib2010/92 A&A 513, A26 (2010) Astronomy DOI: 10.1051/0004-6361/200913609 & c ESO 2010 Astrophysics Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León1,H.Campins2,K.Tsiganis3, A. Morbidelli4, and J. Licandro5,6 1 Instituto de Astrofísica de Andalucía-CSIC, Camino Bajo de Huétor 50, 18008 Granada, Spain e-mail: [email protected] 2 University of Central Florida, PO Box 162385, Orlando, FL 32816.2385, USA e-mail: [email protected] 3 Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece 4 Departement Casiopée: Universite de Nice - Sophia Antipolis, Observatoire de la Cˆote d’Azur, CNRS 4, 06304 Nice, France 5 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain 6 Department of Astrophysics, University of La Laguna, 38205 La Laguna, Tenerife, Spain Received 5 November 2009 / Accepted 26 January 2010 ABSTRACT Aims. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
Polyhymnia, and the Mass of Jupiter
ASTRONOMISCHE NACHRICHTEN. N2 3249. Band 136. On the Elements of (33) Polyhymnia, and the mass of Jupiter. By Simon Newconzb. More than twenty years ago, I called attention to the In the work as first done I used general perturbations great value of observations on the planet (33) Polyhymnia by the Earth, and omitted the action of Uranus entirely. for determining the mass of Jupiter (.4. N.Bd. 79, S. 245). It was found, however, on examination, that decimals enough I hoped by doing so to secure a continuous series of ob- had not been used in one term of long period in the servations at each opposition from that time onward; but general perturbations by the Earth, and I deemed it better this hope has been disappointed. Still, enough of obser- to reject them entirely, and use special perturbations. At vations have been made to afford a value of the mass the same time the opportunity of introducing the action of which I think is entitled to greater weight than any other Uranus was taken advantage of. single determination. In order to lessen thelabor of computing these small The work of making this investigation, like several perturbations, the disturbing forces were not computed for other works in which I am engaged, has been carried on intervals of an integral number of days, as usual, but for piece-meal, in a quite irregular way, for more than ten years. equi-distant mean anomalies of Polyhymnia (5" in the case As far back as 1884-8j, the special perturbations of the of the Earth; IOO in that of Uranus). -
The Basic Physics of the Binary Black Hole Merger GW150914
September 21, 2016 The basic physics of the binary black hole merger GW150914 The LIGO Scientific Collaboration and The Virgo Collaboration¤ The first direct gravitational-wave detection was made by the Advanced Laser Interferometer Gravitational Wave Observatory on September 14, 2015. The GW150914 signal was strong enough to be apparent, without using any waveform model, in the filtered detec- tor strain data. Here those features of the signal visible in these data are used, along with only such concepts from Newtonian physics and general relativity as are ac- cessible to anyone with a general physics background. The simple analysis presented here is consistent with the fully general-relativistic analyses published else- Figure 1 The instrumental strain data in the Livingston detec- where, in showing that the signal was produced by the tor (blue) and Hanford detector (red), as shown in Figure 1 of inspiral and subsequent merger of two black holes. The [1]. Both have been bandpass- and notch-filtered. The Hanford black holes were each of approximately 35M , still strain has been shifted back in time by 6.9 ms and inverted. ¯ Times shown are relative to 09:50:45 Coordinated Universal orbited each other as close as 350 km apart and sub- » Time (UTC) on September 14, 2015. sequently merged to form a single black hole. Similar reasoning, directly from the data, is used to roughly es- timate how far these black holes were from the Earth, A black hole is a region of space-time where the gravita- and the energy that they radiated in gravitational waves. -
IDL-1426.Pdf
The International Development Research Centre is a public corporation created by the Parliament of Canada in 1970 to support research designed to adapt science and technology to the needs of developing countries. The Centre's activity is concentrated in five sectors: agriculture, food and nutrition sciences; health sciences; information sciences; communications; and social sciences. IDRC is financed solely by the Government of Canada; its policies, however, are set by an international Board of Governors. The Centre's headquarters are in Ottawa, Canada. Regional offices are located in Africa, Asia, Latin America, and the Middle East. ©1978 International Development Research Centre Postal Address: Box 8500, Ottawa, Canada KlG 3H9 Head Office: 60 Queen Street, Ottawa Ronald, K. Selley, L.J. Amoroso, E.C. IDRC IDRC-TS13e Biological synopsis of the manatee. Ottawa, IDRC, 1978. 112 p. /IDRC publication/. Monograph on the manatee, an aquatic mammal (/animal species/) of the /tropical zone/s of I Africa south of Sahara/ and /Latin America/, with an extensive /bibliography/ - discusses the /classification/ of the species and subspecies of the genus Trichechus; /morphology/, /physiology/, /behaviour/, /reproduction/, /animal ecology/ (role in /aquatic plant/ /weed control/), and measures for /animal protection/ of the manatee. UDC: 599.55 ISBN: 0-88936-168-1 Microfiche edition available IDRC-TS13e Biological Synopsis of the Manatee K. Ronald, L.J. Selley, and E.C. Amoroso1 College ofBiological Science, University of Guelph, Guelph, Ontario 1 Present address: Agricultural Research Council, Institute of Animal Physiology, Babraham, Cambridge, England. This work was carried out with the aid of a grant from the International Development Research Centre. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 35, NUMBER 3, A.D. 2008 JULY-SEPTEMBER 95. ASTEROID LIGHTCURVE ANALYSIS AT SCT/ST-9E, or 0.35m SCT/STL-1001E. Depending on the THE PALMER DIVIDE OBSERVATORY: binning used, the scale for the images ranged from 1.2-2.5 DECEMBER 2007 – MARCH 2008 arcseconds/pixel. Exposure times were 90–240 s. Most observations were made with no filter. On occasion, e.g., when a Brian D. Warner nearly full moon was present, an R filter was used to decrease the Palmer Divide Observatory/Space Science Institute sky background noise. Guiding was used in almost all cases. 17995 Bakers Farm Rd., Colorado Springs, CO 80908 [email protected] All images were measured using MPO Canopus, which employs differential aperture photometry to determine the values used for (Received: 6 March) analysis. Period analysis was also done using MPO Canopus, which incorporates the Fourier analysis algorithm developed by Harris (1989). Lightcurves for 17 asteroids were obtained at the Palmer Divide Observatory from December 2007 to early The results are summarized in the table below, as are individual March 2008: 793 Arizona, 1092 Lilium, 2093 plots. The data and curves are presented without comment except Genichesk, 3086 Kalbaugh, 4859 Fraknoi, 5806 when warranted. Column 3 gives the full range of dates of Archieroy, 6296 Cleveland, 6310 Jankonke, 6384 observations; column 4 gives the number of data points used in the Kervin, (7283) 1989 TX15, 7560 Spudis, (7579) 1990 analysis. Column 5 gives the range of phase angles. -
IRTF Spectra for 17 Asteroids from the C and X Complexes: a Discussion of Continuum Slopes and Their Relationships to C Chondrites and Phyllosilicates ⇑ Daniel R
Icarus 212 (2011) 682–696 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus IRTF spectra for 17 asteroids from the C and X complexes: A discussion of continuum slopes and their relationships to C chondrites and phyllosilicates ⇑ Daniel R. Ostrowski a, Claud H.S. Lacy a,b, Katherine M. Gietzen a, Derek W.G. Sears a,c, a Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, United States b Department of Physics, University of Arkansas, Fayetteville, AR 72701, United States c Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, AR 72701, United States article info abstract Article history: In order to gain further insight into their surface compositions and relationships with meteorites, we Received 23 April 2009 have obtained spectra for 17 C and X complex asteroids using NASA’s Infrared Telescope Facility and SpeX Revised 20 January 2011 infrared spectrometer. We augment these spectra with data in the visible region taken from the on-line Accepted 25 January 2011 databases. Only one of the 17 asteroids showed the three features usually associated with water, the UV Available online 1 February 2011 slope, a 0.7 lm feature and a 3 lm feature, while five show no evidence for water and 11 had one or two of these features. According to DeMeo et al. (2009), whose asteroid classification scheme we use here, 88% Keywords: of the variance in asteroid spectra is explained by continuum slope so that asteroids can also be charac- Asteroids, composition terized by the slopes of their continua. -
(K)Cudos at Ψtucson
(K)CUDOs at ΨTucson Work based on collaborative effort with present/former AZ students: Jeremiah Birrell and Lance Labun with contributions from exchange student from Germany Ch. Dietl. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 1/39 1. Introduction 2. Dark Matter (CDM) Generalities 3. Strangeletts 4. Dark Matter (DM) CUDOs 5. CUDO impacts Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 2/39 kudos (from Greek kyddos, singular) = honor; glory; acclaim; praise kudo = back formation from kudos construed as a plural cud (Polish, pronounced c-ood) = miracle cudo (colloq. Polish) = of surprising and exceptional character CUDO=Compact UltraDense Object: A new opportunity to search for dark matter. Not dark matter in form of elementary particles (all present day searches) but (self) bound dark matter. Either an ultra-compact impactor or/and condensation seed for comets. There is a lot of dark matter around, cosmological abundance limit shown below. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 3/39 A new type of meteors What if there are ‘dark’ matter meteor and asteroid-like bodies in the Universe? Could some of them have collided with solar system bodies and the Earth? Are they dressed in visible matter from prior impacts and as condensation seeds? CUDOs’ high density of gravitating matter provides the distinct observable, the surface-penetrating puncture: shot through Only a fraction of the kinetic energy damaging the solid surface. Johann Rafelski (UA-Physics) (K)CUDOS at ΨTucson PSITucson,April11,2013 4/39 Asteroids of high density Fruitful Discussions with Marshall Eubanks lead to these data. -
Asteroid Observations at Low Phase Angles. IV. Average Parameters for the New H, G1, G2 Magnitude System Vasilij G
Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎ Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Asteroid observations at low phase angles. IV. Average parameters for the new H, G1, G2 magnitude system Vasilij G. Shevchenko a,b,n, Irina N. Belskaya a, Karri Muinonen c,d, Antti Penttilä c, Yurij N. Krugly a, Feodor P. Velichko a, Vasilij G. Chiorny a, Ivan G. Slyusarev a,b, Ninel M. Gaftonyuk e, Igor A. Tereschenko a a Institute of Astronomy of Kharkiv Karazin National University, Sumska str. 35, Kharkiv 61022, Ukraine b Department of Astronomy and Space Informatics of Kharkiv Karazin National University, Svobody sqr. 4, Kharkiv 61022, Ukraine c Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Finland d Finnish Geospatial Research Institute, P.O. Box 15, Masala, FI-02431, Finland e Crimean Astrophysical Observatory, Crimea, Simeiz 98680, Ukraine article info abstract Article history: We present new observational data for selected main-belt asteroids of different compositional types. The Received 21 January 2015 detailed magnitude–phase dependences including small phase angles (o1°) were obtained for these Received in revised form asteroids, namely: (10) Hygiea (down to the phase angle of 0.3°, C-type), (176) Iduna (0.2°, G-type), (214) 6 September 2015 Aschera (0.2°, E-type), (218) Bianca (0.3°, S-type), (250) Bettina (0.3°, M-type), (419) Aurelia (0.1°, F-type), Accepted 19 November 2015 (596) Scheila (0.2°, D-type), (635) Vundtia (0.2°, B-type), (671) Carnegia (0.2°, P-type), (717) Wisibada (0.1°, T-type), (1021) Flammario (0.6°, B-type), and (1279) Uganda (0.5°, E-type).