Occultation Newsletter Volume 8, Number 4
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Occultation Newsletter Volume 8, Number 4
Volume 8, Number 4 January 2002 $5.00 North Am./$6.25 Other Occultation of Saturn International Occultation Timing Association, Inc. (IOTA) In this Issue Articles Page Lunar Occultation Workbench 3.1: stellar occultations tailor-made to your needs . 4 The GAIA Mission: Main Scientific Goals and Contributions to Occultation Programs . .10 Welcome Our New Members . 12 The Detection of Close Stars by Occultations . 13 Personal Equation Comparison . .16 The February 16, 2001 Asteroid (83) Beatrix Occultation . 17 The Discovery of the Binary Star 64 Orionis. 18 The New Binary Star, 36 Sextantis . 18 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . 19 IOTA European Service (IOTA/ES) . 19 IOTA on the World Wide Web. Back Cover IOTA’s Telephone Network . Back Cover ON THE COVER: Image of the occultation of Saturn on 2002 February 20. This image was taken by Joan and David Dunham. 2 Occultation Newsletter, Volume 8, Number 3; January 2002 International Occultation Timing Association, Inc. (IOTA) What to Send to Whom Membership and Subscription Information All payments made to IOTA must be in United States Send new and renewal memberships and subscriptions, back funds and drawn on a US bank, or by credit card charge to issue requests, address changes, email address changes, graze VISA or MasterCard. If you use VISA or MasterCard, include prediction requests, reimbursement requests, special requests, your account number, expiration date, and signature. (Do not and other IOTA business, but not observation reports, to: send credit card information through e-mail. -
A Radar Survey of Main-Belt Asteroids: Arecibo Observations of 55 Objects During 1999–2003
Icarus 186 (2007) 126–151 www.elsevier.com/locate/icarus A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003 Christopher Magri a,∗, Michael C. Nolan b,StevenJ.Ostroc, Jon D. Giorgini d a University of Maine at Farmington, 173 High Street—Preble Hall, Farmington, ME 04938, USA b Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA c 300-233, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA d 301-150, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA Received 3 June 2006; revised 10 August 2006 Available online 24 October 2006 Abstract We report Arecibo observations of 55 main-belt asteroids (MBAs) during 1999–2003. Most of our targets had not been detected previously with radar, so these observations more than double the number of radar-detected MBAs. Our bandwidth estimates constrain our targets’ pole directions in a manner that is geometrically distinct from optically derived constraints. We present detailed statistical analyses of the disk-integrated properties (radar albedo and circular polarization ratio) of the 84 MBAs observed with radar through March 2003; all of these observations are summarized in the online supplementary information. Certain conclusions reached in previous studies are strengthened: M asteroids have higher mean radar albedos and a wider range of albedos than do other MBAs, suggesting that both metal-rich and metal-poor M-class objects exist; and C- and S-class MBAs have indistinguishable radar albedo distributions, suggesting that most S-class objects are chondritic. Also in accord with earlier results, there is evidence that primitive asteroids from outside the C taxon (F, G, P, and D) are not as radar-bright as C and S objects, but a convincing statistical test must await larger sample sizes. -
The V-Band Photometry of Asteroids from ASAS-SN
Astronomy & Astrophysics manuscript no. 40759˙ArXiV © ESO 2021 July 22, 2021 V-band photometry of asteroids from ASAS-SN Finding asteroids with slow spin ? J. Hanusˇ1, O. Pejcha2, B. J. Shappee3, C. S. Kochanek4;5, K. Z. Stanek4;5, and T. W.-S. Holoien6;?? 1 Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 2 Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 3 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 4 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 5 Center for Cosmology and Astroparticle Physics, The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA 6 The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA Received x-x-2021 / Accepted x-x-2021 ABSTRACT We present V-band photometry of the 20,000 brightest asteroids using data from the All-Sky Automated Survey for Supernovae (ASAS-SN) between 2012 and 2018. We were able to apply the convex inversion method to more than 5,000 asteroids with more than 60 good measurements in order to derive their sidereal rotation periods, spin axis orientations, and shape models. We derive unique spin state and shape solutions for 760 asteroids, including 163 new determinations. This corresponds to a success rate of about 15%, which is significantly higher than the success rate previously achieved using photometry from surveys. -
UV to Far-IR Reflectance Spectra of Carbonaceous Chondrites
UV to far-IR reflectance spectra of carbonaceous chondrites. I. Implications for remote characterization of dark primitive asteroids targeted by sample-return missions Josep M. Trigo-Rodriguez1, Carles E. Moyano-Cambero1, Jordi Llorca2, Sonia Fornasier3, Maria A. Barucci3, Irina Belskaya3, Zita Martins4, Andy S. Rivkin5, Elisabetta Dotto6 José M. Madiedo7, 8, and 9 Jacinto Alonso-Azcárate 1 Institute of Space Sciences (CSIC-IEEC), Campus UAB, Facultat de Ciències, Torre C-5, parells, 2a planta, 08193 Bellaterra (Barcelona), SPAIN 2 Institut de Tècniques Energètiques i Centre de Recerca en Nanoenginyeria. Universitat Politècnica de Catalunya, Diagonal 647, ETSEIB. Barcelona, Spain. 3 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris-Diderot, 5 Place Jules Janssen, 92195 Meudon Principal Cedex, France 4 Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK. 5 John Hopkins University Applied Physics Laboratory, Laurel, MD, USA. 6 INAF-Osservatorio Astronomico di Roma, Rome, Italy. 7 Facultad de Ciencias Experimentales, Universidad de Huelva, Huelva, Spain. 8 Departamento de Física Atómica, Molecular y Nuclear. Facultad de Física, 41012 Sevilla, Spain. 9 Universidad de Castilla-La Mancha, Campus Fábrica de Armas, 45071 Toledo, Spain. Abstract: We analyze here a wide sample of carbonaceous chondrites from historic falls (e.g. Allende, Cold Bokkeveld, Kainsaz, Leoville, Murchison, Murray, Orgueil, and Tagish Lake), and from NASA Antarctic collection in order to get clues on the role of aqueous alteration in promoting the reflectance spectra diversity evidenced in the most primitive chondrite groups. We particularly focus in the identification of spectral features and behavior that can be used to remotely identify primitive carbonaceous asteroids. -
The Minor Planet Bulletin 36, 188-190
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 3, A.D. 2010 JULY-SEPTEMBER 81. ROTATION PERIOD AND H-G PARAMETERS telescope (SCT) working at f/4 and an SBIG ST-8E CCD. Baker DETERMINATION FOR 1700 ZVEZDARA: A independently initiated observations on 2009 September 18 at COLLABORATIVE PHOTOMETRY PROJECT Indian Hill Observatory using a 0.3-m SCT reduced to f/6.2 coupled with an SBIG ST-402ME CCD and Johnson V filter. Ronald E. Baker Benishek from the Belgrade Astronomical Observatory joined the Indian Hill Observatory (H75) collaboration on 2009 September 24 employing a 0.4-m SCT PO Box 11, Chagrin Falls, OH 44022 USA operating at f/10 with an unguided SBIG ST-10 XME CCD. [email protected] Pilcher at Organ Mesa Observatory carried out observations on 2009 September 30 over more than seven hours using a 0.35-m Vladimir Benishek f/10 SCT and an unguided SBIG STL-1001E CCD. As a result of Belgrade Astronomical Observatory the collaborative effort, a total of 17 time series sessions was Volgina 7, 11060 Belgrade 38 SERBIA obtained from 2009 August 20 until October 19. All observations were unfiltered with the exception of those recorded on September Frederick Pilcher 18. MPO Canopus software (BDW Publishing, 2009a) employing 4438 Organ Mesa Loop differential aperture photometry, was used by all authors for Las Cruces, NM 88011 USA photometric data reduction. The period analysis was performed using the same program. David Higgins Hunter Hill Observatory The data were merged by adjusting instrumental magnitudes and 7 Mawalan Street, Ngunnawal ACT 2913 overlapping characteristic features of the individual lightcurves. -
The Planetary and Lunar Ephemeris DE 421
IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence. -
New Reflectance Spectra of 40 Asteroids: a Comparison with the Previous Results and an Interpretation1 V
ISSN 00380946, Solar System Research, 2016, Vol. 50, No. 1, pp. 13–23. © Pleiades Publishing, Inc., 2016. Original Russian Text © V.V. Busarev, 2016, published in Astronomicheskii Vestnik, 2016, Vol. 50, No. 1, pp. 15–26. New Reflectance Spectra of 40 Asteroids: 1 A Comparison with the Previous Results and an Interpretation V. V. Busarev Sternberg Astronomical Institute, Moscow Lomonosov State University, Moscow, 119991 Russia email: [email protected] Received April 22, 2014; in final form, May 28, 2015 Abstract—This paper presents and discusses selected reflectance spectra of 40 Main Belt asteroids. The spec tra have been obtained by the author in the Crimean Laboratory of the Sternberg Astronomical Institute (2003–2009). The aim is to search for new spectral features that characterize the composition of the asteroids’ material. The results are compared with earlier findings to reveal substantial irregularities in the distribution of the chemicalmineralogical compositions of the surface material of a number of minor planets (10 Hygiea, 13 Egeria, 14 Irene, 21 Lutetia, 45 Eugenia, 51 Nemausa, 55 Pandora, 64 Angelina, 69 Hesperia, 80 Sappho, 83 Beatrix, 92 Undina, 129 Antigone, 135 Hertha, and 785 Zwetana), which are manifest at different rotation phases. The vast majority of the analyzed hightemperature asteroids demonstrate subtle spectral features of an atypical hydrated and/or carbonaceous chondrite material (in the form of impurities or separate units), which are likely associated with the peculiarities of the formation of these bodies and the subsequent dynamic and impact processes, which lead, inter alia, to the delivery of atypical materials. Studies of 4 Vesta aboard NASA’s Dawn spacecraft have found that asteroids of similar types can form their own phyllosilicate genera tions provided that their surface material contains buried icy or hydrated fragments of impacting bodies. -
These Two Nebula M 20 Top and M 8 Bottom Are Popular Observing Targets in Sagittarius
These two nebula M 20 top and M 8 bottom are popular observing targets in Sagittarius This stunning two frame photo was taken by Michael Blaylock with an SBIG ST-8300C camera and process with PixInsight 1.8 software Contents: 1 M 20 and M 8 Nebular by Michael Blaylock 2 Upcoming Observing Night Events - Covid Guidelines 3 Alcon 2021 - Aug. 19-21 and Okie-Tex Oct 1-9 4 President’s Message - Dog Days of Summer – by Tamara Green 5 What’s Up in Tonight’s Sky by John Land 6 1/10 billionth scale Walkway through the Solar System coming to Broken Arrow 7 Making Good use of club’s 14” Scope - by Dana Swift & Don Bradford 8-9 Asteroid Occultation timing using the Dome Scope by Skip Whitehurst 10-11 Corner the Great Square of Pegasus by David Prosper 12 Treasurer’s Report and New Members - by John Newton 13 Club Contacts - The Healing Power of Nature - John Muir - Shared by K C Lobrecht Astronomy Club Events Check our website AstroTulsa.com events section for updates Observatory ONLY OPEN for SCHEDULED EVENTS. Click for Observatory Map We are continuing our Members ONLY Events observing nights Friday, August 6, 8:00 PM Friday, Aug 27, 7:30 PM Friday, Sept 3, 7:15 PM Friday, Sept 24, 6:45 PM Weather Backup observing nights on Saturday NOTE: If weather conditions are unfavorable or hazardous forecasts predictions our events may be postponed or cancelled. Please check our website before heading out. September General Meeting Date still to be announced The previously announced club picnic will be rescheduled for a later date Guidelines for Members’ ONLY Observatory Nights. -
The Complete Guide to Observing Lunar, Grazing and Asteroid Occultations
The Complete Guide to Observing Lunar, Grazing and Asteroid Occultations Published by the International Occultation Timing Association Richard Nugent, Editor Copyright 2007 International Occultation Timing Association, Richard Nugent, Editor. All rights reserved. This publication may be reproduced, or copied in any manner freely for one’s own personal use, but it may not be distributed or sold for money or for any other compensation. This publication is protected under the 1976 United States Copyright Act. For any other use of the publication, please contact the Editor and Publisher via email: [email protected]. While the Editor, Authors and Publisher have made their best efforts in preparing the IOTA Occultation Manual, they make no representation or warranties with respect to the accuracy and completeness regard to its contents. The Publisher, Editor and Authors specifically disclaim any implied warranties of merchantability or fitness of the material presented herein for any purpose. The advice and strategies contained herein may not be suitable for your situation and the reader and/or user assumes full responsibility for using and attempting the methods and techniques presented. Neither the publisher nor the authors shall be liable for any loss of profit or any damages, including but not limited to special, incidental, consequential, or other damages and any loss or injury. Persons are advised that occultation observations involve substantial risk and are advised to take the necessary precautions before attempting such observations. Editor in Chief: Richard Nugent Assistant Editor: Lydia Lousteaux Contributors: Trudy E. Bell, Dr. David Dunham, Dr. Joan Dunham, Paul Maley, Guy Nason, Richard Nugent, Walt “Rob” Robinson, Arvind Paranjype, Dr. -
BAA Handbook
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2020 2019 October ISSN 0068–130–X CONTENTS PREFACE . 2 HIGHLIGHTS FOR 2020 . 3 SKY DIARY . .. 4–5 CALENDAR 2020 . 6 SUN . 7–9 ECLIPSES . 10–17 APPEARANCE OF PLANETS . 18 VISIBILITY OF PLANETS . 19 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 20–21 PLANETS – Explanation of Tables . 22 ELEMENTS OF PLANETARY ORBITS . 23 MERCURY . 24–25 VENUS . 26 EARTH . 27 MOON . 27 LUNAR LIBRATION . 28 MOONRISE AND MOONSET . 30–33 SUN’S SELENOGRAPHIC COLONGITUDE . 34 LUNAR OCCULTATIONS . 35–41 GRAZING LUNAR OCCULTATIONS . 42–43 MARS . 44–45 ASTEROIDS . 46 ASTEROID EPHEMERIDES . 47–51 ASTEROID OCCULTATIONS . 52–55 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 56–58 NEO CLOSE APPROACHES TO EARTH . 59 JUPITER . .. 60–64 SATELLITES OF JUPITER . .. 64–68 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 69–78 SATURN . 79–82 SATELLITES OF SATURN . 83–86 URANUS . 87 NEPTUNE . 88 TRANS–NEPTUNIAN & SCATTERED–DISK OBJECTS . 89 DWARF PLANETS . 90–93 COMETS . 94–98 METEOR DIARY . 99–101 VARIABLE STARS (RZ Cassiopeiae; Algol; RS Canum Venaticorum) . 102–103 MIRA STARS . 104 VARIABLE STAR OF THE YEAR (SV Sagittae) . 105–107 EPHEMERIDES OF VISUAL BINARY STARS . 108–109 BRIGHT STARS . 110 ACTIVE GALAXIES . 111 TIME . 112–113 ASTRONOMICAL AND PHYSICAL CONSTANTS . 114–115 GREEK ALPHABET . 115 ACKNOWLEDGMENTS / ERRATA . 116 Front Cover: Comet 46P/Wirtanen, taken 2018 December 8 by Martin Mobberley. Equipment – Televue NP127, FLI ProLine 16803 CCD British Astronomical Association HANDBOOK FOR 2020 NINETY–NINTH YEAR OF PUBLICATION © British Astronomical Association BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 PREFACE Welcome to the 99th Handbook of the British Astronomical Association. -
University Microfilms International 300 N
ASTEROID TAXONOMY FROM CLUSTER ANALYSIS OF PHOTOMETRY. Item Type text; Dissertation-Reproduction (electronic) Authors THOLEN, DAVID JAMES. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 01/10/2021 21:10:18 Link to Item http://hdl.handle.net/10150/187738 INFORMATION TO USERS This reproduction was made from a copy of a docum(~nt sent to us for microfilming. While the most advanced technology has been used to photograph and reproduce this document, the quality of the reproduction is heavily dependent upon the quality of ti.e material submitted. The following explanation of techniques is provided to help clarify markings or notations which may ap pear on this reproduction. I. The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting through an image alld duplicating adjacent pages to assure complete continuity. 2. When an image on the film is obliterated with a round black mark, it is an indication of either blurred copy because of movement during exposure, duplicate copy, or copyrighted materials that should not have been filmed. For blurred pages, a good image of the pagt' can be found in the adjacent frame. -
Observer's Handbook 1983
EDITOR: ROY L. BISHOP THE ROYAL ASTRONOMICAL SOCIETY OF CANADA CONTRIBUTORS AND ADVISORS A l a n H. B a t t e n , Dominion Astrophysical Observatory, Victoria, BC, Canada V8X 3X3 (The Nearest Stars). R o y L. B is h o p , Department of Physics, Acadia University, Wolfville, NS, Canada B0P 1X0 (Editor). Terence Dickinson, R.R. 3, Odessa, ON, Canada K0H 2H0, (The Planets). D a v id W. D u n h a m , International Occultation Timing Association, P.O. Box 7488, Silver Spring, MD 20907, U.S.A. (Planetary Appulses and Occultations). Alan Dyer, Queen Elizabeth Planetarium, 10004-104 Ave., Edmonton, AB, Canada T5J 0K1 (Messier Catalogue, Deep-Sky Objects). M arie Fidler, Royal Astronomical Society of Canada, 124 Merton St., Toronto, ON, Canada M4S 2Z2 (Observatories and Planetaria). Victor Gaizauskas, Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Solar Activity). J o h n A. G a l t , Dominion Radio Astrophysical Observatory, Penticton, BC, Canada V2A 6K3 (Radio Sources). Ian H alliday, Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Miscellaneous Astronomical Data). H e l e n S. H o g g , David Dunlap Observatory, University of Toronto, Richmond Hill, ON, Canada L4C 4Y6 (Foreword). Yoshio Kubo, International Lunar Occultation Centre, Astronomical Division, Hydrographic Department, Tsukiji-5, Chuo-ku, Tokyo, 104 Japan (Total and Grazing Lunar Occultations). D o n a ld A. M a c R a e , David Dunlap Observatory, University of Toronto, Richmond Hill, ON, Canada L4C 4Y6 (The Brightest Stars).