Tribute to an Astronomer: the Work of Max Ernst on Wilhelm Tempel
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The Minor Planet Bulletin, We Feel Safe in Al., 1989)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 43, NUMBER 3, A.D. 2016 JULY-SEPTEMBER 199. PHOTOMETRIC OBSERVATIONS OF ASTEROIDS star, and asteroid were determined by measuring a 5x5 pixel 3829 GUNMA, 6173 JIMWESTPHAL, AND sample centered on the asteroid or star. This corresponds to a 9.75 (41588) 2000 SC46 by 9.75 arcsec box centered upon the object. When possible, the same comparison star and check star were used on consecutive Kenneth Zeigler nights of observation. The coordinates of the asteroid were George West High School obtained from the online Lowell Asteroid Services (2016). To 1013 Houston Street compensate for the effect on the asteroid’s visual magnitude due to George West, TX 78022 USA ever changing distances from the Sun and Earth, Eq. 1 was used to [email protected] vertically align the photometric data points from different nights when constructing the composite lightcurve: Bryce Hanshaw 2 2 2 2 George West High School Δmag = –2.5 log((E2 /E1 ) (r2 /r1 )) (1) George West, TX USA where Δm is the magnitude correction between night 1 and 2, E1 (Received: 2016 April 5 Revised: 2016 April 7) and E2 are the Earth-asteroid distances on nights 1 and 2, and r1 and r2 are the Sun-asteroid distances on nights 1 and 2. CCD photometric observations of three main-belt 3829 Gunma was observed on 2016 March 3-5. Weather asteroids conducted from the George West ISD Mobile conditions on March 3 and 5 were not particularly favorable and so Observatory are described. -
C.H.F. Peters
NATIONAL ACADEMY OF SCIENCES Ch RISTIAN HEINRIC H F RIEDRIC H PETERS A Biographical Memoir by W I L L I A M ShEE H AN Any opinions expressed in this memoir are those of the author(s) and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 1999 NATIONAL ACADEMIES PRESS WASHINGTON D.C. CHRISTIAN HEINRICH FRIEDRICH PETERS September 19, 1813–July 18, 1890 BY WILLIAM SHEEHAN N THE MID-NINETEENTH century the discovery of new aster- Ioids was still far from routine. These objects had not yet grown so numerous as to earn for themselves the contemp- tuous label later applied, “vermin of the skies,” and those who excelled in claiming the starlike wanderers from the camouflage of background stars were honored with renown. Hind, de Gasparis, Goldschmidt, Chacornac, Pogson, and Peters were foremost among the early discoverers. Even on this short list C. H. F. Peters stood out. On May 29, 1861—just weeks after the American Civil War began at Fort Sumter—Peters discovered his first aster- oid (72 Feronia). It was the fifth asteroid discovered in North America (others had been found by Ferguson and Searle). Feronia was the first of forty-eight such discoveries that made Peters the most prolific finder of minor planets of his generation, and even today he remains second only to Johann Palisa among visual discoverers of asteroids. Dur- ing his colorful career, he also compiled meticulous star charts of the zodiac, collated observations from manuscripts of Ptolemy, and embroiled himself in a series of often bitter controversies with other astronomers, notably over the ex- istence of an intra-Mercurial planet. -
Adaptive Optics and Lightcurve Data of Asteroids: Twenty Shape Models and Information Content Analysis
Astronomy & Astrophysics manuscript no. viikinkoski_2017 c ESO 2018 October 14, 2018 Adaptive optics and lightcurve data of asteroids: twenty shape models and information content analysis M. Viikinkoski1, J. Hanuš2, M. Kaasalainen1, F. Marchis3, and J. Durechˇ 2 1 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland 2 Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovickáchˇ 2, 18000 Prague, Czech Republic 3 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View CA 94043, USA Received x-x-2017 / Accepted x-x-2017 ABSTRACT We present shape models and volume estimates of twenty asteroids based on relative photometry and adaptive optics images. We discuss error estimation and the effects of myopic deconvolution on shape solutions. For further analysis of the information capacities of data sources, we also present and discuss ambiguity and uniqueness results for the reconstruction of nonconvex shapes from photometry. Key words. Instrumentation: adaptive optics – Methods: numerical, analytical – Minor planets, asteroids: general – Techniques: photometric 1. Introduction we construct shape models using both unprocessed and decon- voluted images, and compare their differences. In our previous paper (Hanuš et al. 2017b), we derived 3D shape This paper is organized as follows. In Sect. 2 we describe models for about 40 asteroids by combining disk-integrated the data reduction steps and outline the ADAM shape optimiza- photometry, adaptive optics (AO) images, and stellar occulta- 1 tion procedure. We discuss our results and comment on some tion timings by the All-Data Asteroid modelling (ADAM , Vi- of the individual asteroids in Sect. 3. We present a procedure ikinkoski et al. -
British Astronomical Association Handbook 2009
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2009 2008 October ISSN 0068-130-X CONTENTS CALENDAR 2009 . 2 PREFACE. 3 EDITOR’S NOTES REGARDING THE HANDBOOK SURVEY . 4 HIGHLIGHTS FOR 2009. 5-6 SKY DIARY FOR 2009 . 7 VISIBILITY OF PLANETS. 8 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S. 9-10 ECLIPSES . 11-14 TIME. 15-16 EARTH AND SUN. 17-19 MOON . 20 SUN’S SELENOGRAPHIC COLONGITUDE. 21 MOONRISE AND MOONSET . 22-25 & 140 LUNAR OCCULTATIONS . 26-34 GRAZING LUNAR OCCULTATIONS. 35-36 PLANETS – EXPLANATION OF TABLES. 37 APPEARANCE OF PLANETS. 38 MERCURY. 39-40 VENUS. 41 MARS. 42-43 ASTEROIDS AND DWARF PLANETS. 44-63 JUPITER . 64-67 SATELLITES OF JUPITER . 68-88 SATURN. 89-92 SATELLITES OF SATURN . 93-100 URANUS. 101 NEPTUNE. 102 COMETS. 103-114 METEOR DIARY . 115-117 VARIABLE STARS . 118-123 Algol; λ Tauri; RZ Cassiopeiae; Mira Stars; IP Pegasi EPHEMERIDES OF DOUBLE STARS . 124-125 BRIGHT STARS . 126 GALAXIES . 127-128 SUN, MOON AND PLANETS: Physical data. 129 SATELLITES (NATURAL): Physical and orbital data . 130-131 ELEMENTS OF PLANETARY ORBITS . 132 INTERNET RESOURCES. 133-134 CONVERSION FORMULAE AND ERRATA . 134 RADIO TIME SIGNALS. 135 PROGRAM AND DATA LIBRARY . 136 ASTRONOMICAL AND PHYSICAL CONSTANTS . 137-138 MISCELLANEOUS DATA AND TELESCOPE DATA . 139 GREEK ALPHABET . .. 139 Front Cover: The Crab Nebula, M1 (NGC 1952) in Taurus. Imaged in January 2008 by Andrea Tasseli from Lincoln, UK. Intes-Micro M809 8 inch (203mm) f/10 Maksutov-Cassegrain with Starlight Xpress SXV-H9 CCD and Astronomik filter set. Image = L (56x120s) and RHaGB (45x60s). -
Adaptive Optics and Lightcurve Data of Asteroids: Twenty Shape Models and Information Content Analysis
A&A 607, A117 (2017) Astronomy DOI: 10.1051/0004-6361/201731456 & c ESO 2017 Astrophysics Adaptive optics and lightcurve data of asteroids: twenty shape models and information content analysis M. Viikinkoski1, J. Hanuš2, M. Kaasalainen1, F. Marchis3, and J. Durechˇ 2 1 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland e-mail: [email protected] 2 Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovickáchˇ 2, 18000 Prague, Czech Republic 3 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View, CA 94043, USA Received 28 June 2017 / Accepted 16 August 2017 ABSTRACT We present shape models and volume estimates of twenty asteroids based on relative photometry and adaptive optics images. We discuss error estimation and the effects of myopic deconvolution on shape solutions. For further analysis of the information capacities of data sources, we also present and discuss ambiguity and uniqueness results for the reconstruction of nonconvex shapes from photometry. Key words. methods: numerical – methods: analytical – minor planets, asteroids: general – techniques: photometric – instrumenta- tion: adaptive optics 1. Introduction artifacts. To investigate the usefulness of myopic deconvolution, we construct shape models using both unprocessed and decon- In our previous paper (Hanuš et al. 2017b), we derived three- voluted images, and compare their differences. dimensional (3D) shape models for about 40 asteroids by com- This paper is organized as follows. In Sect.2 we describe bining disk-integrated photometry, adaptive optics (AO) images, the data reduction steps and outline the ADAM shape optimiza- and stellar occultation timings by the All-Data Asteroid model- 1 tion procedure. -
Answers to the Practical Questions and Problems Contained in The
m i '-p.-072.] LIEBj'LB'Y' OUT THE UNITED STATES BUREAU OF EDUCATION. Division__ Shelf_ PRESENTED BY ANSWERS^ TO THE PRACTICAL QUESTIONS AND PROBLEMS CONTAINED IN THE FOURTEEN WEEKS COURSES % 0 IN V Physiology, Philosophy, Astronomy, and Chemistry (Old and New Edition). V: V —-» BY 1883 J. DORMAN STEELE, Ph.d.0!, - > call Oi AUTHOR OF THE FOURTEEN WEEKS SERIES IN PHYSIOLOGY, PHILOSOPHY, CHEMISTRY, ASTRONOMY, AND GEOLOGY. A. S. BARNES & COMPANY, NEW YORK AND CHICAGO. THE FOURTEEN WEEKS’ COURSES IN NATURAL SCIENCE, BY J. DORMAN STEELE, A.M., Ph.D. Fourteen Weeks 115 Natural Philosophy, Fourteen Weeks ig CipenQistry^ Fourteen Weeks iq Descriptive Astroijorqy, Fourteen Weeks iij Popular Geology, Fourteen Weeks iij Human Physiology, Fourteen Weeks iq Zoology, Fourteen Weeks iq Botaqy, A Key, containing Answers to the Questions and Problems in Steele’s 14 Weeks’ Courses, 4 ^ISTORIC^L SERIES, ON THE PLAN OF STEELE’S 14 WEEKS IN THE SCIENCES. A Brief FJistory of the Uqited States, A Brief hjistory of France, The same publishers also offer the following standard scientific works, being more extended or difficult treatises than those of Prof. Steele, though still of Academic grade. Peck’s Ganot’s Natural Philosophy, Porter’s Principles of Chemistry, Jarvis’ Physiology and Laws of Health, Wood’s Botanist and Florist, Charqb&rs’ Elements of Zoology, tyclqtyre’s ^stroqomy and the Globes, Page’s Elements of Geology, Entered according to Act of Congress, in the year 1869, by A. S. BARNES & CO., In the Clerk’s Office of the District Court of the United States for the Southern District of New York. -
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A&A 551, A67 (2013) Astronomy DOI: 10.1051/0004-6361/201220701 & c ESO 2013 Astrophysics Asteroids’ physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution J. Hanuš1,J.Durechˇ 1,M.Brož1, A. Marciniak2,B.D.Warner3, F. Pilcher4, R. Stephens5,R.Behrend6, B. Carry7, D. Capekˇ 8, P. Antonini9,M.Audejean10, K. Augustesen11,E.Barbotin12, P. Baudouin13, A. Bayol11, L. Bernasconi14, W. Borczyk2, J.-G. Bosch15, E. Brochard16,L.Brunetto17,S.Casulli18, A. Cazenave12, S. Charbonnel12, B. Christophe19,F.Colas20, J. Coloma21, M. Conjat22, W. Cooney23, H. Correira24,V.Cotrez25, A. Coupier11, R. Crippa26, M. Cristofanelli17,Ch.Dalmas11, C. Danavaro11, C. Demeautis27,T.Droege28,R.Durkee29, N. Esseiva30, M. Esteban11, M. Fagas2,G.Farroni31,M.Fauvaud12,32,S.Fauvaud12,32, F. Del Freo11,L.Garcia11,S.Geier33,34, C. Godon11, K. Grangeon11,H.Hamanowa35,H.Hamanowa35,N.Heck20, S. Hellmich36, D. Higgins37, R. Hirsch2, M. Husarik38,T.Itkonen39,O.Jade11,K.Kaminski´ 2,P.Kankiewicz40,A.Klotz41,42,R.A.Koff43, A. Kryszczynska´ 2, T. Kwiatkowski2,A.Laffont11,A.Leroy12, J. Lecacheux44, Y. Leonie11,C.Leyrat44,F.Manzini45, A. Martin11, G. Masi11, D. Matter11, J. Michałowski46,M.J.Michałowski47, T. Michałowski2, J. Michelet48, R. Michelsen11, E. Morelle49, S. Mottola36,R.Naves50,J.Nomen51,J.Oey52,W.Ogłoza53, A. Oksanen49, D. Oszkiewicz34,54, P. Pääkkönen39,M.Paiella11, H. Pallares11,J.Paulo11,M.Pavic11, B. Payet11,M.Polinska´ 2, D. Polishook55, R. Poncy56,Y.Revaz57,C.Rinner31, M. Rocca11,A.Roche11,D.Romeuf11,R.Roy58, H. Saguin11,P.A.Salom11, S. -
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. -
The Minor Planet Bulletin, 30(3), Pp
1 THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 31, NUMBER 1, A.D. 2004 JANUARY-MARCH 1. ASTROMETRIC PROGRAM FOR JR refers to asteroids nearby to the 3:1 mean motion resonance NEAR-EARTH OBJECT SOURCES with Jupiter, MC are the Mars Crossers, NU are objects in the ν 6 secular resonance. Sergio Foglia UAI Minor Planets Section Recorder References F. Bisleri 11, I-20148 Milano, Italy € [email protected] Morbidelli et. al. (2003). Understanding the distribution on Near Earth Objects. http://www.obs-nice.fr/morby/ESA/ esa.html (Received: 24 September Revised: 6 October) MPC Orbit Database. ftp://ftp-cfa.harvard.edu/pub/MPCORB/ 2003 Sep. 17, Minor Planet Center A new astroometric program is proposed for asteroids located in likely source regions supplying the near-Earth Proper Elements of Minor Planets. http://hamilton.dm object population. .unipi.it/astdys/ 2003 Sep. 17, Asteroid Dynamic Site According to Morbidelli et al. (2003), near-Earth objects (NEOs) come mainly from 5 sources with the following contributions to the population: the ν 6 resonance region at the inner border of the asteroid main belt (37 ± 8 %), the 3:1 resonance region in the middle of the asteroid main belt (23 ± 8 %), the Intermediate Mars-Crossing (IMC) population (25 ± 3 %), the Outer Belt (OB) population€ (8 ± 1 %), and the population of dormant Jupiter Family Comets (JFC) (6 ± 4 %). Astrometric measurements of objects in these source regions would be very useful to increase knowledge about the NEO source population and solar system dynamics. -
Arxiv:1308.0446V1 [Astro-Ph.EP] 2 Aug 2013
Sizes of main-belt asteroids by combining shape models and Keck adaptive aptics observations J. Hanuˇsa,∗, F. Marchisb, J. Durechˇ a aAstronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holeˇsoviˇck´ach 2, 180 00 Prague, Czech Republic. bSETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View CA 94043, USA Abstract We select 50 main-belt asteroids with a diameter between 20 and 400 km for which we have (i) shape models derived by the lightcurve inversion method (LI) and (ii) resolved observations of good quality collected with the Keck II adaptive optics (AO) system in the near-infrared. We derive the size of these asteroids by minimizing the difference between the contours from deconvolved AO images and the projected silhouettes calculated from the shape model at the time of the AO observations. We compute the volume-equivalent diameters for 48 of these asteroids. For 15 of them, we remove the ambiguity of the pole orientation typical for shape models derived by the LI. We have found that our equivalent diameters are smaller by 3%, 7%, and 2% compared with the effective diameters derived from mid-IR photometric observations provided by IRAS, WISE and AKARI. For 40 asteroids with previously determined mass estimates, we compute their bulk densities and discuss the mass–density dependence with respect to taxonomic types. Keywords: asteroids, adaptive optics, photometry, asteroids, composition 1. Introduction An important physical characteristic of an asteroid is its size. The measurement of an asteroid size in combination with its mass, allows us to directly compute the average density, and thus estimate its composition and the structure of its interior. -
Ny8-29012 PRECEDING PAGE BLANK NOT FILMED
Ny8-29012 PRECEDING PAGE BLANK NOT FILMED PHYSICAL OBSERVATIONS AND TAXONOMY OF ASTEROIDS DAVID MORRISON NASA Headquarter:j Wraohington, DC 20546 Since 1970 the physical study of asteroids has been dramat- ically extended 3y wide application of four types of observa- tions: spectrophotometry from 0.3 to 1.1 vm; broad-band UBV photometry; visible photopolarimetry; and broad-band therrrlal radiometry. More than a quzrter of the numbered asteroids have been studied with these techniques, and for most of them the data are adequate to determine approximate size and al- bedo and to provide a rough classification related to mineral- ogical composition. The specific CSM taxonomic system of Chapman et al. (1975) and Bowel1 et al. (1978) is described and used to organize these new data. The CSM taxonomy is also compared with more composi tional ly spe~ific taxonomies, and some future directions for both observation alld classification are indicated. INTRODUCTION During the relatively brief span of years from the Tucson Asteroid Conferer~~e (Gehrels, 1971) to the present, there has been explosive growth in observational data on asteroids. During the first half of the 20th century and well into the 19601s, asteroid science had been limited a!most entirely to searches for new objects and estau: :,hment of photographic magnitudes and accurate orbital elements for the fewer than 2000 steroids that were nared and numbered. During the 19601s, the first major efforts to accumulate more physical data (photoelectric magnitudes and lightcurves, with some co:orimetric and polarimetric work) were undertaken, oric;rilv by G. P. Ku~perand T. -
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A&A 514, A96 (2010) Astronomy DOI: 10.1051/0004-6361/200913346 & c ESO 2010 Astrophysics A ring as a model of the main belt in planetary ephemerides P. Kuchynka1, J. Laskar1,A.Fienga1,2, and H. Manche1 1 Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] 2 Observatoire de Besançon-CNRS UMR6213, 41 bis avenue de l’Observatoire, 25000 Besançon, France Received 24 September 2009 / Accepted 4 February 2010 ABSTRACT Aims. We assess the ability of a solid ring to model a global perturbation induced by several thousands of main-belt asteroids. Methods. The ring is first studied in an analytical framework that provides an estimate of all the ring’s parameters excepting mass. In the second part, numerically estimated perturbations on the Earth-Mars, Earth-Venus, and Earth-Mercury distances induced by various subsets of the main-belt population are compared with perturbations induced by a ring. To account for large uncertainties in the asteroid masses, we obtain results from Monte Carlo experiments based on asteroid masses randomly generated according to available data and the statistical asteroid model. Results. The radius of the ring is analytically estimated at 2.8 AU. A systematic comparison of the ring with subsets of the main belt shows that, after removing the 300 most perturbing asteroids, the total main-belt perturbation of the Earth-Mars distance reaches on average 246 m on the 1969−2010 time interval. A ring with appropriate mass is able to reduce this effect to 38 m.