Composition of the L5 Mars Trojans: Neighbors, Not Siblings
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ESO's VLT Sphere and DAMIT
ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
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. -
Accurate Positions of Pluto and Asteroids Observed in Bucharest During the Year 1932
ACCURATE POSITIONS OF PLUTO AND ASTEROIDS OBSERVED IN BUCHAREST DURING THE YEAR 1932 GHEORGHE BOCŞA, PETRE POPESCU, MIHAELA LICULESCU Astronomical Institute of the Romanian Academy Str. Cuţitul de Argint 5, 040557 Bucharest, Romania E-mail: [email protected] Abstract. The paper contains the observations of minor planets performed in Bucharest Astronomical Observatory in the year 1932 with the 380/6000 mm astrograph. Both Turner’s (constants) and Schlesinger’s (dependences) methods were used in the computation of the normal coordinates of the objects. Keywords: photographic astrometry – minor planets. 1. INTRODUCTION The article is a continuation of the complete investigation of Bucharest Wide-Field Plates Archive initiated in 2010; it contains the plates with asteroids observed in 1932. That year 185 plates were exposed and were stored in the archive, but were not reduced. After analysing them, 98 plates were detected to contain measurable minor planets. The first observed positions in this year were of planet Pluto. They were exposed on 1318cm plates, with 52 minutes exposure .The observations were performed by the famous Romanian astronomer Professor Gheorghe Demetrescu. The most difficult problem was the identification of the planet, the three plates obtained in 1932 having dozens of stars with up to 15 magnitudes. As all the observations were performed in the same month and the planet did not have a great proper motion, it was possible to superpose two plates and to identify Pluto. The values (O–C)α and (O–C)δ were calculated by M. Svechnikov from the Institute of Applied Astronomy in Sankt Petersburg on the basis of precise positions obtained in Bucharest, which we integrated in Pluto’s orbit. -
Planetary Science Institute
PLANETARY SCIENCE INSTITUTE N7'6-3qo84 (NAS A'-CR:1'V7! 3 ) ASTEROIDAL AND PLANETARY ANALYSIS Final Report (Planetary Science Ariz.) 163 p HC $6.75 Inst., Tucson, CSCL 03A Unclas G3/89 15176 i-'' NSA tiFACIWj INP BRANC NASW 2718 ASTEROIDAL AND PLANETARY ANALYSIS Final Report 11 August 1975 Submitted by: Planetary Science Institute 252 W. Ina Road, Suite D Tucson, Arizona 85704 William K. Hartmann Manager TASK 1: ASTEROID SPECTROPHOTOMETRY AND INTERPRETATION (Principal Investigator: Clark R. Chapman) A.* INTRODUCTION The asteroid research program during 1974/5 has three major goals: (1) continued spectrophotometric reconnaissance of the asteroid belt to define compositional types; (2) detailed spectrophotometric observations of particular asteroids, especially to determine variations with rotational phase, if any; and (3) synthesis of these data with other physical studies of asteroids and interpretation of the implications of physical studies of the asteroids for meteoritics and solar system history. The program has been an especially fruitful one, yielding fundamental new insights to the nature of the asteroids and the implications for the early development of the terrestrial planets. In particular, it is believed that the level of understanding of the asteroids has been reached, and sufficiently fundamental questions raised about their nature, that serious consideration should be given to possible future spacecraft missions directed to study a sample of asteroids at close range. Anders (1971) has argued that serious consideration of asteroid missions should be postponed until ground-based techniques for studying asteroids had been sufficiently exploited so that we could intelligently select appropriate asteroids for spacecraft targeting. It is clear that that point has been reached, ,and now that relatively inexpensive fly-by missions have been discovered to be possible by utilizing Venus and Earth gravity assists (Bender and Friedlander, 1975), serious planning for such missions ought to begin. -
Calgary City 1991 Sept E
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A Study of Asteroid Pole-Latitude Distribution Based on an Extended
Astronomy & Astrophysics manuscript no. aa˙2009 c ESO 2018 August 22, 2018 A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method 1 1 1 2 3 4 5 6 7 J. Hanuˇs ∗, J. Durechˇ , M. Broˇz , B. D. Warner , F. Pilcher , R. Stephens , J. Oey , L. Bernasconi , S. Casulli , R. Behrend8, D. Polishook9, T. Henych10, M. Lehk´y11, F. Yoshida12, and T. Ito12 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 4 Goat Mountain Astronomical Research Station, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA 5 Kingsgrove, NSW, Australia 6 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 7 Via M. Rosa, 1, 00012 Colleverde di Guidonia, Rome, Italy 8 Geneva Observatory, CH-1290 Sauverny, Switzerland 9 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 10 Astronomical Institute, Academy of Sciences of the Czech Republic, Friova 1, CZ-25165 Ondejov, Czech Republic 11 Severni 765, CZ-50003 Hradec Kralove, Czech republic 12 National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 17-02-2011 / Accepted 13-04-2011 ABSTRACT Context. In the past decade, more than one hundred asteroid models were derived using the lightcurve inversion method. Measured by the number of derived models, lightcurve inversion has become the leading method for asteroid shape determination. -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
Arxiv:1611.07413V1
Noname manuscript No. (will be inserted by the editor) Trojan capture by terrestrial planets Schwarz, R. · Dvorak, R. the date of receipt and acceptance should be inserted later Abstract The paper is devoted to investigate the capture of asteroids by Venus, Earth and Mars into the 1:1 mean motion resonance especially into Trojan orbits. Current theoretical studies predict that Trojan asteroids are a frequent by-product of the planet formation. This is not only the case for the outer giant planets, but also for the terrestrial planets in the inner Solar System. By using numerical integrations, we investigated the capture efficiency and the stability of the captured objects. We found out that the capture efficiency is larger for the planets in the inner Solar System compared to the outer ones, but most of the captured Trojan asteroids are not long term stable. This temporary captures caused by chaotic behaviour of the objects were investigated without any dissipative forces. They show an interesting dynamical behaviour of mixing like jumping from one Lagrange point to the other one. Keywords Trojan capture · terrestrial planets · Near Earth asteroids · 1:1 mean motion resonance 1 Introduction In February 1906, Max Wolf [38] discovered the first Trojan asteroid named 588 Achilles, after the hero of the Trojan war. Almost a century later, in 1990, the first Martian Trojan (5261 Eureka) was observed by Bowell et al. [4]. In 2001 the first Neptune Trojan was discovered by the Lowell Observatory Deep Ecliptic R. Schwarz T¨urkenschanzstrasse 17, 1180 Vienna Tel.: +43-1-427751841 Fax: +43-1-42779518 E-mail: [email protected] R. -
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Instruction Manual
® SmartStar® CubeTM-E Series Mount and Telescopes (For 8500, 8502, 8503 and 8504) Instruction Manual 1 Table of Content Table of Content .............................................................................................................. 2 1. SmarStar® CubeTM-E Series Overview ........................................................................ 4 1.1. SmartStar® CubeTM-E Series Features ................................................................ 4 1.2. Package Contents ................................................................................................ 5 1.3. Assembly Terms ................................................................................................... 6 1.4. GoToNova® 8405 Hand Controller ........................................................................ 7 1.4.1. Key Description .............................................................................................. 7 1.4.2. The LCD Screen ............................................................................................ 7 1.4.3. Check the Battery ........................................................................................... 9 2. Get Started ................................................................................................................ 10 2.1. Setup SmartStar® Cube Mount ........................................................................... 10 2.2. Get Familiar with Telescope ............................................................................... 14 2.2.1. Assemble the -
Smartstar R-80 Telescope Instruction Manual
SmartStar® R-80 Telescope Instruction Manual For product #9501-W, 9502-W, 9801-W and 9802-W www.iOptron.com 1 Table of Content Table of Content ............................................................................................................................. 2 1. SmarStar® R-80 Overview.......................................................................................................... 4 1.1. SmartStar® R-80 Features.................................................................................................... 4 1.2. SmartStar® R-80 Assembly Terms ...................................................................................... 5 2. Telescope Assembly ................................................................................................................... 6 3. GoToNova® 8405 Hand Controller ............................................................................................ 8 3.1. Key Description ................................................................................................................... 8 3.2. The LCD Screen .................................................................................................................. 8 4. Getting Started .......................................................................................................................... 10 4.1. Level and Align the Mount................................................................................................ 10 4.1.1. Level the Mount.........................................................................................................