Taking the Bull by the 'Horns'
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The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated. -
(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. -
Do Slivan States Exist in the Flora Family? A
Do Slivan states exist in the Flora family? A. Kryszczyńska, F. Colas, M. Polińska, R. Hirsch, V. Ivanova, G. Apostolovska, B. Bilkina, F. Velichko, T. Kwiatkowski, P. Kankiewicz, et al. To cite this version: A. Kryszczyńska, F. Colas, M. Polińska, R. Hirsch, V. Ivanova, et al.. Do Slivan states exist in the Flora family?. Astronomy and Astrophysics - A&A, EDP Sciences, 2012, 546, pp.A72. 10.1051/0004- 6361/201219199. hal-03123875 HAL Id: hal-03123875 https://hal.archives-ouvertes.fr/hal-03123875 Submitted on 28 Jan 2021 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. A&A 546, A72 (2012) Astronomy DOI: 10.1051/0004-6361/201219199 & c ESO 2012 Astrophysics Do Slivan states exist in the Flora family? I. Photometric survey of the Flora region A. Kryszczynska´ 1,F.Colas2,M.Polinska´ 1,R.Hirsch1, V. Ivanova3, G. Apostolovska4, B. Bilkina3, F. P. Velichko5, T. Kwiatkowski1,P.Kankiewicz6,F.Vachier2, V. Umlenski3, T. Michałowski1, A. Marciniak1,A.Maury7, K. Kaminski´ 1, M. Fagas1, W. Dimitrov1, W. Borczyk1, K. Sobkowiak1, J. Lecacheux8,R.Behrend9, A. Klotz10,11, L. Bernasconi12,R.Crippa13, F. Manzini13, R. -
Investigating Taxonomic Diversity Within Asteroid Families Through ATLAS Dual-Band Photometry
Draft version February 20, 2020 Typeset using LATEX twocolumn style in AASTeX62 Investigating Taxonomic Diversity within Asteroid Families through ATLAS Dual-Band Photometry N. Erasmus,1 S. Navarro-Meza,2, 3 A. McNeill,3 D. E. Trilling,3, 1 A. A. Sickafoose,1, 4, 5 L. Denneau,6 H. Flewelling,6 A. Heinze,6 and J. L. Tonry6 1South African Astronomical Observatory, Cape Town, 7925, South Africa. 2Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Ensenada B.C. 22860, Mexico. 3Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86001, USA. 4Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA. 5Planetary Science Institute, Tucson, AZ 85719-2395, USA 6Institute for Astronomy, University of Hawaii, Honolulu, HI 9682, USA. ABSTRACT We present here the c-o colors for identified Flora, Vesta, Nysa-Polana, Themis, and Koronis family members within the historic data set (2015-2018) of the Asteroid Terrestrial-impact Last Alert System (ATLAS). The Themis and Koronis families are known to be relatively pure C- and S-type Bus- DeMeo taxonomic families, respectively, and the extracted color data from the ATLAS broadband c- and o-filters of these two families is used to demonstrate that the ATLAS c-o color is a sufficient parameter to distinguish between the C- and S-type taxonomies. The Vesta and Nysa-Polana families are known to display a mixture of taxonomies possibly due to Vesta's differentiated parent body origin and Nysa-Polana actually consisting of two nested families with differing taxonomies. Our data show that the Flora family also displays a large degree of taxonomic mixing and the data reveal a substantial H-magnitude dependence on color. -
The Minor Planet Bulletin Lost a Friend on Agreement with That Reported by Ivanova Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 3, A.D. 2006 JULY-SEPTEMBER 49. LIGHTCURVE ANALYSIS FOR 19848 YEUNGCHUCHIU Kwong W. Yeung Desert Eagle Observatory P.O. Box 105 Benson, AZ 85602 [email protected] (Received: 19 Feb) The lightcurve for asteroid 19848 Yeungchuchiu was measured using images taken in November 2005. The lightcurve was found to have a synodic period of 3.450±0.002h and amplitude of 0.70±0.03m. Asteroid 19848 Yeungchuchiu was discovered in 2000 Oct. by the author at Desert Beaver Observatory, AZ, while it was about one degree away from Jupiter. It is named in honor of my father, The amplitude of 0.7 magnitude indicates that the long axis is Yeung Chu Chiu, who is a businessman in Hong Kong. I hoped to about 2 times that of the shorter axis, as seen from the line of sight learn the art of photometry by studying the lightcurve of 19848 as at that particular moment. Since both the maxima and minima my first solo project. have similar “height”, it’s likely that the rotational axis was almost perpendicular to the line of sight. Using a remote 0.46m f/2.8 reflector and Apogee AP9E CCD camera located in New Mexico Skies (MPC code H07), images of Many amateurs may have the misconception that photometry is a the asteroid were obtained on the nights of 2005 Nov. 20 and 21. very difficult science. After this learning exercise I found that, at Exposures were 240 seconds. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
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. -
Honolulu, Hawaii 96822 Jan
UNIVERSITY OF HAWAII INSTITlJTE FOR ASTRONOMY 2680 Woodlawn Drive Honolulu, Hawaii 96822 NASA GRANT NGL 12-001-57 SEHIAlWUAL PROGRESS REPORTS #32 and #33 Dale P. Cruikshank, Principal Investigator N87-2 17 t 3 (NASWX-I~O~ 13) BESEARCB SB ELANETABY ZIUDIES ANI: OPEEA1lObl CP TBE FAOX& %EA Unclas CESEBVATORY SePiiannual Praqress Heport, Jan. - Dec. 1965 (Hauaii Univ., Honolulu.)CSCL 038 G3/89 43361 9s p For the Period January-December 1986 I TABLE OF CONTENTS Page I . PERSONNEL ........................................................... 1 I1 . THE RESEARCH PROGRAMS ............................................... 2 A . Highlights ...................................................... 2 B . The Major Planets ............................................... 3 C . Planetary Satellites and Rings .................................. 23 D . Asteroids ....................................................... 50 E . Comets .......................................................... 62 F . Laboratory Studies of Dark Organic Materials .................... 70 G . Theoretical and Analytical Studies: Thermal Inertias and Thermal Conductivities of Particulate Media ................. 72 H . Extrasolar Planetary Material: The Search for Dark Companions of K and M Giants ............................... 77 I11 . OPERATION OF THE 2.2-METER TELESCOPE ................................ 79 IV . PAPERS PUBLISHED OR SUBMITTED FOR PUBLICATION IN 1986 ............... 84 ATTACHMENT: "Albedo Maps of Comets P/Giacobini-Zinner and P/Halley." Hammel et a1 ....................................... -
An Anisotropic Distribution of Spin Vectors in Asteroid Families⋆
A&A 559, A134 (2013) Astronomy DOI: 10.1051/0004-6361/201321993 & c ESO 2013 Astrophysics An anisotropic distribution of spin vectors in asteroid families J. Hanuš1,M.Brož1,J.Durechˇ 1,B.D.Warner2, J. Brinsfield3,R.Durkee4, D. Higgins5,R.A.Koff6,J.Oey7, F. Pilcher8, R. Stephens9,L.P.Strabla10,Q.Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, ACT 2913 Ngunnawal, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), 25020 Brescia, Italy Received 30 May 2013 / Accepted 16 September 2013 ABSTRACT Context. The current number of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study the spin-vector properties of not only the whole population of main-belt asteroids, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the hierarchical clustering method (HCM) as members of ten col- lisional families, among which are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes. -
Thermophysical Modeling of Main-Belt Asteroids from WISE Thermal Data
Thermophysical modeling of main-belt asteroids from WISE thermal data a, b a c J. Hanuˇs ∗, M. Delbo’ , J. Durechˇ , V. Al´ı-Lagoa aAstronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic bUniversit´eCˆote d’Azur, CNRS–Lagrange, Observatoire de la Cˆote d’Azur, CS 34229 – F 06304 NICE Cedex 4, France cMax-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany Abstract By means of a varied-shape thermophysical model of Hanusˇ et al. (2015, Icarus, Volume 256) that takes into account asteroid shape and pole uncertainties, we analyze the thermal infrared data acquired by the NASA’s Wide-field Infrared Survey Explorer of about 300 asteroids with derived convex shape models. We utilize publicly available convex shape models and rotation states as input for the thermophysical modeling. For more than one hundred asteroids, the thermophysical modeling gives us an acceptable fit to the thermal infrared data allowing us to report their thermophysical properties such as size, thermal inertia, surface roughness or visible geometric albedo. This work more than doubles the number of asteroids with determined thermophysical properties, especially the thermal inertia. In the remaining cases, the shape model and pole orientation uncertainties, specific rotation or thermophysical properties, poor thermal infrared data or their coverage prevent the determination of reliable thermophysical properties. Finally, we present the main results of the statistical study of derived thermophysical parameters within the whole population of main-belt asteroids and within few asteroid families. Our sizes based on TPM are, in average, consistent with the radiometric sizes reported by Mainzer et al. -
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. -
Do Slivan States Exist in the Flora Family? I
A&A 546, A72 (2012) Astronomy DOI: 10.1051/0004-6361/201219199 & c ESO 2012 Astrophysics Do Slivan states exist in the Flora family? I. Photometric survey of the Flora region A. Kryszczynska´ 1,F.Colas2,M.Polinska´ 1,R.Hirsch1, V. Ivanova3, G. Apostolovska4, B. Bilkina3, F. P. Velichko5, T. Kwiatkowski1,P.Kankiewicz6,F.Vachier2, V. Umlenski3, T. Michałowski1, A. Marciniak1,A.Maury7, K. Kaminski´ 1, M. Fagas1, W. Dimitrov1, W. Borczyk1, K. Sobkowiak1, J. Lecacheux8,R.Behrend9, A. Klotz10,11, L. Bernasconi12,R.Crippa13, F. Manzini13, R. Poncy14, P. Antonini15, D. Oszkiewicz16,17, and T. Santana-Ros1 1 Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznan,´ Poland e-mail: [email protected] 2 Institut de Mécanique Céleste et Calcul des Éphémérides, Observatoire de Paris, 77 Av. Denfert Rochereau, 75014 Paris, France 3 Institute of Astronomy, Bulgarian Academy of Sciences Tsarigradsko Chausse 72, 1784 Sofia, Bulgaria 4 Faculty of Natural Sciences, Cyril and Methodius University Skopje, Macedonia 5 Institute of Astronomy, Karazin National University, Kharkov, Ukraine 6 Astrophysics Division, Institute of Physics, Jan Kochanowski University, Swietokrzyska´ 15, 25-406 Kielce, Poland 7 San Pedro de Atacama Observatory, Chile 8 Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France 9 Geneva Observatory, 1290 Sauverny, Switzerland 10 Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, 9 avenue du colonel Roche, 31028 Toulouse Cedex 4, France 11 Observatoire