DOCSLIB.ORG

Asteroid Spin Axes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Asteroid Spin Axes ASTEROID SPIN AXES Asteroid Q Period Amp L1 B1 L2 B2 L3 B3 L4 B4 Sid. period Mod Reference 1 Ceres 3 9.074170 0.06 332.0 +70.0 N Saint-Pe, 93 298.0 +78.0 186.6 −58.0 N Drummond, 98 3 322.0 +78.0 N Thomas, 05 352.0 +80.0 N Drummond, 08 346.0 +82.0 N Drummond, 14 2 Pallas 3 7.8132 0.16 228.0 +43.0 7.8106 N Schroll, 76 211.0 +38.0 N Burchi, 83 200.0 +40.0 220.0 +15.0 N Binzel, 84 44.0 +4.0 148.0 +55.0 224.0 −4.0 328.0 −55.0 N Zappala, 84 49.0 +6.0 157.0 +53.0 229.0 −6.0 337.0 −53.0 N Burchi, 85 54.0 −6.0 7.813 N Magnusson, 86 100.0 −22.0 295.0 +16.0 Y Drummond, 89 70.0 +15.0 250.0 +15.0 70.0 −15.0 250.0 −15.0 Y Drummond, 89 3 193.0 +43.0 35.0 −12.0 7.813224 Y Torppa, 03 32.0 −21.0 N Drummond, 08 3 35.6 −12.6 193.1 +44.2 7.813225 Y Higley, 08 2 34.0 −27.0 Y Drummond, 09 3 30.0 −16.0 Y Carry, 10 3 35.0 −12.0 7.81323 N Durech, 11 3 Juno 3 7.210 0.22 71.0 +49.0 7.213 N Chang, 62 101.0 +29.0 321.0 +57.0 141.0 −57.0 281.0 −29.0 Y Zappala, 84 110.0 +40.0 7.210 N Magnusson, 86 104.0 +36.0 316.0 +62.0 7.209526 N Birch, 89 108.0 +34.0 7.20953 Y Erikson, 93 108.0 +38.0 7.20953 Y Dotto, 95 3 103.0 +27.0 7.209531 Y Kaasalainen, 02 118.0 +30.0 N Drummond, 08 3 103.0 +27.0 7.209531 N Durech, 11 103.0 +22.0 7.20953091 Y Viikinkoski, 15 104.0 +20.0 7.209532 Hanus, 16 4 Vesta 3 5.342 0.19 14.0 +80.0 5.3448 N Cailliate, 56 10.689 Y Haupt, 58 57.0 +74.0 5.34212 N Chang, 62 126.0 +65.0 5.342129 N Gehrels, 67 139.0 +47.0 333.0 +39.0 10.6824 N Taylor, 73 103.0 +43.0 301.0 +33.0 5.34213 N Taylor, 85 120.0 +65.0 325.0 +55.0 5.342124 Y Magnusson, 86 85.0 +58.0 310.0 +60.0 Y Cellino, 87 336.0 +55.0 5.3421 Y Drummond, 88 311.0 +67.0 Y Drummond, 89 160.0 +52.0 340.0 +40.0 5.3421 N Reynoldson, 93 343.0 +56.0 Y McCarthy, 94 336.0 +63.0 Y Thomas, 97 321.0 +62.0 Y Drummond, 98 341.0 +51.0 N Drummond, 08 325.0 +55.0 N Drummond, 08 304.5 +41.5 N Li, 11 3 5.34212767 Y Russell, 12 5∗Astraea 3 16.806 0.27 328.0 −9.0 16.8121 Taylor, 78 131.0 +49.0 328.0 +46.0 148.0 −46.0 310.0 −49.0 Y Zappala, 86 125.0 +46.0 318.0 +44.0 16.8006 Y Erikson, 93 114.0 +57.0 16.8006 Y De Angelis, 95 312.0 +58.0 132.0 −58.0 Y Blanco, 00 115.0 +55.0 310.0 +55.0 16.8006 Y Lopez-Gonzalez, 05 3 123.8 +49.7 16.800828 Y Higley, 08 4 126.0 +40.0 310.0 +44.0 16.80061 Y Durech, 09 3 16.8061 N Durech, 11 2 126.0 +40.0 16.80061 N Hanus, 13 6 Hebe 3 7.2745 0.21 145.0 +15.0 N Gehrels, 62 355.0 +50.0 7.27445 Y Gehrels, 77 130.0 +33.0 344.0 +30.0 164.0 −30.0 310.0 −33.0 Y Zappala, 84 355.0 +50.0 7.27446 Y Magnusson, 86 353.0 +60.0 7.27446 N Michalowski, 88 353.0 +24.0 7.27446 Y Dotto, 95 355.0 +27.0 7.27446 Y De Angelis, 95 128.0 +30.0 308.0 −30.0 Y Blanco, 00 339.0 +45.0 7.2744696 Y Torppa, 03 3 340.0 +42.0 7.274471 N Durech, 11 340.0 +42.0 7.274471 N Hanus, 13 7 Iris 3 7.139 0.29 184.0 +55.0 7.12285 Y Cailliate, 56 193.0 +15.0 13.0 −15.0 N Gehrels, 62 11.0 +41.0 191.0 +15.0 7.135 Y Taylor, 77 15.0 +25.0 195.0 +15.0 7.138847 Y Magnusson, 86 18.0 +33.0 193.0 +16.0 13.0 −16.0 198.0 −33.0 Y Zappala, 86 – 7334 – ASTEROID SPIN AXES Asteroid Q Period Amp L1 B1 L2 B2 L3 B3 L4 B4 Sid. period Mod Reference (continuation) 15.0 +25.0 N Mitchell, 95 8.0 +35.0 187.0 +5.0 7.138847 Y De Angelis, 95 2 20.0 +10.0 7.138841 Y Kaasalainen, 02 2+ 15.0 +25.0 7.1388 Y Ostro, 10 2 20.0 +14.0 199.0 −2.0 N Durech, 11 16.0 +15.0 196.0 +2.0 7.138843 N Hanus, 13 19.0 +19.0 198.0 +5.0 7.138843 Hanus, 16 8 Flora 3 12.865 0.11 157.0 +10.0 N Gehrels, 62 148.0 +45.0 328.0 +45.0 148.0 −45.0 328.0 −45.0 Y Hollis, 87 135.0 +43.0 327.0 +32.0 147.0 −32.0 315.0 −43.0 Y Di Martino, 89 139.0 +14.0 319.0 −14.0 Y De Angelis, 95 2 122.0 +37.0 302.0 −37.0 Y Blanco, 98 2 155.0 +5.0 333.0 −2.0 12.799008 Y Torppa, 03 2 335.0 −5.0 155.0 +6.0 N Durech, 11 3 155.0 +6.0 335.0 −5.0 12.86667 Y Durech, 11w 335.0 −5.0 155.0 +6.0 12.86667 N Hanus, 13 9∗Metis 3 5.079 0.32 348.0 +76.0 168.0 −76.0 N Chang, 62 156.0 +15.0 336.0 −15.0 N Gehrels, 62 191.0 +56.0 21.0 −56.0 5.04 Y Zappala, 79 186.0 +43.0 2.0 +26.0 182.0 −26.0 6.0 −43.0 Y Zappala, 84 183.0 +25.0 1.0 +9.0 5.0791776 Y Drummond, 88 180.0 +30.0 0.0 +20.0 5.07917 Y Magnusson, 90 181.0 +23.0 0.0 +7.0 5.07918 Y Drummond, 91 185.0 +31.0 5.07918 Y De Angelis, 95 4 181.0 +23.0 359.0 +9.0 5.0791800 Y Torppa, 03 4 180.0 +21.0 5.079176 Y Marchis, 06 3 180.0 +22.0 5.079176 N Durech, 11 4 5.079176 Y Durech, 11w 176.0 +20.0 N Drummond, 12 180.0 +22.0 N Hanus, 13 10 Hygiea 3 27.630 0.33 112.0 −41.0 299.0 −39.0 27.65909 Y Michalowski, 91 100.0 −34.0 285.0 −34.0 27.62326 N Erikson, 93 2 117.0 −37.0 304.0 −35.0 27.62345 Y Michalowski, 93 113.0 −38.0 300.0 −37.0 27.62333 Y Michalowski, 95 2 118.0 +44.0 298.0 −44.0 302.0 −42.0 102.0 +42.0 Y Blanco, 98 120.0 +34.0 295.0 +43.0 27.62321 Y Lopez-Gonzalez, 00 3 115.0 −30.0 300.0 −30.0 27.62321 Y Kaasalainen, 02 2 122.0 −44.0 312.0 −42.0 27.6591 N Hanus, 11 2 122.0 −44.0 312.0 −42.0 27.65905 N Durech, 11 312.0 −42.0 122.0 −44.0 27.6591 N Hanus, 13 11 Parthenope 3 13.7204 0.12 2 73.0 −51.0 253.0 +51.0 64.0 +38.0 244.0 −38.0 Y Blanco, 98 2 165.0 +15.0 345.0 +15.0 13.7286 Y Stephens, 08 311.0 +14.0 128.0 +14.0 13.72205 N Hanus, 13 12 Victoria 3 8.6599 0.42 242.0 +17.0 62.0 −17.0 8.654 N Tempesti, 69 9.0 +55.0 176.0 +40.0 8.660796 Y Dotto, 95 3 137.0 +55.0 8.6599 Y Torppa, 03 174.0 −17.0 8.66034 Hanus, 16 13∗Egeria 3 7.045 0.37 103.0 +13.0 283.0 −13.0 Y Blanco, 00 2 44.0 +21.0 238.0 +11.0 7.04667 N Hanus, 11 14 Irene 3 15.028 0.16 2 90.0 −34.0 270.0 +34.0 Y Blanco, 98 2 97.0 −22.0 268.0 −24.0 15.02991 N Hanus, 11 95.0 −11.0 15.02986 N Hanus, 13 15∗Eunomia 3 6.083 0.53 R 6.08275 N Groeneveld, 54 2 337.0 −82.0 6.08275 Y Cailliate, 56 R −90.0 6.08275 N Van Houten-Groeneveld, 58 2 70.0 −74.0 6.08275 N Cailliate, 60 R −90.0 6.0806 N Scaltriti, 75 P 6.0806 N Lupishko, 85 2 164.0 +52.0 344.0 −52.0 170.0 +57.0 350.0 −57.0 Y Piironen, 85 2 171.0 +61.0 286.0 +73.0 6.082753 Y Magnusson, 86 N Michalowski, 88 3− 82.0 −78.0 352.0 −61.0 6.082753 Y Drummond, 88 3− 108.0 −74.0 350.0 −59.0 6.083 Y Magnusson, 90 3− 106.0 −73.0 6.082753 Y Drummond, 91 3− 96.0 −63.0 6.082753 N De Angelis, 92 R N Krugly, 92 2 102.0 −76.0 354.0 −57.0 6.082755 Y Michalowski, 93 3− 106.0 −73.0 6.082753 Y De Angelis, 95 3 3.0 −67.0 6.082752 Y Kaasalainen, 02 6.0827 N Nathues, 05 3.0 −67.0 6.082753 N Hanus, 13 – 7335 – ASTEROID SPIN AXES Asteroid Q Period Amp L1 B1 L2 B2 L3 B3 L4 B4 Sid.
Load more

Recommended publications
  • 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.
    [Show full text]
  • The Handbook of the British Astronomical Association
    THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2012 Saturn’s great white spot of 2011 2011 October ISSN 0068-130-X CONTENTS CALENDAR 2012 . 2 PREFACE. 3 HIGHLIGHTS FOR 2012. 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS. 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S. 7-8 ECLIPSES . 9-15 TIME. 16-17 EARTH AND SUN. 18-20 MOON . 21 SUN’S SELENOGRAPHIC COLONGITUDE. 22 MOONRISE AND MOONSET . 23-27 LUNAR OCCULTATIONS . 28-34 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. 44-60 JUPITER . 61-64 SATELLITES OF JUPITER . 65-79 SATURN. 80-83 SATELLITES OF SATURN . 84-87 URANUS. 88 NEPTUNE. 89 COMETS. 90-96 METEOR DIARY . 97-99 VARIABLE STARS . 100-105 Algol; λ Tauri; RZ Cassiopeiae; Mira Stars; eta Geminorum EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 INTERNET RESOURCES. 110-111 GREEK ALPHABET. 111 ERRATA . 112 Front Cover: Saturn’s great white spot of 2011: Image taken on 2011 March 21 00:10 UT by Damian Peach using a 356mm reflector and PGR Flea3 camera from Selsey, UK. Processed with Registax and Photoshop. British Astronomical Association HANDBOOK FOR 2012 NINETY-FIRST YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 2 CALENDAR 2012 January February March April May June July August September October November December Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day of of of of of of of of of of of of of of of of of of of of of of of of of Month Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year 1 Sun.
    [Show full text]
  • Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations ⇑ Petr Pravec A, , Alan W
    Icarus 221 (2012) 365–387 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations ⇑ Petr Pravec a, , Alan W. Harris b, Peter Kušnirák a, Adrián Galád a,c, Kamil Hornoch a a Astronomical Institute, Academy of Sciences of the Czech Republic, Fricˇova 1, CZ-25165 Ondrˇejov, Czech Republic b 4603 Orange Knoll Avenue, La Cañada, CA 91011, USA c Modra Observatory, Department of Astronomy, Physics of the Earth, and Meteorology, FMFI UK, Bratislava SK-84248, Slovakia article info abstract Article history: We obtained estimates of the Johnson V absolute magnitudes (H) and slope parameters (G) for 583 main- Received 27 February 2012 belt and near-Earth asteroids observed at Ondrˇejov and Table Mountain Observatory from 1978 to 2011. Revised 27 July 2012 Uncertainties of the absolute magnitudes in our sample are <0.21 mag, with a median value of 0.10 mag. Accepted 28 July 2012 We compared the H data with absolute magnitude values given in the MPCORB, Pisa AstDyS and JPL Hori- Available online 13 August 2012 zons orbit catalogs. We found that while the catalog absolute magnitudes for large asteroids are relatively good on average, showing only little biases smaller than 0.1 mag, there is a systematic offset of the cat- Keywords: alog values for smaller asteroids that becomes prominent in a range of H greater than 10 and is partic- Asteroids ularly big above H 12. The mean (H H) value is negative, i.e., the catalog H values are Photometry catalog À Infrared observations systematically too bright.
    [Show full text]
  • 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) ..................
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 3, A.D. 2007 JULY-SEPTEMBER 53. CCD PHOTOMETRY OF ASTEROID 22 KALLIOPE Kwee, K.K. and von Woerden, H. (1956). Bull. Astron. Inst. Neth. 12, 327 Can Gungor Department of Astronomy, Ege University Trigo-Rodriguez, J.M. and Caso, A.S. (2003). “CCD Photometry 35100 Bornova Izmir TURKEY of asteroid 22 Kalliope and 125 Liberatrix” Minor Planet Bulletin [email protected] 30, 26-27. (Received: 13 March) CCD photometry of asteroid 22 Kalliope taken at Tubitak National Observatory during November 2006 is reported. A rotational period of 4.149 ± 0.0003 hours and amplitude of 0.386 mag at Johnson B filter, 0.342 mag at Johnson V are determined. The observation of 22 Kalliope was made at Tubitak National Observatory located at an elevation of 2500m. For this study, the 410mm f/10 Schmidt-Cassegrain telescope was used with a SBIG ST-8E CCD electronic imager. Data were collected on 2006 November 27. 305 images were obtained for each Johnson B and V filters. Exposure times were chosen as 30s for filter B and 15s for filter V. All images were calibrated using dark and bias frames Figure 1. Lightcurve of 22 Kalliope for Johnson B filter. X axis is and sky flats. JD-2454067.00. Ordinate is relative magnitude. During this observation, Kalliope was 99.26% illuminated and the phase angle was 9º.87 (Guide 8.0). Times of observation were light-time corrected.
    [Show full text]
  • Download Full Issue
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 47, NUMBER 1, A.D. 2020 JANUARY-MARCH 1. SECTION NEWS: COLLABORATIVE ASTEROID PHOTOMETRY FOR STAFFING CHANGES FOR ASTEROID 2051 CHANG THE MINOR PLANET BULLETIN Alessandro Marchini Frederick Pilcher Astronomical Observatory, DSFTA - University of Siena (K54) Minor Planets Section Recorder Via Roma 56, 53100 - Siena, ITALY [email protected] [email protected] One staffing change and one staffing addition for The Minor Planet Bulletin are announced effective with this issue. Riccardo Papini, Massimo Banfi, Fabio Salvaggio Wild Boar Remote Observatory (K49) MPB Distributor Derald Nye is now retired from his 37 years of San Casciano in Val di Pesa (FI), ITALY service to the Minor Planets Bulletin. Derald stepped in to service at the time the MPB made its transition from the original Editor Melissa N. Hayes-Gehrke, Eric Yates and Section founder, Richard G. Hodgson. As Derald reflected in Department of Astronomy, University of Maryland a short essay written in MPB 40, page 53 (2013), the Distributor College Park, MD, USA 20740 position was the longest job he ever held, having retired from being a programmer for 30 years with IBM. (Work for IBM (Received: 2019 October 15) included programming for the space program.) At its peak, Derald was managing nearly 200 subscriptions. That number dropped to Photometric observations of this main-belt asteroid were the dozen or so libraries maintaining a permanent collection conducted in order to determine its rotation period. The following the MPB transitioning to becoming an on-line electronic authors found a synodic rotation period of 12.013 ± journal with limited printing.
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 39, NUMBER 4, A.D. 2012 OCTOBER-DECEMBER 203. 8077 HOYLE: A SHORT PERIOD ASTEROID 2.7454 ± 0.0002 h with an amplitude of 0.20 ± 0.02 mag. While there is a fair amount of scatter in the individual data points, when Daniel A. Klinglesmith III, Ethan Risley, combined they produce a well-determined period, which was Janek Turk, Angelica Vargas found by using an 8th order fit in the FALC analysis algorithm Etscorn Campus Observatory, New Mexico Tech (Harris et al., 1989). 101 East Road Socorro, NM USA 87801 Acknowledgements [email protected] The Etscorn Campus Observatory operations are supported by the Xianming L. Han, Orry R. Heffner, Adam W. Kidd, Research and Economic Development Office of New Mexico Bradley J. Magnetta, Frederick W. Rastede Institute of Mining and Technology (NMIMT). Student support at Department of Physics and Astronomy, Butler University NMIMT is given by NASA EPScOR grant NNX11AQ35A. We Indianapolis, IN USA would like to thank F. Levinson for a generous gift enabling Butler University's membership in the SARA consortium. (Received: 30 May) References The main-belt asteroid 8077 Hoyle was observed on 13 Etscorn Campus Observatory (ECO) (2012). nights over a span of 47 days in 2012 April-May. A http://www.mro.nmt.edu/education-outreach/etscorn-campus- bimodal synodic period of 2.7454 ± 0.0002 h and an observatory/ amplitude of 0.20 ± 0.02 mag. were obtained. Southeastern Association for Research in Astronomy Observatory (SARA) (2012).
    [Show full text]
  • Planetary Science Institute
    ..q. ( N ASA-C9-102536) PLANETARY ASIPCNCMY Final N80-15003 Peport. (Planetary Science Inst., Tucson, Ariz.) 122 n HC AO6/MF AO 1 CSCI. 0 3A Tin cIa:s G 1/89 15440 dM f PLANETARY SCIENCE INSTITUTE J/ vsr>k` ! "r f "y. .,y _ r{ F yr•t J ` 'F^ r• , !y ^, +F.^ Y L'. ri a^a7„yp ^l S .i- S': a r . i f r x ayy-h' - 's +^ ^+ _ J ^.>`te ^ hr ^.^^. t^rw j .1 ,k ;}, x'S; iY:`ef t.r F^ y,^ _4. ` , ^o A 5` +rf .^ k^^31 s ^ s^ x^r y- ^ r^ Ly ^{ ' .[ a Y£' fir. ^Y ,^ r R. ♦ G£ n r! ^i n s. r -'^F` { ¢ 'j 7•^"^ (NASA-CR-162526:; ^; h t' di7^r. Yfs x . (Planetaryetary sciePLANETARY ASTRONOMY Final nce Inst., Tucson N80-15003 4 -Ariz.) 122 P HC A , 0 6/MF A01 „ 3 CSCL 03A ,^` pnclas x mod, G-3/89 15440 F t ^ M ¢ ._^ , ^ '^ _^",^- 2^'£ :N by A } z5'^; y t r',,ro,' fi t J ^,;,,^I. e4 r :'1 ,(^ n., a ^ ^.-dz a -^ ^ { t L uy ^^ y •^, / { ,{.V,^^ u r 3 wi.;r r f { d ^ 7'^, ^'^^ h{ .d1 {^ '.^+"^i+.Y:,,.^Lu.c^' r feiS. A ^^PNtq:!tir7AetdJ^JAe! ^'J. ` s,.z.`^ h` YT r a ``t ' ^4 5+.e4...'`^+ 1 - 3 9^ H .^ 1 Yf 4.. 1 v^^ 5 .. I L^ ' + [. X j rr y^ 4^ r i+ d s'3 5t: PLANETARY SCIENCE INSTITUTE ^_J -1- i TABLE OF CONTENTS Page TASK 1.1: SPECTROPHOTOMETRIC OBSERVATIONS AND ANALYSIS OF ASTEROIDS .
    [Show full text]
  • Preliminary Program
    20-th Gamow International Astronomical Conference-School “ASTRONOMY AND BEYOND: ASTROPHYSICS, COSMOLOGY AND GRAVITATION, HIGH ENERGY PHYSICS, ASTROPARTICLE PHYSICS, RADIOASTRONOMY AND ASTROBIOLOGY” 9–16 August, 2020, Odessa, Ukraine The 20-th Gamow conference-school is devoted to: the 155-th anniversary of the Odessa I.I.Mechnikov National University; the 55-th anniversary of the discovery of cosmic microwave background radiation of the Universe; the 140-th anniversary of prof. A.Ya.Orlov (Head of the Odessa Astro- nomical Observatory in 1913–1944); the 170-th anniversary of prof A.K.Kononovich (Head of the Odessa As- tronomical Observatory in 1881 – 1911). SCIENTIFIC ORANIZING COMMITEE: Chair of SOC: V.M.Shulga (IRA NASU, Kharkov, Ukraine, [email protected]) Vice-chair: M.I.Ryabov (IRA NASU, Odessa, Ukraine, [email protected]) Secretary: S.M.Melikyants (AO ONU, Odessa, Ukraine, [email protected]) Members of SOC: V.M.Adamyan (ONU), S.M.Andrievsky (ONU), I.L.Andronov (ONMU), A.A.Konovalenko (IRA NASU), N.I.Koshkin (ONU), V.V.Kovtyukh (ONU), T.V.Mishenina (ONU), E.A.Panko (ONU), O.M.Ulyanov (IRA NASU), I.B.Vavilova (MAO), Y.S.Yatskiv (President of UAA), V.V.Zakharenko (IRA NASU), A.I. Zhuk (ONU). LOCAL ORANIZING COMMITEE Chair: I.N.Koval (Rector of ONU) Vice-Chair: M.I.Ryabov Secretary: A.A.Pilipenko Members of LOC: A.Yu.Burgazli, A.V.Chopovsky, A.V.Dragunova, A.Gorbunov, T.I.Kabanova, V.G.Komendant, N.I.Koshkin, S.M.Melikyants, B.A.Murnikov, V.P.Olyeynik, S.L.Strakhova, L.I.Sobitnyak, V.V.Troianskyi.
    [Show full text]
  • The Minor Planet Bulletin Published an Article on Analysis
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 2, A.D. 2007 APRIL-JUNE 27. THE ROTATION PERIOD OF 2651 KAREN Colin Bembrick Mt Tarana Observatory PO Box 1537, Bathurst, NSW 2795, Australia [email protected] Bill Allen Vintage Lane Observatory 83 Vintage Lane, RD3, Blenheim, New Zealand (Received: 6 January) 2651 Karen was observed over 4 nights in 2006. The synodic period was determined as 6.3227 ± 0.0037 hr. The peak to peak amplitude was approximately 0.3 mag, implying an axial ratio (a/b) of 1.32 References Bembrick, C.S., Richards, T., Bolt, G., Pereghy, B., Higgins, D. Minor planet 2651 Karen (1949 QD) was discovered by E. and Allen, W.H. (2004). “172 Baucis – A Slow Rotator”. Minor Johnson in August 1949 at Johannesburg. This is an outer main Planet Bulletin, 31, 51-52. belt asteroid with a diameter of 39.7 km (GUIDE ver 8). The latest list of rotational parameters (Harris & Warner, 2006) has no GUIDE version 8 (2002). http://www.projectpluto.com quoted period. Harris, A.W. and Warner, B.D. (2006). “Minor Planet Lightcurve The observations of Karen in 2006 were conducted from two sites Parameters”. Updated March 14, 2006. – one in New Zealand and one in Australia. The locations of these http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html sites are listed in Bembrick et al (2004). All observations were made using unfiltered differential photometry and all data were Harris, A.W., Young, J.W., Bowell, E., Martin, L.
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 4, A.D. 2006 OCTOBER-DECEMBER 77. ADDITIONAL LIGHTCURVES OF 165 LORELEY of trial periods correspond to possible synodic rotation periods. In this analysis all periods between 6 and 15 hours, at intervals of Frederick Pilcher 0.001 hour, had rms deviations computed. Lightcurves phased to Illinois College each of a large number of periods with local rms minima were Jacksonville, IL 62650 USA plotted and inspected visually for goodness of fit. Periods of [email protected] 7.224 hours, 9.632 hours, 13.515 hours, and 14.448 hours, all ± 0.001 hours, provided nearly identical rms errors and comparably Don C. Jardine good fits on those parts of the lightcurve which overlapped on 12872 Walnut Woods Drive more than one night. Pleasant Plains, IL 62677 USA Hence this study by itself does not obtain a unique determination (Received: 26 April Revised: 12 August) of the synodic rotation period. Harris (2006) stated that he considered a 7.223 hour period to have reliability 3 (secure). Our Lightcurves of 165 Loreley obtained on three nights in 7.224 hour period is consistent with this one, and the accompanying figure is phased to 7.224 hours. early 2006 can be satisfied by several different rotation periods, one of which, 7.224 hours, is consistent with The authors express their thanks to Brian D. Warner, Walt the tabulated value, with an amplitude of 0.17 mag. Cooney, Bob Koff, and Dan Klinglesmith for their instruction and continuing support which made this project possible.
    [Show full text]
  • Major Fields
    CURRICULUM VITAE Vishnu Reddy Assistant Professor, Lunar and Planetary Laboratory University of Arizona 1629 E. University Blvd Tucson, AZ 85721 Ph. 808-342-8932 Chronology of Education: • Bharathiar University (1998): Visual Communications (BS) • Madurai Kamraj University (2001): Communication (MA) • University of North Dakota (2005): SPace Studies (MS) • Title of Master’s Thesis: Mineralogy of Asteroids 246 Asporina and 446 Aeternitas and Investigations of Temperature-induced Spectral Effects • MS Thesis Advisor: Paul Hardersen • University of North Dakota (2009): Earth System Science and Policy (PhD) • Title of Doctoral Dissertation: Mineralogical Survey of Near-Earth Asteroid Population: Implications for Impact Hazard Assessment and Sustainability of Life on Earth • Dissertation Advisor: Michael Gaffey Major Fields: • Physical Characterization of Small Bodies in the Solar System • SPace Situational Awareness • Instrumentation for Ground based Remote Sensing • Laboratory SPectral Characterization of Planetary Materials 1 Chronology of EmPloyment: University of Arizona: Lunar and Planetary Laboratory: Associate Professor 2018-Present University of Arizona: Lunar and Planetary Laboratory: Assistant Professor 2016-2018 University of Arizona: Lunar and Planetary Laboratory: Adjunct Professor 2016 SPring Planetary Science Institute: Research Scientist 2013-2016 Planetary Science Institute: Associate Research Scientist 2013 University of North Dakota: DePartment of SPace Studies Research Assistant Professor 2010- 2013 University of North
    [Show full text]