The 4 Major Asteroids and Chiron Report For
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The 4 Major Asteroids and Chiron Report For
The 4 Major Asteroids and Chiron Report for Brad Roberts 10 January 1964 6:33 AM Winnipeg, Manitoba,Canada Calculated for: Standard time, Time Zone 6 hours West Latitude: 49 N 53 Longitude: 97 W 09 Positions of Planets at Birth: Sun 19 Cap 18 Asc. 20 Sag 35 Moon 1 Sag 21 MC 21 Lib 49 Mercury 6 Cap 24 2nd cusp 0 Aqu 56 Venus 21 Aqu 54 3rd cusp 17 Pis 07 Mars 27 Cap 52 5th cusp 15 Tau 45 Jupiter 11 Ari 42 6th cusp 4 Gem 07 Saturn 21 Aqu 25 Ceres 9 Sag 44 Uranus 9 Vir 47 Pallas 20 Sco 12 Neptune 17 Sco 47 Juno 23 Sco 36 Pluto 14 Vir 47 Vesta 4 Cap 54 True Node11 Can 47 Chiron 11 Pis 23 Aspects and orbs: Conjunction : 7 Deg 00 Min Trine : 5 Deg 00 Min Opposition : 6 Deg 00 Min Sextile : 3 Deg 00 Min Square : 4 Deg 00 Min Interpretations by astrologer Dave Campbell Report and Text Copyright By Cosmic Patterns Software, Inc. The contents of this report are protected by Copyright law. By purchasing this report you agree to comply with this Copyright. Libra Moon, Inc www.libramoonastrology.com www.zodiac-reports.com Chapter 1: Ceres Ceres in Sagittarius: You nurture people with your generosity cheerfulness and encouragement. Giving them the optimism and openness they need. You aim to inspire them and make them feel like they are it. Your honest disposition and behavior is also a gift for them to know your devotion to them. All of these things are exactly what you need in order to feel cared for. -
Occultation Newsletter Volume 8, Number 4
Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date. -
Phase Integral of Asteroids Vasilij G
A&A 626, A87 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935588 & © ESO 2019 Astrophysics Phase integral of asteroids Vasilij G. Shevchenko1,2, Irina N. Belskaya2, Olga I. Mikhalchenko1,2, Karri Muinonen3,4, Antti Penttilä3, Maria Gritsevich3,5, Yuriy G. Shkuratov2, Ivan G. Slyusarev1,2, and Gorden Videen6 1 Department of Astronomy and Space Informatics, V.N. Karazin Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine e-mail: [email protected] 2 Institute of Astronomy, V.N. Karazin Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine 3 Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2, 00560 Helsinki, Finland 4 Finnish Geospatial Research Institute FGI, Geodeetinrinne 2, 02430 Masala, Finland 5 Institute of Physics and Technology, Ural Federal University, Mira str. 19, 620002 Ekaterinburg, Russia 6 Space Science Institute, 4750 Walnut St. Suite 205, Boulder CO 80301, USA Received 31 March 2019 / Accepted 20 May 2019 ABSTRACT The values of the phase integral q were determined for asteroids using a numerical integration of the brightness phase functions over a wide phase-angle range and the relations between q and the G parameter of the HG function and q and the G1, G2 parameters of the HG1G2 function. The phase-integral values for asteroids of different geometric albedo range from 0.34 to 0.54 with an average value of 0.44. These values can be used for the determination of the Bond albedo of asteroids. Estimates for the phase-integral values using the G1 and G2 parameters are in very good agreement with the available observational data. -
Iso and Asteroids
r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep. -
Appendix 1 1311 Discoverers in Alphabetical Order
Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D. -
Updated IAA RAS Planetary Ephemerides-EPM2011 and Their
ISSN 0038-0946, Solar System Research, 2013, Vol. 47, No. 5, pp. 386-402. c Pleiades Publishing, Inc., 2013. Original Russian Text c E.V. Pitjeva, 2013, published in Astronomicheskii Vestnik, 2013, Vol. 47, No. 5, pp. 419-435 UDK 521.172:523.2 Updated IAA RAS Planetary Ephemerides-EPM2011 and Their Use in Scientific Research c 2013 г. E. V. Pitjeva Institute of Applied Astronomy, Russian Academy of Sciences, nab. Kutuzova 10, St. Petersburg, 191187 Russia Received December 20, 2012 Abstract -The EPM (Ephemerides of Planets and the Moon) numerical ephemerides were first created in the 1970s in support of Russian space flight missions and since then have been constantly improved at IAA RAS. In the following work, the latest version of the planetary part of the EPM2011 numerical ephemerides is presented. The EPM2011 ephemerides are computed using an updated dynamical model, new values of the parameters, and an extended observation database that contains about 680 000 positional measurements of various types obtained from 1913 to 2011. The dynamical model takes into account mutual perturbations of the major planets, the Sun, the Moon, 301 massive asteroids, and 21 of the largest trans-Neptunian objects (TNOs), as well as perturbations from the other main-belt asteroids and other TNOs. The EPM ephemerides are computed by numerical integration of the equations of motion of celestial bodies in the parameterized post-Newtonian n-body metric in the BCRS coordinate system for the TDB time scale over a 400-year interval. The ephemerides were oriented to the ICRF system using 213 VLBI observations (taken from arXiv:1308.6416v1 [astro-ph.EP] 29 Aug 2013 1989 to 2010) of spacecraft near planets with background quasars, the coordinates of which are given in the ICRF system. -
Pallas Rpitsbitdt Icarus to Submitted Preprint Foundation
Physical Properties of (2) Pallas✩ Benoˆıt Carrya,b, Christophe Dumasa, Mikko Kaasalainenc, J´erˆome Berthierd, William J. Merlinee, St´ephane Erardb, Al Conradf, Jack D. Drummondg, Daniel Hestrofferd, Marcello Fulchignonib, Thierry Fuscoh aESO, Alonso de C´ordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile bLESIA, Observatoire de Paris, CNRS, 5 place Jules Janssen, 92190 Meudon Cedex, France cP.O. Box 68 (Gustaf H¨allstr¨omin katu 2b), FI-00014 University of Helsinki, Finland dIMCCE, Observatoire de Paris, CNRS, 77 av. Denfert Rochereau, 75014 Paris, France eSouthwest Research Institute, 1050 Walnut St. # 300, Boulder, CO 80302, U.S.A. fW. M. Keck Observatory, Hawaii, U.S.A. gStarfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, New Mexico 87117-577, U.S.A. hONERA, BP 72, 92322 Chˆatillon Cedex, France Abstract Ground-based high angular-resolution images of asteroid (2) Pallas at near-infrared wavelengths have been used to determine its physical properties (shape, dimensions, spatial orientation and albedo distribution). We acquired and analyzed adaptive-optics (AO) J/H/K-band observations from Keck II and the Very Large Telescope taken during four Pallas oppositions between 2003 and 2007, with spatial resolution spanning 32–88 km (image scales 13–20 km/pix). We improve our determination of the size, shape, and pole by a novel method that combines our AO data with 51 visual light-curves spanning 34 years of observations as well as archived occultation data. The shape model of Pallas derived here reproduces well both the projected shape of Pallas on the sky (average deviation of edge profile of 0.4 pixel) and light-curve behavior (average deviation of 0.019 mag) at all the epochs considered. -
Rocks in Space Asteroids, Comets and Meteors
Modern Astronomy: Voyage to the Planets Lecture 6 Rocks in Space asteroids, comets and meteors University of Sydney Centre for Continuing Education Autumn 2009 Tonight: • Asteroids – rocks that circle • Comets – rocks that evaporate • Trans-Neptunian objects – really cold rocks • Meteorites – rocks that fall Asteroids The Solar System contains a large number of small bodies, of which the largest are the asteroids. Some orbit the Sun inside the Earth’s orbit, and others have highly elliptical orbits which cross the Earth’s. However, the vast bulk of asteroids orbit the Sun in nearly circular orbits in a broad belt between Mars and Jupiter. An asteroid (or strictly minor planet*) is smaller than major planets, but larger than meteoroids, which are 10m or less in size. * since 2006, these are now officially small solar system bodies, though the term “minor planet” may still be used As of April 2009, there are 212,999 asteroids which have been given numbers; 15190 have been given names. The rate of discovery of new bodies is about 5000 per month. It is estimated there are between 1.1 and 1.9 million asteroids larger than 1 km in diameter. Number of minor planets with orbits (red) and names (green) The largest are 1 Ceres (1000 km in diameter), 2 Pallas (550 km), 4 Vesta (530!km), and 10 Hygiea (410 km). Only 16 asteroids are larger than 240 km in size. Ceres is by far the largest and most massive body in the asteroid belt, and contains approximately a third of the belt's total mass. -
Dawn: a Journey to the Beginning of the Solar System
DAWN: A JOURNEY TO THE BEGINNING OF THE SOLAR SYSTEM C.T. Russell(1), A. Coradini(2), W.C. Feldman(3), R. Jaumann(4), A.S. Konopliv(5), T.B. McCord(6), L.A. McFadden(7), H.Y. McSween(8), S. Mottola(4), G. Neukum(9), C.M. Pieters(10) C.A. Raymond(5), D.E. Smith(11), M.V. Sykes(12) B.G. Williams(5), and M.T. Zuber(13) 1IGPP&ESS, UCLA, Los Angeles, CA 90095-1567; [email protected] 2IFSI, Via del fosso del Cavaliere, 00133 ROMA Italy 3LANL, MS D466, NIS-1, Los Alamos, NM 87545 4DLR Rutherfordstr 2, D-12489 Berlin, Germany 5JPL, 4800 Oak Grove Dr., Pasadena, CA 91109 6University of Hawaii, 2525 Correa Rd., Honolulu, HI 96822 7University of Maryland, College Park, MD 20742 8University of Tennessee, Knoxville, TN 37996-1410 9Freie Universitat Berlin, Malteser Str.74-100, 12249 Berlin, Germany 10Brown University, Providence, RI 02912 11GSFC, MC 920, Greenbelt, MD 20771 12U of Arizona, Tucson, AZ 85721 13MIT, Cambridge, MA 02139 ABSTRACT/RESUME Once Jupiter formed, by gravitational collapse, its orbital motion relative to the asteroids Dawn, NASA's ninth Discovery mission, is provided a periodic gravitational pulse that scheduled to launch on May 27, 2006 on a accelerated them so they would no longer journey that will take it into orbit about the two accrete. Thus the formation of Jupiter stopped most massive asteroids 4 Vesta and 1 Ceres. much of the geochemical evolution of this Dawn's goal is to understand the conditions and region. By exploring the two most massive processes present at the solar system's earliest planetesimals, Dawn studies some of the earliest epoch, and the role of water content and size in processes in the solar system, those occurring planetary evolution. -
Towards a Multi-Dimensional Classification Scheme for Minor Planets
TOWARDS A MULTI-DIMENSIONAL CLASSIFICATION SCHEME FOR MINOR PLANETS Max Mahlke Centro de Astrobiología (CSIC-INTA) in collaboration with Enrique Solano, Benoit Carry, Bruno Merín, Remi Flamary, the Spanish Virtual Observatory and the ESASky team TOWARDS A MULTI-DIMENSIONAL CLASSIFICATION SCHEME FOR MINOR PLANETS Max Mahlke Centro de Astrobiología (CSIC-INTA) in collaboration with Enrique Solano, Benoit Carry, Bruno Merín, Remi Flamary, the Spanish Virtual Observatory and the ESASky team NASA/JPL-Caltech/UCLA/MPS/DLR/IDA !1 Ceres DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Pallas Mercury Venus Earth Mars Ceres Juno Jupiter Saturn Uranus Vesta DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Pallas Mercury Venus Earth Mars Ceres Juno Jupiter Saturn UranusNeptune Vesta DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Mercury Venus Earth Mars Jupiter Saturn UranusNeptune DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Mercury Venus Earth Mars Jupiter Saturn UranusNeptune Pluto DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas 1992 QB Mercury Venus Earth Mars Jupiter Saturn UranusNeptune Pluto Albion DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Mercury Venus Earth Mars Jupiter Saturn UranusNeptune DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Mercury Venus Earth Mars Jupiter Saturn UranusNeptune June 2019: 795,000 DeMeo+ 2015 Max Mahlke | ESAC Science Seminar | 13 June 2019 !2 Pallas Centaurs Trans-Neptunian Objects // DeMeo & Carry 2014 Heterogeneous in heliocentric distance: <1AU to >100AU in shapes in orbital inclination: 0° to 33° for Main Belt asteroids in rotation: hours to days in orbital eccentricity: 0. -
Nasa Technical Memorandum .1
NASA TECHNICAL MEMORANDUM NASA TM X-64677 COMETS AND ASTEROIDS: A Strategy for Exploration REPORT OF THE COMET AND ASTEROID MISSION STUDY PANEL May 1972 .1!vP -V (NASA-TE-X- 6 q767 ) COMETS AND ASTEROIDS: A RR EXPLORATION (NASA) May 1972 CSCL 03A NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Reproduced by ' NATIONAL "TECHINICAL INFORMATION: SERVICE US Depdrtmett ofCommerce :. Springfield VA 22151 TECHNICAL REPORT STANDARD TITLE PAGE · REPORT NO. 2. GOVERNMENT ACCESSION NO. 3, RECIPIENT'S CATALOG NO. NASA TM X-64677 . TITLE AND SUBTITLE 5. REPORT aE COMETS AND ASTEROIDS ___1_ A Strategy for Exploration 6. PERFORMING ORGANIZATION CODE AUTHOR(S) 8. PERFORMING ORGANIZATION REPORT # Comet and Asteroid Mission Study Panel PERFORMING ORGANIZATION NAME AND ADDRESS 10. WORK UNIT NO. 11. CONTRACT OR GRANT NO. 13. TYPE OF REPORT & PERIOD COVERED 2. SPONSORING AGENCY NAME AND ADDRESS National Aeronautics and Space Administration Technical Memorandum Washington, D. C. 20546 14. SPONSORING AGENCY CODE 5. SUPPLEMENTARY NOTES ABSTRACT Many of the asteroids probably formed near the orbits where they are found today. They accreted from gases and particles that represented the primordial solar system cloud at that location. Comets, in contrast to asteroids, probably formed far out in the solar system, and at very low temperatures; since they have retained their volatile components they are probably the most primordial matter that presently can be found anywhere in the solar system. Exploration and detailed study of comets and asteroids, therefore, should be a significant part of NASA's efforts to understand the solar system. A comet and asteroid program should consist of six major types of projects: ground-based observations;Earth-orbital observations; flybys; rendezvous; landings; and sample returns. -
Athena: the First-Ever Encounter of (2) Pallas with a Smallsat
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 2225.pdf ATHENA: THE FIRST-EVER ENCOUNTER OF (2) PALLAS WITH A SMALLSAT. J. G. O’Rourke1,*, J. Castillo-Rogez2, L. T. Elkins-Tanton1, R. R. Fu3, T. N. Harrison1, S. Marchi4, R. Park2, B. E. Schmidt5, D. A. Wil- liams1, C. C. Seybold2, R. N. Schindhelm6, J. D. Weinberg6, 1School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 2Jet Propulsion Laboratory, Pasadena, CA, 3Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, 4Southwest Research Institute, Boulder, CO, 5School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA, 6Ball Aerospace, Boulder, CO, *[email protected]. Introduction: Pallas is the largest unexplored and • How have the myriad chemical and physical most off-ecliptic protoplanet in the main belt and the processes that shaped the solar system operated, parent of a populous impact family that includes many interacted, and evolved over time? near-Earth asteroids. Discovered in 1802 by serendipity • How did the current population of asteroids during the earliest observations of Ceres, Pallas is nearly evolve in time and space? the same size as Vesta. Protoplanets provide fascinating Athena makes substantial progress towards achieving examples of planetary processes like volcanism, tecton- two broad, high-level science goals: ics, and internal differentiation. Existing observations 1. Understand the role of water in the evolution hint that Pallas fills an observational gap in terms of wa- of Pallas. ter content between Vesta and Ceres—the two pro- 2. Constrain the dynamical evolution of Pallas toplanets explored by NASA’s Dawn Mission [1,2].