An Introduction to Gravity in the Solar System
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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 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. -
Dynamical Evolution of the Cybele Asteroids
MNRAS 451, 244–256 (2015) doi:10.1093/mnras/stv997 Dynamical evolution of the Cybele asteroids Downloaded from https://academic.oup.com/mnras/article-abstract/451/1/244/1381346 by Universidade Estadual Paulista J�lio de Mesquita Filho user on 22 April 2019 V. Carruba,1‹ D. Nesvorny,´ 2 S. Aljbaae1 andM.E.Huaman1 1UNESP, Univ. Estadual Paulista, Grupo de dinamicaˆ Orbital e Planetologia, 12516-410 Guaratingueta,´ SP, Brazil 2Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA Accepted 2015 May 1. Received 2015 May 1; in original form 2015 April 1 ABSTRACT The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is ad- jacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only relatively recently the first dynamical groups were identified in this area. Among these, the Sylvia group has been proposed to be one of the oldest families in the extended main belt. In this work we identify families in the Cybele region in the context of the local dynamics and non-gravitational forces such as the Yarkovsky and stochastic Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effects. We confirm the detec- tion of the new Helga group at 3.65 au, which could extend the outer boundary of the Cybele region up to the 5J:-3A mean-motion resonance. -
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. -
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. -
Dynamical Evolution of the Cybele Asteroids 3 Resonances, of Which the Most Studied (Vokrouhlick´Yet Al
Mon. Not. R. Astron. Soc. 000, 1–14 (2015) Printed 18 April 2018 (MN LATEX style file v2.2) Dynamical evolution of the Cybele asteroids V. Carruba1⋆, D. Nesvorn´y2, S. Aljbaae1, and M. E. Huaman1 1UNESP, Univ. Estadual Paulista, Grupo de dinˆamica Orbital e Planetologia, Guaratinguet´a, SP, 12516-410, Brazil 2Department of Space Studies, Southwest Research Institute, Boulder, CO, 80302, USA Accepted ... Received 2015 ...; in original form 2015 April 1 ABSTRACT The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only relatively recently the first dynamical groups were identified in this area. Among these, the Sylvia group has been proposed to be one of the oldest families in the extended main belt. In this work we identify families in the Cybele region in the context of the local dynamics and non-gravitational forces such as the Yarkovsky and stochastic YORP effects. We confirm the detection of the new Helga group at ≃3.65 AU, that could extend the outer boundary of the Cybele region up to the 5J:-3A mean-motion reso- nance. We obtain age estimates for the four families, Sylvia, Huberta, Ulla and Helga, currently detectable in the Cybele region, using Monte Carlo methods that include the effects of stochastic YORP and variability of the Solar luminosity. -
Dynamical Evolution of the Cybele Asteroids V Carruba, D
Dynamical evolution of the Cybele asteroids V Carruba, D. Nesvorný, Safwan Aljbaae, M Huaman To cite this version: V Carruba, D. Nesvorný, Safwan Aljbaae, M Huaman. Dynamical evolution of the Cybele asteroids. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2015, 451 (1), pp.1 - 14. 10.1093/mnras/stv997. hal-02481140 HAL Id: hal-02481140 https://hal.sorbonne-universite.fr/hal-02481140 Submitted on 17 Feb 2020 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. Mon. Not. R. Astron. Soc. 000, 1–14 (2015) Printed 15 May 2015 (MN LATEX style file v2.2) Dynamical evolution of the Cybele asteroids V. Carruba1⋆, D. Nesvorn´y2, S. Aljbaae1, and M. E. Huaman1 1UNESP, Univ. Estadual Paulista, Grupo de dinˆamica Orbital e Planetologia, Guaratinguet´a, SP, 12516-410, Brazil 2Department of Space Studies, Southwest Research Institute, Boulder, CO, 80302, USA Accepted ... Received 2015 ...; in original form 2015 April 1 ABSTRACT The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. -
The British Astronomical Association Handbook 2019
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2019 2018 October ISSN 0068–130–X CONTENTS PREFACE . 2 HIGHLIGHTS FOR 2019 . 3 SKY DIARY . .. 4-5 CALENDAR 2019 . 6 SUN . 7-9 ECLIPSES . 10-17 APPEARANCE OF PLANETS . 18 VISIBILITY OF PLANETS . 19 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 20-21 PLANETS – Explanation of Tables . 22 ELEMENTS OF PLANETARY ORBITS . 23 MERCURY . 24-25 VENUS . 26 EARTH . 27 MOON . 27 LUNAR LIBRATION . 28 MOONRISE AND MOONSET . 30-33 SUN’S SELENOGRAPHIC COLONGITUDE . 34 LUNAR OCCULTATIONS . 35-41 GRAZING LUNAR OCCULTATIONS . 42-43 MARS . 44-45 ASTEROIDS . 46 ASTEROID EPHEMERIDES . 47-51 ASTEROID OCCULTATIONS (incl. TNO Hightlight:28978 Ixion) . 52-55 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 56-58 NEO CLOSE APPROACHES TO EARTH . 59 JUPITER . .. 60-64 SATELLITES OF JUPITER . .. 64-68 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 69-78 SATURN . 79-82 SATELLITES OF SATURN . 83-86 URANUS . 87 NEPTUNE . 88 TRANS–NEPTUNIAN & SCATTERED-DISK OBJECTS . 89 DWARF PLANETS . 90-93 COMETS . 94-98 METEOR DIARY . 99-101 VARIABLE STARS (RZ Cassiopeiae; Algol; RS Canum Venaticorum) . 102-103 MIRA STARS . 104 VARIABLE STAR OF THE YEAR (RS Canum Venaticorum) . .. 105-107 EPHEMERIDES OF VISUAL BINARY STARS . 108-109 BRIGHT STARS . 110 ACTIVE GALAXIES . 111 TIME . 112-113 ASTRONOMICAL AND PHYSICAL CONSTANTS . 114-115 GREEK ALPHABET . 115 ACKNOWLEDGMENTS / ERRATA . 116 Front Cover: Mercury - taken between 2018 June 25 and July 12 by Simon Kidd using a C14 scope, ASI224MC camera and 742nm filter. Different processing is combined for limb and main image content, owing to extremely low contrast. -
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 ....................................... -
ASTEROID LIGHTCURVE DATA BASE (LCDB) Revised 2021 April 15
ASTEROID LIGHTCURVE DATA BASE (LCDB) Revised 2021 April 15 SPECIAL NOTICES The README.txt file is no longer distributed. Only the bookmarked PDF version is included. 2021 April VERY IMPORTANT Changes Regarding Phase Slope Parameter G(1), G2 To accommodate the currently adopted absolute magnitude/phase slope parameter H-G12 (H- G1,2) systems that replaced the traditional H-G system, new fields have been added to the Summary and Details tables and reports. See section 3.1.1 THE H-G, H-G12, and H-G1,G2 SYSTEMS. Changes Regarding Groups/Families The LCDB has been revised to use a hybrid of the Nesvorny (2015) and Nesvorny et al. (2015) families and those defined on the AstDys (2021) web site. As such, all entries in the “Family” column in those reports that include it, now have a text value that represents a number from either the Nesvorny or AstDys site family definitions. See section 3.1.2 FAMILY/GROUP MEMBERSHIP, DEFAULT ALBEDOS, AND TAXONOIMC CLASS. File Name Changes The file names in the distribution have been changed to match those in the set submitted to the NASA Planetary Data System Small Bodies Node. See section 2.1.0 DISTRIBUTION FILES for the revised file list. As a result of the changes above, column mappings for the lc_summary, lc_details, and lc_diameters reports have changed and there is a new lc_familylookup table. The new listings are given the appropriate subsections of Section 4. 2020 December The CLASS column in the Summary and Details table was expanded to 10 characters. This changed the column mapping for this and all subsequent columns. -
The British Astronomical Association Handbook 2018
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2018 2017 October ISSN 0068–130–X CONTENTS PREFACE . 2 HIGHLIGHTS FOR 2018 . 3 SKY DIARY . .. 4-5 CALENDAR 2018 . 6 SUN . 7-9 ECLIPSES . 10-15 APPEARANCE OF PLANETS . 16 VISIBILITY OF PLANETS . 17 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 18-19 PLANETS – Explanatin of Tables . 20 ELEMENTS OF PLANETARY ORBITS . 21 MERCURY . 22-23 VENUS . 24 EARTH . 25 MOON . 25 LUNAR LIBRATION . 26 MOONRISE AND MOONSET . 27-31 SUN’S SELENOGRAPHIC COLONGITUDE . 32 LUNAR OCCULTATIONS . 33-39 GRAZING LUNAR OCCULTATIONS . 40-41 MARS . 42-43 ASTEROIDS . 44 ASTEROID EPHEMERIDES . 45-49 ASTEROID OCCULTATIONS (incl. TNO Hightlight:1998 WV31) . 50-53 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 54-56 NEO CLOSE APPROACHES TO EARTH . 57 JUPITER . .. 58-62 SATELLITES OF JUPITER . .. 62-66 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 67-76 SATURN . 77-80 SATELLITES OF SATURN . 81-84 URANUS . 85 NEPTUNE . 86 TRANS–NEPTUNIAN & SCATTERED-DISK OBJECTS . 87 DWARF PLANETS . 88-91 COMETS . 92-96 METEOR DIARY . 97-99 VARIABLE STARS (RZ Cassiopeiae; Algol; RS Canum Venaticorum) . 100-101 MIRA STARS . 102 VARIABLE STAR OF THE YEAR (VV Cephei) . .. .. 103-105 EPHEMERIDES OF VISUAL BINARY STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 TIME . 110-111 ASTRONOMICAL AND PHYSICAL CONSTANTS . 112-113 INTERNET RESOURCES . 114-115 GREEK ALPHABET . 115 ACKNOWLEDGEMENTS / ERRATA . 116 Front Cover: Mars - Apparent Diam. 18.4" taken from Barbados on 2016 June 05 by Damian Peach using a 356mm aper- ture Schmidt-Cassegrain telescope (North up) British Astronomical Association HANDBOOK FOR 2018 NINETY–SEVENTH YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 PREFACE Welcome to the 97th Handbook of the British Astronomical Association. -
Identification and Dynamical Properties of Asteroid Families
Identification and Dynamical Properties of Asteroid Families David Nesvorny´ Department of Space Studies, Southwest Research Institute, Boulder Miroslav Brozˇ Institute of Astronomy, Charles University, Prague Valerio Carruba Department of Mathematics, UNESP, Guaratinguet´a Asteroids formed in a dynamically quiescent disk but their orbits became gravitationally stirred enough by Jupiter to lead to high-speed collisions. As a result, many dozen large asteroids have been disrupted by impacts over the age of the Solar System, producing groups of fragments known as asteroid families. Here we explain how the asteroid families are identified, review their current inventory, and discuss how they can be used to get insights into long-term dynamics of main belt asteroids. Electronic tables of the membership for 122 notable families are reported on the Planetary Data System node. See related chapters in this volume for the significance of asteroid families for studies of physics of large scale collisions, collisional history of the main belt, source regions of the near-Earth asteroids, meteorites and dust particles, and space weathering. 1. INTRODUCTION from dynamical considerations. Telescopic surveys such as the Sloan Digital Sky Survey As witnessed by the heavily cratered surfaces imaged by (SDSS), Wide-field Infrared Survey Explorer (WISE) and spacecrafts, the chief geophysical process affecting aster- AKARI All-Sky Survey provide a wealth of data on physi- oids is impacts. On rare occasions, the impact of a large cal properties of the main belt asteroids (Ivezi´cet al., 2001; projectile can be so energetic that the target asteroid is vio- Mainzer et al., 2011; Usui et al., 2013). -
Johann Palisa, the Most Successful Visual Discoverer of Asteroids
PDFMAILER.COM Print and send PDF files as Emails with any application, ad-sponsored and free of charge www.pdfmailer.com Johann Palisa, the most successful visual discoverer of asteroids Herbert Raaba,b a Astronomical Society of Linz, Sternwarteweg 5, A-4020 Linz, Austria b Herbert Raab, Schönbergstr. 23/21, A-4020 Linz, Austria; [email protected] Part of the Programme of MACE 2002 was a trip to the remnants of the old Pola observatory. Among minor planet observers, this observatory is mostly known for the work of Johann Palisa. This paper provides a short biography of Johann Palisa, as well as some information about his discoveries. Palisa was director of the Pola observatory from 1872 until 1880. He discovered 28 minor planets and one comet during that time. In 1880, he took a position at the new Vienna observatory. Here, he discovered further 94 minor planets, all by visual observations. His most famous discovery is probably the Amor-type asteroid (719) Albert. Today, Palisa remains the most successful visual discoverer of asteroids. A short biography of Johann Palisa used to send his assistants to bed at midnight, but continued to observe until the break of dawn, handling the Johann Palisa was born on December 6, 1848 in Troppau, instrument all alone. Palisa discovered further 94 asteroids Silesia (now Czech Republic) [1,2]. From 1866 to 1870 he at Vienna, all by visual observations, using the 27” and the studied mathematics and astronomy at the University of 12” refractor. In addition, Palisa discovered eight objects Vienna, but did not graduate until 1884.