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Photometry of Asteroids: Lightcurves of 24 Asteroids Obtained in 1993–2005
ARTICLE IN PRESS Planetary and Space Science 55 (2007) 986–997 www.elsevier.com/locate/pss Photometry of asteroids: Lightcurves of 24 asteroids obtained in 1993–2005 V.G. Chiornya,b,Ã, V.G. Shevchenkoa, Yu.N. Kruglya,b, F.P. Velichkoa, N.M. Gaftonyukc aInstitute of Astronomy of Kharkiv National University, Sumska str. 35, 61022 Kharkiv, Ukraine bMain Astronomical Observatory, NASU, Zabolotny str. 27, Kyiv 03680, Ukraine cCrimean Astrophysical Observatory, Crimea, 98680 Simeiz, Ukraine Received 19 May 2006; received in revised form 23 December 2006; accepted 10 January 2007 Available online 21 January 2007 Abstract The results of 1993–2005 photometric observations for 24 main-belt asteroids: 24 Themis, 51 Nemausa, 89 Julia, 205 Martha, 225 Henrietta, 387 Aquitania, 423 Diotima, 505 Cava, 522 Helga, 543 Charlotte, 663 Gerlinde, 670 Ottegebe, 693 Zerbinetta, 694 Ekard, 713 Luscinia, 800 Kressmania, 1251 Hedera, 1369 Ostanina, 1427 Ruvuma, 1796 Riga, 2771 Polzunov, 4908 Ward, 6587 Brassens and 16541 1991 PW18 are presented. The rotation periods of nine of these asteroids have been determined for the first time and others have been improved. r 2007 Elsevier Ltd. All rights reserved. Keywords: Asteroids; Photometry; Lightcurve; Rotational period; Amplitude 1. Introduction telescope of the Crimean Astrophysics Observatory in Simeiz. Ground-based observations are the main source of knowledge about the physical properties of the asteroid 2. Observations and their reduction population. The photometric lightcurves are used to determine rotation periods, pole coordinates, sizes and Photometric observations of the asteroids were carried shapes of asteroids, as well as to study the magnitude-phase out in 1993–1994 using one-channel photoelectric photo- relation of different type asteroids. -
ARISTOTLE UNIVERSITY of THESSALONIKI (Auth) FACULTY
ARISTOTLE UNIVERSITY OF THESSALONIKI (AUTh) FACULTY OF SCIENCES SCHOOL OF PHYSICS SECTION OF ASTROPHYSICS, ASTRONOMY & MECHANICS DIPLOMA THESIS “ANALYSIS OF OCCULTATIONS AND PHOTOMETRY DATA FROM NEAR- EARTH ASTEROIDS” CHRYSOVALANTIS SARAKIS SUPERVISOR: KLEOMENIS TSIGANIS THESSALONIKI, GREECE OCTOBER 2017 2 3 Table of Contents TABLE OF CONTENTS ....................................................................................................................... 3 ABSTRACT ............................................................................................................................................ 7 ΠΕΡΙΛΗΨΗ ............................................................................................................................................ 7 ACKNOWLEDGEMENTS - INTRODUCTION ................................................................................ 9 CHAPTER 1 ......................................................................................................................................... 11 ASTEROIDS ......................................................................................................................................... 11 1.1 ORBITAL ELEMENTS ............................................................................................................ 11 1.1.1 Semi-major axis (a) .......................................................................................................... 11 1.1.2 Eccentricity (e) ................................................................................................................ -
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. -
A Radar Survey of Main-Belt Asteroids: Arecibo Observations of 55 Objects During 1999–2003
Icarus 186 (2007) 126–151 www.elsevier.com/locate/icarus A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003 Christopher Magri a,∗, Michael C. Nolan b,StevenJ.Ostroc, Jon D. Giorgini d a University of Maine at Farmington, 173 High Street—Preble Hall, Farmington, ME 04938, USA b Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA c 300-233, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA d 301-150, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA Received 3 June 2006; revised 10 August 2006 Available online 24 October 2006 Abstract We report Arecibo observations of 55 main-belt asteroids (MBAs) during 1999–2003. Most of our targets had not been detected previously with radar, so these observations more than double the number of radar-detected MBAs. Our bandwidth estimates constrain our targets’ pole directions in a manner that is geometrically distinct from optically derived constraints. We present detailed statistical analyses of the disk-integrated properties (radar albedo and circular polarization ratio) of the 84 MBAs observed with radar through March 2003; all of these observations are summarized in the online supplementary information. Certain conclusions reached in previous studies are strengthened: M asteroids have higher mean radar albedos and a wider range of albedos than do other MBAs, suggesting that both metal-rich and metal-poor M-class objects exist; and C- and S-class MBAs have indistinguishable radar albedo distributions, suggesting that most S-class objects are chondritic. Also in accord with earlier results, there is evidence that primitive asteroids from outside the C taxon (F, G, P, and D) are not as radar-bright as C and S objects, but a convincing statistical test must await larger sample sizes. -
Appendix 1 897 Discoverers in Alphabetical Order
Appendix 1 897 Discoverers in Alphabetical Order Abe, H. 22 (7) 1993-1999 Bohrmann, A. 9 1936-1938 Abraham, M. 3 (3) 1999 Bonomi, R. 1 (1) 1995 Aikman, G. C. L. 3 1994-1997 B¨orngen, F. 437 (161) 1961-1995 Akiyama, M. 14 (10) 1989-1999 Borrelly, A. 19 1866-1894 Albitskij, V. A. 10 1923-1925 Bourgeois, P. 1 1929 Aldering, G. 3 1982 Bowell, E. 563 (6) 1977-1994 Alikoski, H. 13 1938-1953 Boyer, L. 40 1930-1952 Alu, J. 20 (11) 1987-1993 Brady, J. L. 1 1952 Amburgey, L. L. 1 1997 Brady, N. 1 2000 Andrews, A. D. 1 1965 Brady, S. 1 1999 Antal, M. 17 1971-1988 Brandeker, A. 1 2000 Antonini, P. 25 (1) 1996-1999 Brcic, V. 2 (2) 1995 Aoki, M. 1 1996 Broughton, J. 179 1997-2002 Arai, M. 43 (43) 1988-1991 Brown, J. A. 1 (1) 1990 Arend, S. 51 1929-1961 Brown, M. E. 1 (1) 2002 Armstrong, C. 1 (1) 1997 Broˇzek, L. 23 1979-1982 Armstrong, M. 2 (1) 1997-1998 Bruton, J. 1 1997 Asami, A. 5 1997-1999 Bruton, W. D. 2 (2) 1999-2000 Asher, D. J. 9 1994-1995 Bruwer, J. A. 4 1953-1970 Augustesen, K. 26 (26) 1982-1987 Buchar, E. 1 1925 Buie, M. W. 13 (1) 1997-2001 Baade, W. 10 1920-1949 Buil, C. 4 1997 Babiakov´a, U. 4 (4) 1998-2000 Burleigh, M. R. 1 (1) 1998 Bailey, S. I. 1 1902 Burnasheva, B. A. 13 1969-1971 Balam, D. -
The Planetary and Lunar Ephemeris DE 421
IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence. -
Astrometric Asteroid Masses: a Simultaneous Determination
A&A 565, A56 (2014) Astronomy DOI: 10.1051/0004-6361/201322766 & c ESO 2014 Astrophysics Astrometric asteroid masses: a simultaneous determination Edwin Goffin Aartselaarstraat 14, 2660 Hoboken, Belgium e-mail: [email protected] Received 27 September 2013 / Accepted 18 March 2014 ABSTRACT Using over 89 million astrometric observations of 349 737 numbered minor planets, an attempt was made to determine the masses of 230 of them by simultaneously solving for corrections to all orbital elements and the masses. For 132 minor planets an acceptable result was obtained, 49 of which appear to be new. Key words. astrometry – celestial mechanics – minor planets, asteroids: general 1. Introduction substantial number of test asteroids (349 737). Section 2 explains the basic principles and problems of simultaneous asteroid mass The astrometric determination of asteroid masses is the tech- determination and in Sect. 3 the details of the actual calculations nique of calculating the mass of asteroids (hereafter called “per- are given. Section 4 briefly deals with the observations used and turbing asteroids” or “perturbers”) from the gravitational pertur- explains the statistical analysis of the residuals that was used to bations they exert on the motion of other asteroids (called “test assign weights to, or reject observations. In Sect. 5 the results asteroids”). are presented and Sect. 6 discusses them. The usual procedure to calculate the mass of one aster- Throughout this paper, asteroid masses are expressed in units oid is, first, to identify potential test asteroids by searching −10 of 10 solar masses (M) and generally given to 3 decimal for close approaches with the perturbing asteroids and then places. -
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
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). -
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. -
The Minor Planet Bulletin Are Indexed in the Astrophysical Data System (ADS) and So Can Be Referenced by Others in Subsequent Papers
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 4, A.D. 2017 OCTOBER-DECEMBER 287. PHOTOMETRIC OBSERVATIONS OF MAIN-BELT were operated at sensor temperature of –15°C and images were ASTEROIDS 1990 PILCHER AND 8443 SVECICA calibrated with dark and flat-field frames. Stephen M. Brincat Both telescopes and cameras were controlled remotely from a Flarestar Observatory (MPC 171) nearby location via Sequence Generator Pro (Binary Star Fl.5/B, George Tayar Street Software). Photometric reduction, lightcurve construction, and San Gwann SGN 3160, MALTA period analyses were done using MPO Canopus software (Warner, [email protected] 2017). Differential aperture photometry was used and photometric measurements were based on the use of comparison stars of near- Winston Grech solar colour that were selected by the Comparison Star Selector Antares Observatory (CSS) utility available through MPO Canopus. Asteroid 76/3, Kent Street magnitudes were based on MPOSC3 catalog supplied with MPO Fgura FGR 1555, MALTA Canopus. (Received: 2017 June 8) 1990 Pilcher is an inner main-belt asteroid that was discovered on 1956 March 9 by K. Reinmuth at Heidelberg. Also known as 1956 We report on photometric observations of two main-belt EE, this asteroid was named in honor of Frederick Pilcher, asteroids, 1990 Pilcher and 8443 Svecica, that were associate professor of physics at Illinois College, Jacksonville acquired from 2017 March to May. We found the (Illinois), who has promoted extensively, the interest in minor synodic rotation period of 1990 Pilcher as 2.842 ± planets among amateur astronomers (Schmadel & Schmadel, 0.001 h and amplitude of 0.08 ± 0.03 mag and of 8443 1992). -
Accepted by Signature Redacted Richard P
A Near-Ultraviolet Spectroscopic Survey of B-Type Asteroids by Ashley J. Peter Submitted to the Department of Earth, Atmospheric and Planetary Sciences in Partial Fulfillment of the Requirements for the Degree of Bachelor of Science in Earth, Atmospheric and Planetary Sciences at the Massachusetts Institute of Technology May 13, 2015 1 y 5 2015 Ashley J. Peter. All rights reserved. The author hereby grants to MIT permission to reproduce and to distribute publicly paper and electronic copies of this thesis document in whole or in part in any medium now known or hereafter created. Author Signature redacted Department of Earth, Atmospheric and Planetary Sciences May 13, 2015 Certified by Signature redacted Richard P. Binzel Thesis Supervisor Accepted by_ Signature redacted Richard P. Binzel ARCHIVES Chair, Committee on Undergraduate Program nn/AOOA INMui TUTE OF TECHNOLOGY SEP 2 8 2017 LIBRARIES A Near-Ultraviolet Spectroscopic Survey of B-Type Asteroids Ashley J. Peter Advisors Julia de Le6n, PhD Instituto de Astroffsica de Canarias, Universidad de La Laguna Javier Licandro, PhD Instituto de Astrofisica de Canarias Richard P. Binzel, PhD Massachusetts Institute of Technology Abstract This study aimed to evaluate the presence of spectral slope variations of B-type asteroids in the near-ultraviolet wavelength range and further compare variations to those found in the near-infrared (de Le6n et al., 2012) and infrared (All-Lagoa et al., 2013). New observations of 19 B-type asteroids were obtained using the Telescopio Nazionale Galileo (TNG) and additional observations were collected on the William Herschel Telescope (WHT) and Isaac Newton Telescope (INT). After identifying appropriate solar analogs for spectral reduction, it was found that 1) not all asteroids are B-types as classified by the M4AST online tool (Popescu et al., 2012), and 2) spectral slope variations were present amongst the B-type asteroids.