Perturbations in the Motion of the Quasicomplanar Minor Planets For
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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. -
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. -
The Minor Planet Bulletin and How the Situation Has Gone from One Mt Tarana Observatory of Trying to Fill Pages to One of Fitting Everything In
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 2, A.D. 2006 APRIL-JUNE 29. PHOTOMETRY OF ASTEROIDS 133 CYRENE, adjusted up or down to line up with the V-band data). The near- 454 MATHESIS, 477 ITALIA, AND 2264 SABRINA perfect overlay of V- and R-band data show no evidence of color change as the asteroid rotates. This result replicates the lightcurve Robert K. Buchheim period reported by Harris et al. (1984), and matches the period and Altimira Observatory lightcurve shape reported by Behrend (2005) at his website. 18 Altimira, Coto de Caza, CA 92679 USA [email protected] (Received: 4 November Revised: 21 November) Photometric studies of asteroids 133 Cyrene, 454 Mathesis, 477 Italia and 2264 Sabrina are reported. The lightcurve period for Cyrene of 12.707±0.015 h (with amplitude 0.22 mag) confirms prior studies. The lightcurve period of 8.37784±0.00003 h (amplitude 0.32 mag) for Mathesis differs from previous studies. For Italia, color indices (B-V)=0.87±0.07, (V-R)=0.48±0.05, and phase curve parameters H=10.4, G=0.15 have been determined. For Sabrina, this study provides the first reported lightcurve period 43.41±0.02 h, with 0.30 mag amplitude. Altimira Observatory, located in southern California, is equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron NexStar- 454 Mathesis. DiMartino et al. (1994) reported a rotation period of 11 operating at F/6.3), and CCD imager (ST-8XE NABG, with 7.075 h with amplitude 0.28 mag for this asteroid, based on two Johnson-Cousins filters). -
The British Astronomical Association Handbook 2017
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2017 2016 October ISSN 0068–130–X CONTENTS PREFACE . 2 HIGHLIGHTS FOR 2017 . 3 CALENDAR 2017 . 4 SKY DIARY . .. 5-6 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 – EXPLANATION 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 . 45-50 ASTEROID OCCULTATIONS .. ... 51-53 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; λ Tauri) . 100-101 MIRA STARS . 102 VARIABLE STAR OF THE YEAR (T Cassiopeiæ) . .. 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: Northern Lights - taken from Mount Storsteinen, near Tromsø, on 2007 February 14. A great effort taking a 13 second exposure in a wind chill of -21C (Pete Lawrence) British Astronomical Association HANDBOOK FOR 2017 NINETY–SIXTH YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 PREFACE Welcome to the 96th Handbook of the British Astronomical Association. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
~XECKDING PAGE BLANK WT FIL,,Q
1,. ,-- ,-- ~XECKDING PAGE BLANK WT FIL,,q DYNAMICAL EVIDENCE REGARDING THE RELATIONSHIP BETWEEN ASTEROIDS AND METEORITES GEORGE W. WETHERILL Department of Temcltricrl kgnetism ~amregie~mtittition of Washington Washington, D. C. 20025 Meteorites are fragments of small solar system bodies (comets, asteroids and Apollo objects). Therefore they may be expected to provide valuable information regarding these bodies. How- ever, the identification of particular classes of meteorites with particular small bodies or classes of small bodies is at present uncertain. It is very unlikely that any significant quantity of meteoritic material is obtained from typical ac- tive comets. Relatively we1 1-studied dynamical mechanisms exist for transferring material into the vicinity of the Earth from the inner edge of the asteroid belt on an 210~-~year time scale. It seems likely that most iron meteorites are obtained in this way, and a significant yield of complementary differec- tiated meteoritic silicate material may be expected to accom- pany these differentiated iron meteorites. Insofar as data exist, photometric measurements support an association between Apollo objects and chondri tic meteorites. Because Apol lo ob- jects are in orbits which come close to the Earth, and also must be fragmented as they traverse the asteroid belt near aphel ion, there also must be a component of the meteorite flux derived from Apollo objects. Dynamical arguments favor the hypothesis that most Apollo objects are devolatilized comet resiaues. However, plausible dynamical , petrographic, and cosmogonical reasons are known which argue against the simple conclusion of this syllogism, uiz., that chondri tes are of cometary origin. Suggestions are given for future theoretical , observational, experimental investigations directed toward improving our understanding of this puzzling situation. -
And X-Class Asteroids. II. Summary and Synthesis
Icarus 208 (2010) 221–237 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus A radar survey of M- and X-class asteroids II. Summary and synthesis Michael K. Shepard a,*, Beth Ellen Clark b, Maureen Ockert-Bell b, Michael C. Nolan c, Ellen S. Howell c, Christopher Magri d, Jon D. Giorgini e, Lance A.M. Benner e, Steven J. Ostro e, Alan W. Harris f, Brian D. Warner g, Robert D. Stephens h, Michael Mueller i a Bloomsburg University, 400 E. Second St., Bloomsburg, PA 17815, USA b Ithaca College, 267 Center for Natural Sciences, Ithaca, NY 14853, USA c NAIC/Arecibo Observatory, HC 3 Box 53995, Arecibo, PR 00612, USA d University of Maine at Farmington, 173 High Street, Preble Hall, ME 04938, USA e Jet Propulsion Laboratory, Pasadena, CA 91109, USA f Space Science Institute, La Canada, CA 91011-3364, USA g Palmer Divide Observatory/Space Science Institute, Colorado Springs, CO 80908, USA h Santana Observatory, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA i Observatoire de la Côte d’Azur, B.P. 4229, 06304 NICE Cedex 4, France article info abstract Article history: Using the S-band radar at Arecibo Observatory, we observed six new M-class main-belt asteroids (MBAs), Received 21 September 2009 and re-observed one, bringing the total number of Tholen M-class asteroids observed with radar to 19. Revised 12 January 2010 The mean radar albedo for all our targets is r^ OC ¼ 0:28 Æ 0:13, significantly higher than the mean radar Accepted 14 January 2010 albedo of every other class (Magri, C., Nolan, M.C., Ostro, S.J., Giorgini, J.D. -
WG Photometry and Polarimetry of Asteroids
PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION Abstracts The International Workshop -2 80 0 60 2 40 4 20 6 Relative Magnitude Polarization Degree 0 8 10 -20 0 20 40 60 80 100 120 140 160 180 Phase Angle June 15–18, 2003, Kharkiv, Ukraine Organized by Research Institute of Astronomy of V. N. Karazin Kharkiv National University, Ukrainian Astronomical Association Ministry of Education and Science of Ukraine Sponsored by Kharkiv City Charity Fund “AVEC” PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION The International Workshop June 15–18, 2003 Kharkiv, Ukraine A B S T R A C T S The Organizing Committee: Lupishko Dmitrij (co-Chairman), Kiselev Nikolai (co-Chairman), Belskaya Irina, Krugly Yurij, Shevchenko Vasilij, Velichko Fiodor, Luk’yanyk Igor Kharkiv - 2003 2 Contents Belskaya I.N., Shevchenko V.G., Efimov Yu.S., Shakhovskoj N.M., Gaftonyuk N.M., Krugly Yu.N., Chiorny V.G. Opposition Polarimetry and Photometry of Asteroids 5 Bochkov V.V., Prokof’eva V.V. Spectrophotometric Observations of Asteroids in the Crimean Astrophysical Observatory 6 Butenko G., Gerashchenko O., Ivashchenko Yu., Kazantsev A., Koval’chuk G., Lokot V. Estimates of Rotation Periods of Asteroids Derived from CCD- Observations in Andrushivka Astronomical Observatory 7 Bykov O.P., L'vov V.N. Method of accuracy estimation of asteroid positional CCD observations and results its application with EPOS Software 7 Cellino A., Gil Hutton R., Di Martino M., Tedesco E.F., Bendjoya Ph. Polarimetric Observations of Asteroids with the Torino UBVRI Photopolarimeter 9 Chiorny V.G., Shevchenko V.G., Krugly Yu.N., Velichko F.P., Gaftonyuk N.M. -
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. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
From Natural Philosophy to Natural Science: the Entrenchment of Newton's Ideal of Empirical Success
From Natural Philosophy to Natural Science: The Entrenchment of Newton's Ideal of Empirical Success Pierre J. Boulos Graduate Pro gram in Philosophy Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy Faculty of Graduate Studies The Universly of Western Ontario London, Ontario April 1999 O Pierre J- Boulos 1999 National Library Bibliotheque nationale of Canada du Canada Acquisitions and Acquisitions et Bibliographic Services services bibliographiques 395 Wellington Street 395, rue Wellington Ottawa ON KIA ON4 Ottawa ON KIA ON4 Canada Canada Your Me Voue reference Our file Notre rddrence The author has granted a non- L'auteur a accorde me licence non exclusive licence dowing the exclusive pennettant a la National Library of Canada to Bibliotheque nationale du Canada de reproduce, loan, distribute or sell reproduire, preter, distribuer ou copies of this thesis in microform, vendre des copies de cette these sous paper or electronic formats. la forme de microfiche/£ih, de reproduction sur papier ou sur format electronique. The author retains ownership of the L'auteur conserve la propriete du copyright in this thesis. Neither the droit d'auteur qui protege cette these. thesis nor substantial extracts &om it Ni la these ni des extraits substantieis may be printed or otherwise de celle-ci ne doivent Stre imprimes reproduced without the author's ou autrement reproduits sans son permission. autorisation. ABSTRACT William Harper has recently proposed that Newton's ideal of empirical success as exempli£ied in his deductions fiom phenomena informs the transition fiom natural philosophy to natural science. This dissertation examines a number of methodological themes arising fiom the Principia and that purport to exemplifjr Newton's ideal of empirical success. -
IRTF Spectra for 17 Asteroids from the C and X Complexes: a Discussion of Continuum Slopes and Their Relationships to C Chondrites and Phyllosilicates ⇑ Daniel R
Icarus 212 (2011) 682–696 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus IRTF spectra for 17 asteroids from the C and X complexes: A discussion of continuum slopes and their relationships to C chondrites and phyllosilicates ⇑ Daniel R. Ostrowski a, Claud H.S. Lacy a,b, Katherine M. Gietzen a, Derek W.G. Sears a,c, a Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, United States b Department of Physics, University of Arkansas, Fayetteville, AR 72701, United States c Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, AR 72701, United States article info abstract Article history: In order to gain further insight into their surface compositions and relationships with meteorites, we Received 23 April 2009 have obtained spectra for 17 C and X complex asteroids using NASA’s Infrared Telescope Facility and SpeX Revised 20 January 2011 infrared spectrometer. We augment these spectra with data in the visible region taken from the on-line Accepted 25 January 2011 databases. Only one of the 17 asteroids showed the three features usually associated with water, the UV Available online 1 February 2011 slope, a 0.7 lm feature and a 3 lm feature, while five show no evidence for water and 11 had one or two of these features. According to DeMeo et al. (2009), whose asteroid classification scheme we use here, 88% Keywords: of the variance in asteroid spectra is explained by continuum slope so that asteroids can also be charac- Asteroids, composition terized by the slopes of their continua.