Against the Biases in Spins and Shapes of Asteroids
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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. -
New Cases of Unusual Polarimetric Behavior in Asteroids
A&A 482, 309–314 (2008) Astronomy DOI: 10.1051/0004-6361:20078965 & c ESO 2008 Astrophysics New cases of unusual polarimetric behavior in asteroids R. Gil-Hutton1,2, V. Mesa2, A. Cellino3, P. Bendjoya4, L. Peñaloza2,andF.Lovos2 1 Complejo Astronómico El Leoncito – CONICET, Av. España 1512 sur, J5402DSP San Juan, Argentina e-mail: [email protected] 2 Universidad Nacional de San Juan, J. I. de la Roza 590 oeste, 5400 Rivadavia, San Juan, Argentina 3 INAF, Osservatorio Astronomico di Torino, 10025 Pino Torinese (TO), Italy 4 Laboratoire Fizeau, UMR 6525 Université Nice Sophia Antipolis , Observatoire de la Côte d’Azur, CNRS, 06108 Nice Cedex 2, France Received 30 October 2007 / Accepted 5 February 2008 ABSTRACT Aims. Results of different polarimetric campaigns at Complejo Astronómico El Leoncito (Casleo), San Juan, Argentina are presented. The aim of these campaigns was to search for objects exhibiting anomalous polarimetric properties, similar to those shown by the Ld-class asteroid (234) Barbara, among members of the same or similar taxonomic classes. Methods. The data have been obtained with Torino and CASPROF polarimeters at the 2.15 m telescope. The Torino polarimeter is an instrument that allows simultaneous measurement of polarization in five different bands, and CASPROF polarimeter is a two-hole aperture polarimeter with rapid modulation. Results. The campaigns began in 2005, and we found four new asteroids with Barbara-like polarimetric properties: the L-class objects (172) Baucis, (236) Honoria and (980) Anacostia, and the K-class asteroid (679) Pax. The polarimetric properties of the phase-polarization curves of these objects may be produced by a mixture of high- and low-albedo particles in their regolith as a result of the fragmentation of a substrate that is spectrally analog to the CO3/CV3 chondrites. -
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). -
JRASC-2007-04-Hr.Pdf
Publications and Products of April / avril 2007 Volume/volume 101 Number/numéro 2 [723] The Royal Astronomical Society of Canada Observer’s Calendar — 2007 The award-winning RASC Observer's Calendar is your annual guide Created by the Royal Astronomical Society of Canada and richly illustrated by photographs from leading amateur astronomers, the calendar pages are packed with detailed information including major lunar and planetary conjunctions, The Journal of the Royal Astronomical Society of Canada Le Journal de la Société royale d’astronomie du Canada meteor showers, eclipses, lunar phases, and daily Moonrise and Moonset times. Canadian and U.S. holidays are highlighted. Perfect for home, office, or observatory. Individual Order Prices: $16.95 Cdn/ $13.95 US RASC members receive a $3.00 discount Shipping and handling not included. The Beginner’s Observing Guide Extensively revised and now in its fifth edition, The Beginner’s Observing Guide is for a variety of observers, from the beginner with no experience to the intermediate who would appreciate the clear, helpful guidance here available on an expanded variety of topics: constellations, bright stars, the motions of the heavens, lunar features, the aurora, and the zodiacal light. New sections include: lunar and planetary data through 2010, variable-star observing, telescope information, beginning astrophotography, a non-technical glossary of astronomical terms, and directions for building a properly scaled model of the solar system. Written by astronomy author and educator, Leo Enright; 200 pages, 6 colour star maps, 16 photographs, otabinding. Price: $19.95 plus shipping & handling. Skyways: Astronomy Handbook for Teachers Teaching Astronomy? Skyways Makes it Easy! Written by a Canadian for Canadian teachers and astronomy educators, Skyways is Canadian curriculum-specific; pre-tested by Canadian teachers; hands-on; interactive; geared for upper elementary, middle school, and junior-high grades; fun and easy to use; cost-effective. -
Perturbations in the Motion of the Quasicomplanar Minor Planets For
Publications of the Department of Astronom} - Beograd, N2 ID, 1980 UDC 523.24; 521.1/3 osp PERTURBATIONS IN THE MOTION OF THE QUASICOMPLANAR MI NOR PLANETS FOR THE CASE PROXIMITIES ARE UNDER 10000 KM J. Lazovic and M. Kuzmanoski Institute of Astronomy, Faculty of Sciences, Beograd Received January 30, 1980 Summary. Mutual gravitational action during proximities of 12 quasicomplanar minor pla nets pairs have been investigated, whose minimum distances were under 10000 km. In five of the pairs perturbations of several orbital elements have been stated, whose amounts are detectable by observations from the Earth. J. Lazovic, M. Kuzmanoski, POREMECAJI ELEMENATA KRETANJA KVAZIKOM PLANARNIH MALIH PLANETA U PROKSIMITETIMA NJIHOVIH PUTANJA SA DA LJINAMA MANJIM OD 10000 KM - Ispitali smo medusobna gravitaciona de;stva pri proksi mitetima 12 parova kvazikomplanarnih malih planeta sa minimalnim daljinama ispod 10000 km. Kod pet parova nadeni su poremecaji u vi~e putanjskih elemenata, ~iji bi se iznosi mogli ustano viti posmatranjima sa Zemlje. Earlier we have found out 13 quasicomplanar minor planets pairs (the angle I between their orbital planes less than O~500), whose minimum mutual distances (pmin) were less than 10000 km (Lazovic, Kuzmanoski, 1978). The shortest pro ximity distance of only 600 km among these pairs has been stated with minor planet pair (215) Oenone and 1851 == 1950 VA. The corresponding perturbation effects in this pair have been calculated (Lazovic, Kuzmanoski, 1979a). This motivated us to investigate the mutual perturbing actions in the 12 remaining minor planets pairs for the case they found themselves within the proximities of their correspon ding orbits. -
Modelling and Scaling Neglected Asteroids
Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Modelling and scaling neglected asteroids A. Marciniak1 with V. Alí-Lagoa, T. Müller, P. Bartczak, R. Behrend, M. Butkiewicz-B ˛ak, G. Dudzinski,´ R. Duffard, K. Dziadura, S. Fauvaud, M. Ferrais, S. Geier, J. Grice, R. Hirsch, J. Horbowicz, K. Kaminski,´ P. Kankiewicz, D.-H. Kim, M.-J. Kim, I. Konstanciak, V. Kudak, L. Molnár, F. Monteiro, W. Ogłoza, D. Oszkiewicz, A. Pál, N. Parley, F. Pilcher, E. Podlewska - Gaca, T. Polakis, J. J. Sanabria, T. Santana-Ros, B. Skiff, K. Sobkowiak, R. Szakáts, S. Urakawa, M. Zejmo,˙ K. Zukowski˙ 1. Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Poznan,´ Poland ESOP XXXIX, 29 August 2020 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Asteroid lightcurves (219) Thusnelda P = 59.74 h 487 Venetia P = 13.355h 2014 -2,1 Oct 11.1 Suhora 2012/2013 -2,2 Oct 12.1 Suhora Oct 29.0 Bor Oct 24.1 Bor. -2,05 Nov 10.2 Suh Oct 28.1 Bor. Nov 11.1 Suh CCCCCC Nov 4.0 Bor. CCCCCCCCC CC C C Nov 7.4 Organ M. Dec 28.8 Bor C Mar 2.8 Bor C Nov 8.4 Organ M. AAAA -2 Mar 3.8 Bor AAAAAA C Nov 13.4 Organ M. AAAA C CCC Nov 14.4 Organ M. A -2,1 AAA CCC A Nov 15.4 Organ M. A AA Nov 21.4 Winer -1,95 Dec 2.1 OAdM Dec 3.0 OAdM Dec 5.0 Bor. -
The Minor Planet Bulletin 44 (2017) 142
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin. -
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. -
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. -
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. -
Machine-Learning Identification of Asteroid Groups
MNRAS 488, 1377–1386 (2019) doi:10.1093/mnras/stz1795 Advance Access publication 2019 July 1 Machine-learning identification of asteroid groups V. Carruba ,1‹ S. Aljbaae2 and A. Lucchini1 1Sao˜ Paulo State University (UNESP), School of Natural Sciences and Engineering, Guaratingueta,´ SP, 12516-410, Brazil 2National Space Research Institute (INPE), Division of Space Mechanics and Control, C.P. 515, 12227-310, Sao˜ Jose´ dos Campos, SP, Brazil Accepted 2019 June 27. Received 2019 June 26; in original form 2019 May 7 Downloaded from https://academic.oup.com/mnras/article-abstract/488/1/1377/5526253 by guest on 23 September 2019 ABSTRACT Asteroid families are groups of asteroids that share a common origin. They can be the outcome of a collision or be the result of the rotational failure of a parent body or its satellites. Collisional asteroid families have been identified for several decades using hierarchical clustering methods (HCMs) in proper elements domains. In this method, the distance of an asteroid from a reference body is computed, and, if it is less than a critical value, the asteroid is added to the family list. The process is then repeated with the new object as a reference, until no new family members are found. Recently, new machine-learning clustering algorithms have been introduced for the purpose of cluster classification. Here, we apply supervised- learning hierarchical clustering algorithms for the purpose of asteroid families identification. The accuracy, precision, and recall values of results obtained with the new method, when compared with classical HCM, show that this approach is able to found family members with an accuracy above 89.5 per cent, and that all asteroid previously identified as family members by traditional methods are consistently retrieved.