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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. -
The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes. -
Asteroids DOI: 10.17794/Rgn.2016.1.5
The Mining-Geology-Petroleum Engineering Bulletin UDC: 523.6 Asteroids DOI: 10.17794/rgn.2016.1.5 Review scientific paper Željko Andreić1; 1University of Zagreb, Faculty of Mining, Geology and Petroleum Engineering, Pierottijeva 6, 10000 Zagreb, Croatia, full professor Abstract Asteroids are the largest minor bodies in the Solar System. Nowadays they are in the research focus due to several facts about them: first, a subclass of asteroids can collide with Earth, and consequences of such a collision are dramatic. Second, they are now seen as source of materials that are becoming scarce on Earth, and they will be needed in future space constructions anyway. Third, they are holding clues about the origin and evolution of the Solar System. In this article, a short overview of current knowledge about asteroids is presented. Last, but not least, as several Croatian scientists were recently honored by naming an asteroid after them, a short overview of the naming process is given. Keywords Solar System, asteroids, mining the asteroids 1. Introduction Even today, some textbooks describe the Solar System as a quiet, highly ordered structure. The Sun is in the center and planets revolve around it on neat elliptical orbits that are assumed to be the same since the time of creation of the Solar System. The space in between (the interplanetary space) is mostly empty, permeated by a very rarefied gas called solar wind that is peppered with a few grains of dust. Asteroids may be revealed as smaller bodies contained in the so-called asteroidal belt between Mars and Jupiter. And, beyond the last planet, Pluto, there is just cold, empty, interstellar space. -
The Minor Planet Bulletin Lost a Friend on Agreement with That Reported by Ivanova Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 3, A.D. 2006 JULY-SEPTEMBER 49. LIGHTCURVE ANALYSIS FOR 19848 YEUNGCHUCHIU Kwong W. Yeung Desert Eagle Observatory P.O. Box 105 Benson, AZ 85602 [email protected] (Received: 19 Feb) The lightcurve for asteroid 19848 Yeungchuchiu was measured using images taken in November 2005. The lightcurve was found to have a synodic period of 3.450±0.002h and amplitude of 0.70±0.03m. Asteroid 19848 Yeungchuchiu was discovered in 2000 Oct. by the author at Desert Beaver Observatory, AZ, while it was about one degree away from Jupiter. It is named in honor of my father, The amplitude of 0.7 magnitude indicates that the long axis is Yeung Chu Chiu, who is a businessman in Hong Kong. I hoped to about 2 times that of the shorter axis, as seen from the line of sight learn the art of photometry by studying the lightcurve of 19848 as at that particular moment. Since both the maxima and minima my first solo project. have similar “height”, it’s likely that the rotational axis was almost perpendicular to the line of sight. Using a remote 0.46m f/2.8 reflector and Apogee AP9E CCD camera located in New Mexico Skies (MPC code H07), images of Many amateurs may have the misconception that photometry is a the asteroid were obtained on the nights of 2005 Nov. 20 and 21. very difficult science. After this learning exercise I found that, at Exposures were 240 seconds. -
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) .................. -
Download Full Issue
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 47, NUMBER 1, A.D. 2020 JANUARY-MARCH 1. SECTION NEWS: COLLABORATIVE ASTEROID PHOTOMETRY FOR STAFFING CHANGES FOR ASTEROID 2051 CHANG THE MINOR PLANET BULLETIN Alessandro Marchini Frederick Pilcher Astronomical Observatory, DSFTA - University of Siena (K54) Minor Planets Section Recorder Via Roma 56, 53100 - Siena, ITALY [email protected] [email protected] One staffing change and one staffing addition for The Minor Planet Bulletin are announced effective with this issue. Riccardo Papini, Massimo Banfi, Fabio Salvaggio Wild Boar Remote Observatory (K49) MPB Distributor Derald Nye is now retired from his 37 years of San Casciano in Val di Pesa (FI), ITALY service to the Minor Planets Bulletin. Derald stepped in to service at the time the MPB made its transition from the original Editor Melissa N. Hayes-Gehrke, Eric Yates and Section founder, Richard G. Hodgson. As Derald reflected in Department of Astronomy, University of Maryland a short essay written in MPB 40, page 53 (2013), the Distributor College Park, MD, USA 20740 position was the longest job he ever held, having retired from being a programmer for 30 years with IBM. (Work for IBM (Received: 2019 October 15) included programming for the space program.) At its peak, Derald was managing nearly 200 subscriptions. That number dropped to Photometric observations of this main-belt asteroid were the dozen or so libraries maintaining a permanent collection conducted in order to determine its rotation period. The following the MPB transitioning to becoming an on-line electronic authors found a synodic rotation period of 12.013 ± journal with limited printing. -
Prediction of Transits of Solar System Objects In
Prediction of transits of solar system objects in Kepler /K2 images: An extension of the Virtual Observatory service SkyBoT Jérôme Berthier, B Carry, F Vachier, S Eggl, A Santerne To cite this version: Jérôme Berthier, B Carry, F Vachier, S Eggl, A Santerne. Prediction of transits of solar system objects in Kepler /K2 images: An extension of the Virtual Observatory service SkyBoT. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2016, 457 (3), 10.1093/mnras/stw492. hal-01278026 HAL Id: hal-01278026 https://hal.archives-ouvertes.fr/hal-01278026 Submitted on 23 Feb 2016 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. Copyright MNRAS 000,1{4 (2016) Preprint 23 February 2016 Compiled using MNRAS LATEX style file v3.0 Prediction of transits of solar system objects in Kepler/K2 images: An extension of the Virtual Observatory service SkyBoT J. Berthier,1? B. Carry,1;2 F. Vachier,1 S. Eggl,1 and A. Santerne,3 1IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universit´es, UPMC Univ Paris 06, Univ Lille, France 2Laboratoire Lagrange, Universit´ede Nice-Sophia Antipolis, CNRS, Observatoire de la C^ote d'Azur, France 3Instituto de Astrof´ısica e Ci^encias do Espa¸co, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal Accepted XXX. -
JRASC August 2006, High Resolution (PDF)
Publications and Products of August / août 2006 Volume/volume 100 Number/numéro 4 [719] 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 INSIDE THIS ISSUE elementary, middle school, and junior-high grades; fun and easy to use; cost-effective. -
LIGHTCURVE of 755 QUINTILLA the Nightly Zero-Point Was Determined by Imaging a Landolt Standard Field That Was Fortuitously Only a Few Degrees Away from Robert K
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 1, A.D. 2005 JANUARY-MARCH 1. LIGHTCURVE OF 755 QUINTILLA The nightly zero-point was determined by imaging a Landolt standard field that was fortuitously only a few degrees away from Robert K. Buchheim the asteroid, thereby avoiding the need to account for air mass Altimira Observatory (G76) difference. The standard field was measured in B, V, and R filters 18 Altimira, Coto de Caza, CA 92679 immediately before and after imaging of the asteroid. [email protected] The asteroid imaging sequence was V-R-B-B-R-V. During this Donald Pray 25-minute imaging sequence, the asteroid’s rotational phase Carbuncle Hill Observatory (I00) orientation (referring to Figure) ranged from 0.63 to 0.73, so the Greene, Rhode Island measured absolute magnitude during this sequence is quite close [email protected] to the mean brightness (averaged over the lightcurve). (Received: 27 June Revised: 3 September) The measured color indices were: (B-V) = 0.67 ± 0.03 (which is in good agreement with the Small Bodies Node), and (V-R) = 0.41 ± The lightcurve period of 755 Quintilla is 4.552 ± 0.001 0.03. The observed V = 14.61, when adjusted for distance from hours, with an amplitude of 0.38 mag. We also report the Earth and Sun gives a reduced magnitude of VR = 10.88 at color indices of B-V=0.67±0.03 and V-R=0.41±0.03. solar phase angle = 19.1 degrees. -
Prediction of Transits of Solar System Objects in Kepler/K2 Images: an Extension of the Virtual Observatory Service Skybot
MNRAS 458, 3394–3398 (2016) doi:10.1093/mnras/stw492 Advance Access publication 2016 March 2 Prediction of transits of Solar system objects in Kepler/K2 images: an extension of the Virtual Observatory service SkyBoT J. Berthier,1‹ B. Carry,1,2‹ F. Vachier,1 S. Eggl1 and A. Santerne3‹ 1IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites,´ UPMC Univ Paris 06, Univ Lille, France 2Laboratoire Lagrange, Universite´ de Nice-Sophia Antipolis, CNRS, Observatoire de la Coteˆ d’Azur, France 3Instituto de Astrof´ısica e Cienciasˆ do Espac¸o, Universidade do Porto, CAUP, Rua das Estrelas, P-4150-762 Porto, Portugal Accepted 2016 February 26. Received 2016 February 23; in original form 2016 February 4 ABSTRACT All the fields of the extended space mission Kepler/K2 are located within the ecliptic. Many Solar system objects thus cross the K2 stellar masks on a regular basis. We aim at providing to Downloaded from the entire community a simple tool to search and identify Solar system objects serendipitously observed by Kepler. The sky body tracker (SkyBoT) service hosted at Institut de mecanique´ celeste´ et de calcul des eph´ em´ erides´ provides a Virtual Observatory compliant cone search that lists all Solar system objects present within a field of view at a given epoch. To generate http://mnras.oxfordjournals.org/ such a list in a timely manner, ephemerides are pre-computed, updated weekly, and stored in a relational data base to ensure a fast access. The SkyBoT web service can now be used with Kepler. Solar system objects within a small (few arcminutes) field of view are identified and listed in less than 10 s. -
Prediction of Transits of Solar System Objects in Kepler/K2 Images: an Extension of the Virtual Observatory Service Skybot
MNRAS 000,1{6 (2016) Preprint 8 October 2018 Compiled using MNRAS LATEX style file v3.0 Prediction of transits of solar system objects in Kepler/K2 images: An extension of the Virtual Observatory service SkyBoT J. Berthier,1? B. Carry,1;2 F. Vachier,1 S. Eggl,1 and A. Santerne,3 1IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universit´es, UPMC Univ Paris 06, Univ Lille, France 2Laboratoire Lagrange, Universit´ede Nice-Sophia Antipolis, CNRS, Observatoire de la C^ote d'Azur, France 3Instituto de Astrof´ısica e Ci^encias do Espa¸co, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal Accepted XXX. Received YYY; in original form ZZZ ABSTRACT All the fields of the extended space mission Kepler/K2 are located within the ecliptic. Many solar system objects thus cross the K2 stellar masks on a regular basis. We aim at providing to the entire community a simple tool to search and identify solar system objects serendipitously observed by Kepler. The SkyBoT service hosted at IMCCE provides a Virtual Observatory (VO) compliant cone-search that lists all solar system objects present within a field of view at a given epoch. To generate such a list in a timely manner, ephemerides are pre-computed, updated weekly, and stored in a relational database to ensure a fast access. The SkyBoT Web service can now be used with Kepler. Solar system objects within a small (few arcminutes) field of view are identified and listed in less than 10 s. Generating object data for the entire K2 field of view (14◦) takes about a minute.