Catalogue of Minor Planet Names and Discovery Circumstances
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Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. -
On the V-Type Asteroids Outside the Vesta Family. I. Interplay Of
Astronomy & Astrophysics manuscript no. carruba September 16, 2018 (DOI: will be inserted by hand later) On the V-type asteroids outside the Vesta family I. Interplay of nonlinear secular resonances and the Yarkovsky effect: the cases of 956 Elisa and 809 Lundia V. Carruba1, T. A. Michtchenko1 , F. Roig2, S. Ferraz-Mello1, and D. Nesvorn´y3, 1 IAG, Universidade de S˜ao Paulo, S˜ao Paulo, SP 05508-900, Brazil e-mail: [email protected] 2 Observat´orio Nacional, Rio de Janeiro, RJ 20921-400, Brazil e-mail: [email protected] 3 Southwest Research Institute, Department of Space Studies, Boulder, Colorado 80302 e-mail: [email protected] Received May 2nd 2005; accepted June 22nd 2005. Abstract. Among the largest objects in the main belt, asteroid 4 Vesta is unique in showing a basaltic crust. It is also the biggest member of the Vesta family, which is supposed to originate from a large cratering event about 1 Gyr ago (Marzari et al. 1996). Most of the members of the Vesta family for which a spectral classification is available show a V-type spectra. Due to their characteristic infrared spectrum, V-type asteroids are easily distinguished. Before the discovery of 1459 Magnya (Lazzaro et al. 2000) and of several V-type NEA (Xu 1995), all the known V-type asteroids were members of the Vesta family. Recently two V-type asteroids, 809 Lundia and 956 Elisa, (Florczak et al. 2002) have been discovered well outside the limits of the family, near the Flora family. We currently know 22 V-type asteroids outside the family, in the inner asteroid belt (see Table 2). -
Binary Minor Planets
ANRV273-EA34-03 ARI 17 April 2006 23:17 Binary Minor Planets Derek C. Richardson and Kevin J. Walsh Department of Astronomy, University of Maryland, College Park, Maryland 20740-2421; email: [email protected], [email protected] Annu. Rev. Earth Planet. Sci. Key Words 2006. 34:47–81 First published online as a asteroids, comets, evolution, origin, satellites Review in Advance on October 31, 2005 Abstract The Annual Review of A review of observations and theories regarding binary asteroids and binary trans- by University of Central Florida on 10/27/08. For personal use only. Earth and Planetary Science Neptunian objects [collectively, binary minor planets (BMPs)] is presented. To date, is online at earth.annualreviews.org these objects have been discovered using a combination of direct imaging, lightcurve analysis, and radar. They are found throughout the Solar System, and present a chal- doi: 10.1146/ Annu. Rev. Earth Planet. Sci. 2006.34:47-81. Downloaded from arjournals.annualreviews.org annurev.earth.32.101802.120208 lenge for theorists modeling their formation in the context of Solar System evolution. The most promising models invoke rotational disruption for the smallest, shortest- Copyright c 2006 by Annual Reviews. All rights lived objects (the asteroids nearest to Earth), consistent with the observed fast rotation reserved of these bodies; impacts for the larger, longer-lived asteroids in the main belt, con- 0084-6597/06/0530- sistent with the range of size ratios of their components and slower rotation rates; 0047$20.00 and mutual capture for the distant, icy, trans-Neptunian objects, consistent with their large component separations and near-equal sizes. -
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. -
1922MNRAS..82..149G Jan. 1922. Long-Period Inequalities In
Jan. 1922. Long-Period Inequalities in Movements of Asteroids. 149 In the case = an integer ~ is a multiple of and the solutions X2 X2 a1 1922MNRAS..82..149G with period nearly equal to — may also be regarded as periodic solution» Ai with period nearly equal to —-. A . But we have not been able (in the case when ^ is an integer) to A2 prove the existence of periodic solutions with period ^ which are not A2 • • • 2 TT at the same time periodic with period nearly equal to — . Ax Note.—The above work was completed in 1920 November, before the appearance of Moulton’s Periodic Orbits. The details of the exist- ence proofs are different from those of Buck, and it is hoped that they may be of interest. In Buck’s paper, which apparently was completed in 1912 or earlier, the equations of motion are transformed and the jacobians take a relatively simple form. In this paper only two of the families of periodic orbits treated by Buck are discussed. A full account of the other families, and also of the actual development in series of the periodic solutions, is given in Back’s paper. On Long-Period Inequalities in the Movements of Asteroids ivhose Mean Motions are nearly half that of Mars. By Wt M. H. Greaves, B. A., Isaac Newton Student in the University of Cambridge. (Communicated by Professor H. F. Baker.) In the ordinary theory of the movements of the planets as developed by Laplace and Le Verrier, the equations of motion are integrated by a method of successive approximation with regard to the masses. -
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). -
A Handbook of Double Stars, with a Catalogue of Twelve Hundred
The original of this bool< is in the Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924064295326 3 1924 064 295 326 Production Note Cornell University Library pro- duced this volume to replace the irreparably deteriorated original. It was scanned using Xerox soft- ware and equipment at 600 dots per inch resolution and com- pressed prior to storage using CCITT Group 4 compression. The digital data were used to create Cornell's replacement volume on paper that meets the ANSI Stand- ard Z39. 48-1984. The production of this volume was supported in part by the Commission on Pres- ervation and Access and the Xerox Corporation. Digital file copy- right by Cornell University Library 1991. HANDBOOK DOUBLE STARS. <-v6f'. — A HANDBOOK OF DOUBLE STARS, WITH A CATALOGUE OF TWELVE HUNDRED DOUBLE STARS AND EXTENSIVE LISTS OF MEASURES. With additional Notes bringing the Measures up to 1879, FOR THE USE OF AMATEURS. EDWD. CROSSLEY, F.R.A.S.; JOSEPH GLEDHILL, F.R.A.S., AND^^iMES Mt^'^I^SON, M.A., F.R.A.S. "The subject has already proved so extensive, and still ptomises so rich a harvest to those who are inclined to be diligent in the pursuit, that I cannot help inviting every lover of astronomy to join with me in observations that must inevitably lead to new discoveries." Sir Wm. Herschel. *' Stellae fixac, quae in ccelo conspiciuntur, sunt aut soles simplices, qualis sol noster, aut systemata ex binis vel interdum pluribus solibus peculiari nexu physico inter se junccis composita. -
Arecibo Radar Observations of 14 High-Priority Near-Earth Asteroids in CY2020 and January 2021 Patrick A
Arecibo Radar Observations of 14 High-Priority Near-Earth Asteroids in CY2020 and January 2021 Patrick A. Taylor (LPI, USRA), Anne K. Virkki, Flaviane C.F. Venditti, Sean E. Marshall, Dylan C. Hickson, Luisa F. Zambrano-Marin (Arecibo Observatory, UCF), Edgard G. Rivera-Valent´ın, Sriram S. Bhiravarasu, Betzaida Aponte-Hernandez (LPI, USRA), Michael C. Nolan, Ellen S. Howell (U. Arizona), Tracy M. Becker (SwRI), Jon D. Giorgini, Lance A. M. Benner, Marina Brozovic, Shantanu P. Naidu (JPL), Michael W. Busch (SETI), Jean-Luc Margot, Sanjana Prabhu Desai (UCLA), Agata Rozek˙ (U. Kent), Mary L. Hinkle (UCF), Michael K. Shepard (Bloomsburg U.), and Christopher Magri (U. Maine) Summary We propose the continuation of the long-running project R3037 to physically and dynamically characterize the population of near-Earth asteroids with the Arecibo S-band (2380 MHz; 12.6 cm) planetary radar system. The objectives of project R3037 are to: (1) collect high-resolution radar images of and (2) report ultra-precise radar astrometry for the strongest predicted radar targets for the 2020 calendar year plus early January 2021. Such images will be used for three-dimensional shape modeling as the data sets allow. These observations will be carried out as part of the NASA- funded Arecibo planetary radar program, Grant No. 80NSSC19K0523, to PI Anne Virkki (Arecibo Observatory, University of Central Florida) with Patrick Taylor as Institutional PI at the Lunar and Planetary Institute (Universities Space Research Association). Background Radar is arguably the most powerful Earth-based technique for post-discovery physical and dynamical characterization of near-Earth asteroids (NEAs) and plays a crucial role in the nation’s planetary defense initiatives led through the NASA Planetary Defense Coordination Office. -
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. -
Dynamical Erosion of the Asteroid Belt and Implications for Large Impacts in the Inner Solar System
Icarus 207 (2010) 744–757 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System David A. Minton *, Renu Malhotra Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, United States article info abstract Article history: The cumulative effects of weak resonant and secular perturbations by the major planets produce chaotic Received 15 September 2009 behavior of asteroids on long timescales. Dynamical chaos is the dominant loss mechanism for asteroids Revised 2 December 2009 with diameters D J 10 km in the current asteroid belt. In a numerical analysis of the long-term evolution Accepted 3 December 2009 of test particles in the main asteroid belt region, we find that the dynamical loss history of test particles Available online 11 December 2009 from this region is well described with a logarithmic decay law. In our simulations the loss rate function that is established at t 1 Myr persists with little deviation to at least t ¼ 4 Gyr. Our study indicates that Keywords: the asteroid belt region has experienced a significant amount of depletion due to this dynamical erosion— Asteroids having lost as much as 50% of the large asteroids—since 1 Myr after the establishment of the current Asteroids, Dynamics Cratering dynamical structure of the asteroid belt. Because the dynamical depletion of asteroids from the main belt is approximately logarithmic, an equal amount of depletion occurred in the time interval 10–200 Myr as in 0.2–4 Gyr, roughly 30% of the current number of large asteroids in the main belt over each interval. -
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. -
Asteroid Pairs: a Complex Picture
Asteroid pairs: a complex picture P. Pravec a, P. Fatka a,b, D. Vokrouhlick´y b, P. Scheirich a, J. Durechˇ b, D. J. Scheeres c, P. Kuˇsnir´ak a, K. Hornoch a, A. Gal´ad d, D. P. Pray e, Yu. N. Krugly f, O. Burkhonov g, Sh. A. Ehgamberdiev g, J. Pollock h, N. Moskovitz i, J. L. Ortiz j, N. Morales j, M. Hus´arik k, R. Ya. Inasaridze ℓ,m, J. Oey n, D. Polishook o, J. Hanuˇs b, H. Kuˇc´akov´a a,b, J. Vraˇstil b, J. Vil´agi d, S.ˇ Gajdoˇs d, L. Kornoˇs d, P. Vereˇs d,p, N. M. Gaftonyuk q, T. Hromakina f, A. V. Sergeyev f, I. G. Slyusarev f, V. R. Ayvazian ℓ,m, W. R. Cooney r, J. Gross r, D. Terrell r,s, F. Colas t, F. Vachier t, S. Slivan u, B. Skiff i, F. Marchis af,w, K. E. Ergashev g, D.-H. Kim x,y A. Aznar z, M. Serra-Ricart aa,ab, R. Behrend ac, R. Roy ad, F. Manzini ae, I. E. Molotov af aAstronomical Institute, Academy of Sciences of the Czech Republic, Friˇcova 1, CZ-25165 Ondˇrejov, Czech Republic bInstitute of Astronomy, Charles University, Prague, V Holeˇsoviˇck´ach 2, CZ-18000 Prague 8, Czech Republic cDepartment of Aerospace Engineering Sciences, The University of Colorado at Boulder, Boulder, CO, USA dModra Observatory, Department of Astronomy, Physics of the Earth, and Meteorology, FMPI UK, Bratislava SK-84248, Slovakia eSugarloaf Mountain Observatory, South Deerfield, MA, USA f Institute of Astronomy of Kharkiv National University, Sumska Str.