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Astro‑Ph 2020.05.18‑05.22 2020.05.18 2020.05.19

astro‑ph 2020.05.18‑05.22 2020.05.18 Borysenko+, Astronomische Nachrichten – Broadband photometry of asteroid 6478 Gault: acvity and morphology hps://arxiv.org/pdf/2005.07270.pdf Acve Asteroids(AAs): small bodies with orbits typical of asteroids that exhibit cometary acvity (Jewi2012) 7968 Rlst (133P/Elst) is the ﬁrst AAs 2 dozens of Main Belt asteroids are resistered coma, tail by ice sublimaon → Main‑Belt Comet (MBCs) but some AAs have no more signs of acvity like 596 Scheila. the acvity of 596 Scheila is considered as collisional result, though collisional probability is very low Gault is a Phocaea family asteroid 2019 the tail caused by YORP spin up has been found V,R‑band photometry results of Gault 2020.05.19 Orz+, The large Trans‑Neptunian Object 2002 TC302 from combined stellar occultaon, photometry and astrometry data hps://arxiv.org/pdf/2005.08881.pdf characterizaon of large Trans‑Neptunian Objects 2002 TC302 occultaon with m_v ~ 15.3 star occurs on 28th Jan. 2018 12 occultaon results reveal the shape 543 km mes 460 km shape model has been created combined with light curve geometric albedo was edmated 0.147 from occultaon shape and abusolute magnitude no ring structure has been detected Batygin & Motbidelli, Formaon of Giant Planet Satellites hps://arxiv.org/pdf/2005.08330.pdf numerical simulaon about saelites formaon with both gas and dust in the circumplanetary disk (not pp‑disk) the result is consistent with the known property of Jovian and Saturnian moons (this paper result imply Nice model migraon is not necessarity needed for giant planets to get natural satellites ?) 2020.05.20 Heager, A trampoline eﬀect occurring in the stages of planetary reseeding hps://arxiv.org/pdf/2005.09360.pdf lithopanspermia theory refugium hypothesis(退避仮説) reseeding stage1, 2, 3 Arimatsu+, Evidence for a rapid decrease of Pluto’s atmospheric pressure revealed by a stellar occultaon in 2019 hps://arxiv.org/pdf/2005.09189.pdf occultaon by Plute on 2019 July 17 using CMOS camera mounted on the Tohoku Univ. 60cm telescope in Haleakala, Hawaii brapid pressure drop is detected at a 2.4 sigma level 2020.05.21 Kaasalainen+, Asteroid models from generalised projecons: Essenal facts for asteroid modellers and geometric inverse problem solvers hps://arxiv.org/pdf/2005.09947.pdf review of the problem of asteroid shape and spin various observaon about asteroids.

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Color Changes for the Surface of 6478 Gault (??) Submitted to Apjl
Draft version August 3, 2020 Typeset using LATEX twocolumn style in AASTeX63 Color changes for the Surface of 6478 Gault (??) 1 2 2 3 4 5 1 Remington Cantelas, Karen J. Meech, Jan T. Kleyna, Erica Bufanda, Alan Fitzsimmons, James Bauer, 2 2 2 6 2 2 Larry Denneau, Robert Weryk, Jacqueline V. Keane, Olivier R. Hainaut, and Richard J. Wainscoat 1 3 University of Central Florida, 4111 Libra Drive, Orlando, FL 32816, USA 2 4 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 3 5 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822 USA 4 6 Astrophysics Research Centre, Queen's University Belfast, Belfast BT7 1NN, UK 5 7 University of Maryland, Dept. of Astronomy, College Park, MD 20742-2421 USA 6 8 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München,Germany 9 Submitted to ApJL 10 ABSTRACT 11 (6478) Gault is a main belt asteroid in the Phocaea Family which was discovered to have activity in 12 January 2019, and precovery images reveal it has been consistently active since at least September 2013. 13 Gault's activity is believed to be caused by it being a fast rotator near the asteroid break-up limit. We 14 have collected images and photometry from several telescopes dating back several apparitions. Using 15 this data we attempt to produce a reliable rotational light curve and confirm Gault's rotation period. 16 We also investigate possible color variations on the surface of the asteroid by measuring it's spectral 17 reflectivity over the course of 7 months between January and August 2019.
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An Anisotropic Distribution of Spin Vectors in Asteroid Families
Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
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1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H.
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Multiple Outbursts of Asteroid (6478) Gault∗
Draft version March 14, 2019 Typeset using LATEX default style in AASTeX62 Multiple Outbursts of Asteroid (6478) Gault∗ 1, 2 3 4 5, 6, 5 Quanzhi Ye (叶泉志), Michael S. P. Kelley, Dennis Bodewits, Bryce Bolin, y Lynne Jones, Zhong-Yi Lin (林忠©),7 Eric C. Bellm,5 Richard Dekany,8 Dmitry A. Duev,1 Steven Groom,2 George Helou,2 Shrinivas R. Kulkarni,1 Thomas Kupfer,9 Frank J. Masci,2 Thomas A. Prince,1 and Maayane T. Soumagnac10 1Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, U.S.A. 2Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, U.S.A. 3Department of Astronomy, University of Maryland, College Park, MD 20742, U.S.A. 4Department of Physics, Auburn University, Auburn, AL 36849, U.S.A. 5DIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, U.S.A. 6B612 Asteroid Institute, 20 Sunnyside Ave, Suite 427, Mill Valley, CA 94941, U.S.A. 7Institute of Astronomy, National Central University, 32001, Taiwan 8Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, U.S.A. 9Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, U.S.A. 10Department of Particle Physics and Astrophysics, Weizmann Institute of Science 234 Herzl St., Rehovot, 76100, Israel (Received {; Revised {; Accepted {) Submitted to ApJL ABSTRACT Main-belt asteroid (6478) Gault unexpectedly sprouted two tails in late 2018 and early 2019, iden- tifying it as a new active asteroid. Here we present observations obtained by the 1.2-m Zwicky Tran- sient Facility survey telescope that provide detailed time-series coverage of the onset and evolution of Gault's activity.
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The Sporadic Activity of (6478) Gault: a YORP-Driven Event?
The Astrophysical Journal Letters, 874:L20 (7pp), 2019 April 1 https://doi.org/10.3847/2041-8213/ab0f40 © 2019. The American Astronomical Society. All rights reserved. The Sporadic Activity of (6478) Gault: A YORP-driven Event? Jan T. Kleyna1 , Olivier R. Hainaut2 , Karen J. Meech1 , Henry H. Hsieh3,4 , Alan Fitzsimmons5 , Marco Micheli6,7 , Jacqueline V. Keane1 , Larry Denneau1 , John Tonry1 , Aren Heinze1 , Bhuwan C. Bhatt8 , Devendra K. Sahu8 , Detlef Koschny6,9,10 , Ken W. Smith5 , Harald Ebeling1 , Robert Weryk1 , Heather Flewelling1 , and Richard J. Wainscoat1 1 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany 3 Planetary Science Institute, 1700 East Fort Lowell Road, Suite 106, Tucson, AZ 85719, USA 4 Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan 5 Astrophysics Research Centre, Queen’s University Belfast, Belfast BT7 1NN, UK 6 ESA NEO Coordination Centre, Largo Galileo Galilei, 1, I-00044 Frascati (RM), Italy 7 INAF—Osservatorio Astronomico di Roma, Via Frascati, 33, I-00040 Monte Porzio Catone (RM), Italy 8 Indian Institute for Astrophysics, II Block, Koramangala, Bangalore 560 034, India 9 ESTEC, European Space Agency, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands 10 Chair of Astronautics, Technical University of Munich, Boltzmannstraße 15, D-85748 Garching bei München, Germany Received 2019 February 22; revised 2019 March 13; accepted 2019 March 13; published 2019 April 1 Abstract On 2019 January 5 a streamer associated with the 4–10 km main belt asteroid (6478)Gault was detected by the ATLAS sky survey, a rare discovery of activity around a main belt asteroid.
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Asteroid Belt - Wikipedia
12/2/2018 Asteroid belt - Wikipedia Asteroid belt The asteroid belt is the circumstellar disc in the Solar System located roughly between the orbits of the planets Mars and Jupiter. It is occupied by numerous irregularly shaped bodies called asteroids or minor planets. The asteroid belt is also termed the main asteroid belt or main belt to distinguish it from other asteroid populations in the Solar System such as near-Earth asteroids and trojan asteroids.[1] About half the mass of the belt is contained in the four largest asteroids: Ceres, Vesta, Pallas, and Hygiea.[1] The total mass of the asteroid belt is approximately 4% that of the Moon, or 22% that of Pluto, and roughly twice that of Pluto's moon Charon (whose diameter is 1200 km). Ceres, the asteroid belt's only dwarf planet, is about 950 km in diameter, whereas 4 Vesta, 2 Pallas, and 10 Hygiea have mean diameters of less than 600 km.[2][3][4][5] The remaining bodies range down to the size of a dust particle. The asteroid material is so thinly distributed that numerous unmanned spacecraft have traversed it without incident.[6] Nonetheless, collisions between large asteroids do occur, and these can produce an asteroid family whose members have similar orbital characteristics and compositions. Individual asteroids within the asteroid belt are categorized by their spectra, with most falling into three basic groups: carbonaceous (C-type), silicate (S-type), and metal-rich (M-type). The asteroid belt formed from the primordial solar nebula as a group of planetesimals.[7] Planetesimals are the The asteroids of the inner Solar System and Jupiter: The donut-shaped asteroid belt is located smaller precursors of the protoplanets.
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Synthetic Tracking Using ZTF Deep Drilling Data Sets Chengxing Zhai1 , Quanzhi Ye2,3,4, Michael Shao1, Russell Trahan1, Navtej S
Publications of the Astronomical Society of the Pacific, 132:064502 (8pp), 2020 June https://doi.org/10.1088/1538-3873/ab828b © 2020. The Astronomical Society of the Pacific Printed in the U.S.A. Synthetic Tracking Using ZTF Deep Drilling Data Sets Chengxing Zhai1 , Quanzhi Ye2,3,4, Michael Shao1, Russell Trahan1, Navtej S. Saini1, Janice Shen1, Thomas A. Prince2, Eric C. Bellm5, Matthew J. Graham2 , George Helou3, Shrinivas R. Kulkarni2, Thomas Kupfer6, Russ R. Laher3, Ashish Mahabal2,3 , Frank J. Masci3 , Ben Rusholme3, Philippe Rosnet7, and David L. Shupe3 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr, Pasadena, CA 91109, USA; [email protected] 2 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 3 IPAC, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA 4 University of Maryland, Department of Astronomy, College Park, MD 20742, USA 5 DIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USA 6 Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 7 Université Clermont Auvergne, CNRS/IN2P3, LPC, Clermont-Ferrand, France Received 2020 January 13; accepted 2020 March 23; published 2020 April 21 Abstract The Zwicky Transit Facility (ZTF) is a powerful time domain survey telescope with a large field of view of 47 deg2. We apply the synthetic tracking technique to integrate a ZTF’s deep drilling data set, which consists of 133 nominal 30 s exposure frames spanning about 1.5 hr, to search for slowly moving asteroids down to approximately 23rd magnitude.
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Prezentácia Programu Powerpoint
VÝSKUM ASTEROIDOV A KOMÉT NA ASTRONOMICKOM ÚSTAVE SAV MAREK HUSÁRIK ASTRONOMICKÝ ÚSTAV SAV, T. LOMNICA BEZOVEC 2020 2. OKTÓBER BRIEF HISTORY OF COMET AND ASTEROID RESEARCH • 1943 – starting of comet discoveries and meteor research • 1946 – discovery of the first comet Pajdušáková-Rotbart-Weber • 1946-1959 – 70 new comets discovered over the world, 18 from Skalnate Pleso (Honda- Mrkos-Pajdušáková, Tuttle-Giacobini-Kresák, 1957 V Mrkos,...) • 1964 – asteroid observations and astrometry CURRENT RESEARCH AT THE INTERPLANETARY MATTER DEPARTMENT • Investigation of the activity, physical and dynamical evolution of selected cometary nuclei • Color photometry, lightcurves, and modelling of shapes of the asteroids • Study of transfer orbits, interrelations and evolution among different populations regarding near- Earth objects • Study of the structure of the outer part of the Oort cloud and the Edgeworth-Kuiper belt • Study of structure and dynamics of meteoroid streams, evolution of their parent bodies, the distribution of meteoroid particles in the inner Solar System, search for meteoroid streams of asteroidal origin, search for hyperbolic and interstellar meteoroids • Operation of the all-sky bolide cameras within the European Fireball Network • Study of meteorite properties • Study of the physical and chemical properties of asteroid/comet surfaces and their relevant terrestrial analogs, simulation of effects of space weathering in laboratory conditions • The IAU Meteor Data Center (MDC) operates at the AI SAS under the auspices of Division F (Planetary Systems and Bioastronomy) of the International Astronomical Union (IAU). The MDC is responsible for the designation of meteor showers, for the efficient collection, (computation,) checking and dissemination of trajectory observations and orbits of meteors. It acts as a central depository for meteor orbits obtained by photographic, video and radar techniques.
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The Minor Planet Bulletin 40 (2013) 207
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 40, NUMBER 4, A.D. 2013 OCTOBER-DECEMBER 187. LIGHTCURVE ANALYSIS OF EXTREMELY CLOSE Canopus package (Bdw Publishing). NEAR-EARTH ASTEROID – 2012 DA14 Asteroid 2012 DA14 is a near-Earth object (Aten category, q = Leonid Elenin 0.8289, a = 0.9103, e = 0.0894, i = 11.6081). Before the current Keldysh Institute of Applied Mathematics RAS close approach, 2012 DA14 had orbital elements within the Apollo ISON-NM Observatory (MPC H15), ISON category (q = 0.8894, a = 1.0018, e = 0.1081, i = 10.3372). 140007, Lyubertsy, Moscow region, 8th March str., 47-17 Parameters of the orbit make this asteroid an interesting target for a [email protected] possible space mission. Asteroid 202 DA14 was discovered on Feb 23 2012 by the La Sagra Sky Survey, LSSS (MPC code J75). Igor Molotov Keldysh Institute of Applied Mathematics RAS An extremely close approach to the Earth (0.00022 AU or ~34 000 ISON km) occurred 2013 Feb 15.80903. We observed this asteroid after its close approach, 2013 Feb 16, from 02:11:35 UT to 12:17:43 UT (Received: 20 February*) (Table1). Our total observational interval was 10 h 16 min, i.e. ~108% of the rotation period. In this paper we present one of the first lightcurves of near-Earth asteroid 2012 DA14. This is a very interesting near-Earth asteroid, which approached the Earth at a very close distance on Feb. 15 2013. From our UT Δ r phase mag measurements we find a rotational period of 9.485 ± 02:11:35 0.0011 0.988 73.5 11.8 0.144 h with an amplitude of 1.79 mag.
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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).
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Six Years of Sustained Activity from Active Asteroid (6478) Gault Colin Orion Chandler,1 Jay Kueny,1 Annika Gustafsson,1 Chadwick A
Draft version May 3, 2019 Typeset using LATEX preprint2 style in AASTeX62 Six Years of Sustained Activity from Active Asteroid (6478) Gault Colin Orion Chandler,1 Jay Kueny,1 Annika Gustafsson,1 Chadwick A. Trujillo,1 Tyler D. Robinson,1 and David E. Trilling1 1Department of Physics & Astronomy, Northern Arizona University, PO Box 6010, Flagstaﬀ, AZ 86011, USA ABSTRACT We present archival observations demonstrating that main belt asteroid (6478) Gault has an extensive history of comet-like activity. Outbursts have taken place during multiple epochs since 2013 and at distances extending as far as 2.68 au, nearly aphelion. (6478) Gault is a member of the predominately S-type (i.e., volatile-poor) Phocaea family; no other main belt object of this type has ever shown more than a single activity outburst. Furthermore, our data suggest this is the longest duration of activity caused by a body spinning near the rotational breakup barrier. If activity is indeed unrelated to volatiles, as appears to be the case, (6478) Gault represents a new class of object, perpetually active due to rotational spin-up. Keywords: minor planets, asteroids: individual ((6478) Gault) | comets: individual ((6478) Gault) 1. INTRODUCTION Active asteroids like (6478) Gault (Figure1, this work) are dynamically asteroidal objects but they uncharacteristically manifest cometary features such as tails or comae (Hsieh & Je- witt 2006a). With only ∼20 known to date (see Table 1 of Chandler et al. 2018), active asteroids remain poorly understood, yet they promise insight into solar system volatile dis- position and, concomitantly, the origin of water on Earth (Hsieh & Jewitt 2006b).
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An Anisotropic Distribution of Spin Vectors in Asteroid Families⋆
A&A 559, A134 (2013) Astronomy DOI: 10.1051/0004-6361/201321993 & c ESO 2013 Astrophysics An anisotropic distribution of spin vectors in asteroid families J. Hanuš1,M.Brož1,J.Durechˇ 1,B.D.Warner2, J. Brinsfield3,R.Durkee4, D. Higgins5,R.A.Koff6,J.Oey7, F. Pilcher8, R. Stephens9,L.P.Strabla10,Q.Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, ACT 2913 Ngunnawal, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), 25020 Brescia, Italy Received 30 May 2013 / Accepted 16 September 2013 ABSTRACT Context. The current number of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study the spin-vector properties of not only the whole population of main-belt asteroids, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the hierarchical clustering method (HCM) as members of ten col- lisional families, among which are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
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