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4 results on '"Goat Mountain Astronomical Research Station"'

1. Physical models of ten asteroids from an observers' collaboration network

Author

R. Dymock, F. Manzini, S. Boroumand, Stephen M. Slivan, Robert D. Stephens, R. A. Koff, Greg Bolt, M. Fagas, R. Roy, Michael Fauerbach, Brian D. Warner, Josef Ďurech, Margaret Pan, A. Marciniak, M. Crow, Angel F. Lopez, Mikko Kaasalainen, Merideth Frey, Frederick Pilcher, Rita Pacheco, Thomas Bennett, S. Fauvaud, L. Crespo da Silva, C. Bembrick, W. Pych, Donald P. Pray, R. Crippa, Raoul Behrend, R. Poncy, S. Sposetti, Jérôme Berthier, T. Kwiatkowski, Marek Wolf, G. Santacana, R. Durkee, D. Jardine, Krzysztof Kamiński, Tadeusz Michalowski, W. H. Allen, Rui Soles Gonçalves, L. Bernasconi, R. Hirsch, Astronomical Institute, Charles University, Department of Mathematics and Statistics, Rolf Nevanlinna Institute, University of Helsinki, Astronomical Observatory, Adam Mickiewicz University, Vintage Lane Observatory, Observatoire Astronomique de l'Université de Genève, Mount Tarana Observatory, Florida Gulf Coast University, Observatoire des Engarouines, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Stazzione Astronomica di Sozzago, The WW Crow Observatory, Shed of Science Observatory, Association AstroQueyras, Groupe européen d’observation stellaire (GEOS), Department of Astronomy, Whitin Observatory, Wellesley College, Observatório Astronómico de Linhaceira, Illinois College, Antelope Hills Observatory, 980 Antelope Drive West, Bennett, Observatori Astronomic de Consell, Carbuncle Hill Observatory, Centrum Astronomiczne im. M. Kopernika, Warszawa (CAMK), Observatoire de Blauvac, Observatorio di Gnosca, Goat Mountain Astronomical Research Station, and Palmer Divide Observatory, Colorado Springs

Subjects
Physics, Physical model, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Inversion (meteorology), Astrophysics, 01 natural sciences, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Asteroid, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; Aims:We present physical models of ten asteroids obtained by means of lightcurve inversion. A substantial part of the photometric data was observed by amateur astronomers. We emphasize the importance of a coordinated network of observers that will be of extreme importance for future all-sky asteroid photometric surveys. Methods: The lightcurve inversion method was used to derive spin states and shape models of the asteroids. Results: We derived spin states and shape model for ten new asteroids: (110) Lydia, (125) Liberatrix, (130) Elektra, (165) Loreley, (196) Philomela, (218) Bianca, (306) Unitas, (423) Diotima, (776) Berbericia, and (944) Hidalgo. This increases the number of asteroid models up to nearly one hundred.

Published
2007

2. Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author

J. Hanuš, J. Ďurech, M. Brož, A. Marciniak, B. D. Warner, F. Pilcher, R. Stephens, R. Behrend, B. Carry, D. Čapek, P. Antonini, M. Audejean, K. Augustesen, E. Barbotin, P. Baudouin, A. Bayol, L. Bernasconi, W. Borczyk, J.-G. Bosch, E. Brochard, L. Brunetto, S. Casulli, A. Cazenave, S. Charbonnel, B. Christophe, F. Colas, J. Coloma, M. Conjat, W. Cooney, H. Correira, V. Cotrez, A. Coupier, R. Crippa, M. Cristofanelli, Ch. Dalmas, C. Danavaro, C. Demeautis, T. Droege, R. Durkee, N. Esseiva, M. Esteban, M. Fagas, G. Farroni, M. Fauvaud, S. Fauvaud, F. Del Freo, L. Garcia, S. Geier, C. Godon, K. Grangeon, H. Hamanowa, N. Heck, S. Hellmich, D. Higgins, R. Hirsch, M. Husarik, T. Itkonen, O. Jade, K. Kamiński, P. Kankiewicz, A. Klotz, R. A. Koff, A. Kryszczyńska, T. Kwiatkowski, A. Laffont, A. Leroy, J. Lecacheux, Y. Leonie, C. Leyrat, F. Manzini, A. Martin, G. Masi, D. Matter, J. Michałowski, M. J. Michałowski, T. Michałowski, J. Michelet, R. Michelsen, E. Morelle, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, A. Oksanen, D. Oszkiewicz, P. Pääkkönen, M. Paiella, H. Pallares, J. Paulo, M. Pavic, B. Payet, M. Polińska, D. Polishook, R. Poncy, Y. Revaz, C. Rinner, M. Rocca, A. Roche, D. Romeuf, R. Roy, H. Saguin, P. A. Salom, S. Sanchez, G. Santacana, T. Santana-Ros, J.-P. Sareyan, K. Sobkowiak, S. Sposetti, D. Starkey, R. Stoss, J. Strajnic, J.-P. Teng, B. Trégon, A. Vagnozzi, F. P. Velichko, N. Waelchli, K. Wagrez, H. Wücher, Astronomical Institute of Charles University, Charles University [Prague] (CU), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Palmer Divide Observatory, Organ Mesa Observatory, Goat Mountain Astronomical Research Station, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Observatoire de Bédoin, Observatoire de Chinon, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Harfleur Observatory, Observatoire des Engarouines, Collonges Observatory, Chercheur indépendant, Observatoire N°139 d'Antibes, Osservatorio Colleverde di Guidonia, Observatoire de Saint-Sulpice N°947, DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatorio de San Gervasi, Observatoire de Cabris, Blackberry Observatory, Centre d'Astronomie de Saint-Michel l'Observatoire, Observatoire de Sainte-Hélène, Observatorio Astronómico de Tradate, 138 Village-Neuf, The Amateur Sky Survey (TASS), The Amateur Sky Survey, Shed of Science Observatory, Association AstroQueyras, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Observatoire du Bois de Bardon, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Hamanowa Astronomical Observatory, DLR Institute of Planetary Research, German Aerospace Center (DLR), Hunters Hill Observatory, Skalnaté Pleso Observatory, A83 Jakokoski Observatory, Institute of Physics [Kielce], Jan Kochanowski University, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Antelope Hills Observatory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stazione Astronomica di Sozzago, Forte Software, Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Nyrölä Observatory (NYTT), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Mt. Suhora Observatory, Pedagogical University, Astronomy Department, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), François-Xavier Bagnoud Observatory, Blauvac Obsevatory, Blauvac Observatory, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Observatoire astronomique des Makes, Laboratoire Kastler Brossel (LKB (Lhomond)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), University of Geneva [Switzerland], European Space Agency (ESA), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki-University of Helsinki, Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, photometry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Inverse transform sampling, Astrophysics, 01 natural sciences, Photometry (optics), models, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Physical model, Minor planets, Astronomy and Astrophysics, Asteroids: general, 13. Climate action, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6., Accepted for publication in A&A, January 15, 2013

Published
2013

3. Analysis of the rotation period of asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger - search for the YORP effect

Author

Franck Marchis, Brian D. Warner, V. Fuller, Yu. N. Krugly, David Polishook, Igor Molotov, Petr Pravec, Josef Ďurech, Matti Viikinkoski, O. A. Burkhonov, R. Ya. Inasaridze, B. Macomber, Walter R. Cooney, Sławomir Breiter, Robert D. Stephens, N. M. Gaftonyuk, David Vokrouhlický, Z. Vanderplate, Joe Pollock, Gy. M. Szabó, Julian Oey, Dirk Terrell, Frédéric Vachier, E. Litvinenko, I. Slyusarev, Vasilij G. Shevchenko, Krisztián Sárneczky, O. I. Kvaratshelia, John Gross, Mikko Kaasalainen, A. Baransky, Astronomical Institute of Charles University, Charles University [Prague], Astronomical Observatory, Taras Shevchenko National University of Kyiv, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań ( UAM ), Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Sonoita Research Observatory, Department of Physics and Astronomy, Appalachian State University, Crimean Astrophysical Observatory ( CrAO ), Abastumani Astrophysical Observatory, Ilia State University [ Tbilisi], Department of Mathematics [Tampere], Tampere University of Technology [Tampere] ( TUT ), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University ( KhNU ), The Central Pulkovo Astronomical Observatory, Russian Academy of Sciences [Moscow] ( RAS ), Astronomy Department [Berkeley], University of California [Berkeley], Carl Sagan Center, SETI Institute, Keldysh Institute of Applied Mathematics, Kingsgrove Observatory, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] ( EAPS ), Massachusetts Institute of Technology ( MIT ), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] ( ASCR ), Konkoly Observatory, Hungarian Academy of Sciences [Budapest], Goat Mountain Astronomical Research Station, Department of Experimental Physics, University of Szeged [Szeged], ELTE Gao-Lendulet Research Group, Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Palmer Divide Observatory, Charles University [Prague] (CU), Astronomical Observatory of Kiev, Adam Mickiewicz University in Poznań (UAM), Uzbekistan Academy of Sciences, Department of Physics and Astronomy [Boone], University of North Carolina System (UNC)-University of North Carolina System (UNC), Crimean Astrophysical Observatory (CrAO), Ilia State University [Tbilisi], Tampere University of Technology [Tampere] (TUT), V.N. Karazin Kharkiv National University (KhNU), Russian Academy of Sciences [Moscow] (RAS), Department of Astronomy [Berkeley], University of California-University of California, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Czech Academy of Sciences [Prague] (CAS), Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), ELTE Gothard Astrophysical Observatory, Eötvös Loránd University (ELTE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Rotation period, Physics, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astronomy and Astrophysics, Acceleration (differential geometry), Context (language use), Astrophysics, Rotation, Light curve, 01 natural sciences, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Photometry (optics), [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Space and Planetary Science, Asteroid, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

The original publication is available at www.aanda.org. Copyright ESO.; International audience; The spin state of small asteroids can change on a long timescale by the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, the net torque that arises from anisotropically scattered sunlight and proper thermal radiation from an irregularly-shaped asteroid. The secular change in the rotation period caused by the YORP effect can be detected by analysis of asteroid photometric lightcurves. We analyzed photometric lightcurves of near-Earth asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger with the aim to detect possible deviations from the constant rotation caused by the YORP effect. We carried out new photometric observations of the three asteroids, combined the new lightcurves with archived data, and used the lightcurve inversion method to model the asteroid shape, pole direction, and rotation rate. The YORP effect was modeled as a linear change in the rotation rate in time d\omega /dt. Values of d\omega/ dt derived from observations were compared with the values predicted by theory. We derived physical models for all three asteroids. We had to model Eger as a nonconvex body because the convex model failed to fit the lightcurves observed at high phase angles. We probably detected the acceleration of the rotation rate of Eger d\omega / dt = (1.4 +/- 0.6) x 10^{-8} rad/d (3\sigma error), which corresponds to a decrease in the rotation period by 4.2 ms/yr. The photometry of Cerberus and Ra-Shalom was consistent with a constant-period model, and no secular change in the spin rate was detected. We could only constrain maximum values of |d\omega / dt| < 8 x 10^{-9} rad/d for Cerberus, and |d\omega / dt| < 3 x 10^{-8} rad/d for Ra-Shalom.

Published
2012

4. Spin rate distribution of small asteroids

Author

Robert D. Stephens, Štefan Gajdoš, Adrian Galad, François Colas, Petr Pravec, Rui Soles Gonçalves, J. Lecacheux, John Gross, Walter R. Cooney, David Vokrouhlický, Alan W. Harris, N. Gaftonyuk, R. A. Koff, Gianluca Masi, Yu. N. Krugly, Peter Kusnirak, Leonard Kornoš, David Higgins, Vasilij G. Chiorny, Dirk Terrell, R. Durkee, Donald P. Pray, Vasilij G. Shevchenko, Kamil Hornoch, J. G. Ries, Julian Oey, R. R. Dyvig, Vishnu Reddy, Marek Husárik, Jozef Vilagi, Brian D. Warner, Astronomical Institute, Academy of Sciences, Space Science Institute, La Canada, Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, Palmer Divide Observatory, Colorado Springs, Carbuncle Hill Observatory, Hunters Hill Observatory, Leura Observatory, Modra Observatory, Department of Astronomy, Physics of the Earth and Meteorology, Astronomical Institute, Slovak Academy of Sciences, Institute of Astronomy, Kharkiv National University, Crimean Astrophysical Observatory (CrAO), Sonoita Research Observatory, 77 Paint Trail, Sonoita, Goat Mountain Astronomical Research Station, Riverside Astronomical Society, Badlands Observatory, Department of Earth System Science and Policy, University of North Dakota, Grand Forks, Astronomy Department, McDonald Observatory, University of Texas, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Shed of Science Observatory, Bellatrix Astronomical Observatory, Antelope Hills Observatory, 980 Antelope Drive West, Bennett, and Observatório Astronómico de Linhaceira

Subjects
Physics, Solar System, education.field_of_study, Near-Earth object, Population, Astronomy, Astronomy and Astrophysics, Photometry (optics), Space and Planetary Science, Asteroid, Magnitude (astronomy), education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Residence time (statistics), Spin-½
Abstract

The spin rate distribution of main belt/Mars crossing (MB/MC) asteroids with diameters 3–15 km is uniform in the range from f = 1 to 9.5 d−1, and there is an excess of slow rotators with f 1 d−1. The observed distribution appears to be controlled by the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. The magnitude of the excess of slow rotators is related to the residence time of slowed down asteroids in the excess and the rate of spin rate change outside the excess. We estimated a median YORP spin rate change of ≈ 0.022 d −1 / Myr for asteroids in our sample (i.e., a median time in which the spin rate changes by 1 d−1 is ≈ 45 Myr ), thus the residence time of slowed down asteroids in the excess is ≈ 110 Myr . The spin rate distribution of near-Earth asteroids (NEAs) with sizes in the range 0.2–3 km (∼5 times smaller in median diameter than the MB/MC asteroids sample) shows a similar excess of slow rotators, but there is also a concentration of NEAs at fast spin rates with f = 9 – 10 d −1 . The concentration at fast spin rates is correlated with a narrower distribution of spin rates of primaries of binary systems among NEAs; the difference may be due to the apparently more evolved population of binaries among MB/MC asteroids.

Published
2008

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