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Shape and spin determination of Barbarian asteroids

AutorDevogèle, M.; Tanga, P.; Bendjoya, P.; Rivet, J.P.; Surdej, J.; Hanuš, J.; Abe, L.; Antonini, P.; Artola, R.A.; Audejean, M.; Behrend, R.; Berski, F.; Bosch, J.G.; Bronikowska, M.; Carbognani, A.; Char, F.; Kim, M.J.; Choi, Y.J.; Colazo, C.A.; Coloma, J.; Coward, D.; Durkee, R.; Erece, O.; Forne, E.; Hickson, P.; Hirsch, R.; Horbowicz, J.; Kami¿ski, K.; Kankiewicz, P.; Kaplan, M.; Kwiatkowski, T.; Konstanciak, I.; Kruszewki, A.; Kudak, V.; Manzini, F.; Moon, H.K.; Marciniak, A.; Murawiecka, M.; Nadolny, J.; Og¿oza, W.; Ortiz, José Luis ; Oszkiewicz, D.; Pallares, H.; Peixinho, N.; Poncy, R.; Reyes, F.; De Los Reyes, J.A.; Santana-Ros, T.; Sobkowiak, K.; Pastor, S.
Palabras claveTechniques: photometric
Methods: observational
Minor planets, asteroids: general
Fecha de publicación2017
EditorEDP Sciences
CitaciónAstronomy and Astrophysics 607: A119 (2017)
ResumenContext. The so-called Barbarian asteroids share peculiar, but common polarimetric properties, probably related to both their shape and composition. They are named after (234) Barbara, the first on which such properties were identified. As has been suggested, large scale topographic features could play a role in the polarimetric response, if the shapes of Barbarians are particularly irregular and present a variety of scattering/incidence angles. This idea is supported by the shape of (234) Barbara, that appears to be deeply excavated by wide concave areas revealed by photometry and stellar occultations. Aims. With these motivations, we started an observation campaign to characterise the shape and rotation properties of Small Main-Belt Asteroid Spectroscopic Survey (SMASS) type L and Ld asteroids. As many of them show long rotation periods, we activated a worldwide network of observers to obtain a dense temporal coverage. Methods. We used light-curve inversion technique in order to determine the sidereal rotation periods of 15 asteroids and the convergence to a stable shape and pole coordinates for 8 of them. By using available data from occultations, we are able to scale some shapes to an absolute size. We also study the rotation periods of our sample looking for confirmation of the suspected abundance of asteroids with long rotation periods. Results. Our results show that the shape models of our sample do not seem to have peculiar properties with respect to asteroids with similar size, while an excess of slow rotators is most probably confirmed.© 2017 ESO.
URIhttp://hdl.handle.net/10261/167539
Identificadoresdoi: 10.1051/0004-6361/201630104
issn: 1432-0746
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