Size-Frequency Distribution of Boulders ≥7 M on Comet 67P/Churyumov
A&A 583, A37 (2015) Astronomy DOI: 10.1051/0004-6361/201525975 & c ESO 2015 Astrophysics Rosetta mission results pre-perihelion Special feature Size-frequency distribution of boulders ≥7moncomet 67P/Churyumov-Gerasimenko Maurizio Pajola1, Jean-Baptiste Vincent2, Carsten Güttler2, Jui-Chi Lee3, Ivano Bertini1, Matteo Massironi4, Emanuele Simioni5, Francesco Marzari6, Lorenza Giacomini4, Alice Lucchetti1, Cesare Barbieri1,6, Gabriele Cremonese7, Giampiero Naletto8, Antoine Pommerol9, Mohamed R. El-Maarry9, Sébastien Besse10, Michael Küppers11, Fiorangela La Forgia6, Monica Lazzarin6, Nicholas Thomas9, Anne-Thérèse Auger12, Holger Sierks2, Philippe Lamy12, Rafael Rodrigo13,14, Detlef Koschny11, Hans Rickman15,16, Horst U. Keller17, Jessica Agarwal2, Michael F. A’Hearn18, Maria A. Barucci19,20, Jean-Loup Bertaux21, Vania Da Deppo5, Björn Davidsson15, Mariolino De Cecco22, Stefano Debei23, Francesca Ferri1, Sonia Fornasier19,20, Marco Fulle24, Olivier Groussin12, Pedro J. Gutierrez25, Stubbe F. Hviid26, Wing-Huen Ip3, Laurent Jorda12, Jörg Knollenberg26, J.-Rainer Kramm2, Ekkehard Kürt26,LuisaM.Lara25, Zhong-Yi Lin3, Jose J. Lopez Moreno25, Sara Magrin6, Simone Marchi27, Harald Michalik28, Richard Moissl10, Stefano Mottola26, Nilda Oklay2, Frank Preusker26, Frank Scholten26, and Cecilia Tubiana2 (Affiliations can be found after the references) Received 26 February 2015 / Accepted 8 June 2015 ABSTRACT Aims. We derive for the first time the size-frequency distribution of boulders on a comet, 67P/Churyumov-Gerasimenko (67P), computed from the images taken by the Rosetta/OSIRIS imaging system. We highlight the possible physical processes that lead to these boulder size distributions. Methods. We used images acquired by the OSIRIS Narrow Angle Camera, NAC, on 5 and 6 August 2014. The scale of these images (2.44−2.03 m/px) is such that boulders ≥7 m can be identified and manually extracted from the datasets with the software ArcGIS.
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