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The pebbles/boulders size distributions on Sais: Rosetta’s final landing site on comet 67P/Churyumov–Gerasimenko

Maurizio Pajola 1 Alice Lucchetti 2 Marco Fulle 3 Stefano Mottola 4 Maximilian Hamm 4 Vania da Deppo 5 Luca Penasa 6, 7 Gabor Kovacs 8 Matteo Massironi 7 Xian Shi 8 Cécilia Tubiana 8 Carsten Güttler 8 Nilda Oklay 4 Jean-Baptiste Vincent 4 Imre Toth 9, 10 Björn Davidsson 11 Giampiero Naletto 12, 6, 5 Holger Sierks 8 Cesare Barbieri 6, 13 Philippe L. Lamy 9 Rafael Rodrigo 14, 15 Detlef Koschny 16 Hans Rickman 17, 18 Horst Uwe Keller 5, 19 Jessica Agarwal 8 Michael F. A'Hearn 20 Maria Antonella Barucci 21 Jean-Loup Bertaux 22 Ivano Bertini 6 Gabriele Cremonese 2 Stefano Debei 23 Mariolino de Cecco 24 Jakob Deller 8 Mohamed Ramy El Maarry 25, 26 Sonia Fornasier 21 Elisa Frattin 2, 13 Adeline Gicquel 8, 11 Olivier Groussin 9 Pedro J. Gutiérrez 27 Sebastien Höfner 8 Marc Hofmann 8 Stubbe F. Hviid 4 Wing-Huen Ip 28, 29 Laurent Jorda 9 Jörg Knollenberg 4 Jörg-Rainer Kramm 8 Ekkehard Kührt 4 Michael Küppers 30 Luisa M. Lara 31 Monica Lazzarin 13 José J. Lopez Moreno 27 Francesco Marzari 13 Harald Michalik 32 Frank Preusker 4 Frank Scholten 4 Nicolas Thomas 33, 26 
LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales
Abstract : By using the imagery acquired by the Optical, Spectroscopic, and Infrared Remote Imaging System Wide-Angle Camera (OSIRIS WAC), we prepare a high-resolution morphological map of the Rosetta Sais final landing site, characterized by an outcropping consolidated terrain unit, a coarse boulder deposit and a fine particle deposit. Thanks to the 0.014 m resolution images, we derive the pebbles/boulders size-frequency distribution (SFD) of the area in the size range of 0.07–0.70 m. Sais’ SFD is best fitted with a two-segment differential power law: the first segment is in the range 0.07–0.26 m, with an index of −1.7 ± 0.1, while the second is in the range 0.26–0.50 m, with an index of −4.2 +0.4/−0.8. The ‘knee’ of the SFD, located at 0.26 m, is evident both in the coarse and fine deposits. When compared to the Agilkia Rosetta Lander Imaging System images, Sais surface is almost entirely free of the ubiquitous, cm-sized debris blanket observed by Philae. None the less, a similar SFD behaviour of Agilkia, with a steeper distribution above ∼0.3 m, and a flatter trend below that, is observed. The activity evolution of 67P along its orbit provides a coherent scenario of how these deposits were formed. Indeed, different lift pressure values occurring on the two locations and at different heliocentric distances explain the presence of the cm-sized debris blanket on Agilkia observed at 3.0 au inbound. Contrarily, Sais activity after 2.1 au outbound has almost completely eroded the fine deposits fallen during perihelion, resulting in an almost dust-free surface observed at 3.8 au.
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Maurizio Pajola, Alice Lucchetti, Marco Fulle, Stefano Mottola, Maximilian Hamm, et al.. The pebbles/boulders size distributions on Sais: Rosetta’s final landing site on comet 67P/Churyumov–Gerasimenko. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2017, 471 (1), pp.680 - 689. ⟨10.1093/mnras/stx1620⟩. ⟨insu-01574968⟩



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