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Models of Rosetta/OSIRIS 67P dust coma phase function

Fernando Moreno 1 Daniel Guirado 1 Olga Muñoz 1 Ivano Bertini 2 Cécilia Tubiana 3 Carsten Güttler 3 Marco Fulle 4 Alessandra Rotundi 5, 6 Vincenzo Della Corte 5, 6 Stavro Ivanovski 5 Giovanna Rinaldi 5 Dominique Bockelée-Morvan 7 Vladimir Zakharov 8, 5 Jessica Agarwal 3 Stefano Mottola 9 Imre Toth 10 Elisa Frattin 2 Luisa Maria Lara 1 Pedro J. Gutiérrez 1 Zhong Yi Lin 11 Ludmilla Kolokolova 12 Holger Sierks 3 Giampiero Naletto 13, 14, 2 Philippe L. Lamy 15 Rafael Rodrigo 16, 17 Detlief Koschny 18 Björn Davidsson 19 Maria Antonietta Barucci 7 Jean-Loup Bertaux 15 Dennis Bodewits 12 Gabriele Cremonese 20 Vania da Deppo 21 Stefano Debei 22 Mariolino de Cecco 23 Jakob Deller 3 Sonia Fornasier 7 Wing-H. Ip 24, 25 Horst Uwe Keller 9, 26 Monica Lazzarin 2 José Juan Moreno 1 Francesco Marzari 2 Xian Shi 3
Abstract : The phase function of the dust coma of comet 67P has been determined from Rosetta/OSIRIS images. This function shows a deep minimum at phase angles near 100°, and a strong backscattering enhancement. These two properties cannot be reproduced by regular models of cometary dust, most of them based on wavelength-sized and randomly oriented aggregate particles. We show, however, that an ensemble of oriented elongated particles of a wide variety of aspect ratios, with radii r gsim 10 μm, and whose long axes are perpendicular to the direction of the solar radiation, are capable of reproducing the observed phase function. These particles must be absorbing, with an imaginary part of the refractive index of about 0.1 to match the expected geometric albedo, and with porosity in the 60%–70% range.
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Fernando Moreno, Daniel Guirado, Olga Muñoz, Ivano Bertini, Cécilia Tubiana, et al.. Models of Rosetta/OSIRIS 67P dust coma phase function. The Astronomical Journal, American Astronomical Society, 2018, 156 (5), 237. ⟨10.3847/1538-3881/aae526⟩. ⟨hal-01962604⟩



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