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Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

AuthorsMoreno, Fernando ; Guirado, D.; Muñoz, Olga ; Tubiana, C.; Güttler, C.; Fulle, M.; Rotundi, A.; Della Corte, V.; Ivanovski, S.L.; Rinaldi, G.; Bockelée-Morvan, D.; Zakharov, V.V.; Agarwal, J.; Mottola, S.; Toth, I.; Frattin, E.; Lara, Luisa María ; Gutiérrez, Pedro J. ; Lin, Z.Y.; Kolokolova, L.; Sierks, H.; Naletto, G.; Lamy, P.L.; Rodrigo Montero, Rafael ; Koschny, D.; Davidsson, B.; Barucci, M.A.; Bertaux, J.L.; Bodewits, D.; Cremonese, G.; Da Deppo, V.; Debei, S.; De Cecco, M.; Deller, J.; Fornasier, S.; Ip, W.H.; Keller, H.U.; Lazzarin, M.; López-Moreno, José Juan ; Marzari, F.; Shi, X.; Bertini, I.
KeywordsMethods: numerical
Minor planets,asteroids: individual (67P/Churyumov-Gerasimenko)
Issue Date2018
PublisherIOP Publishing
CitationAstronomical Journal 156(5): 237 (2018)
AbstractThe 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 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.© 2018. The American Astronomical Society. All rights reserved..
Publisher version (URL)http://dx.doi.org/10.3847/1538-3881/aae526
Identifiersdoi: 10.3847/1538-3881/aae526
issn: 0004-6256
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(IAA) Artículos
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