Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

Moreno, F.; Guirado, D.; Muñoz, O.; Bertini, I.; Tubiana, Cecilia; Güttler, Carsten; Fulle, M.; Rotundi, A.; Corte, V. Della; Ivanovski, S. L.; Rinaldi, G.; Bockelée-Morvan, D.; Zakharov, V. V.; Agarwal, Jessica; Mottola, S.; Toth, I.; Frattin, E.; Lara, L. M.; Gutiérrez, P. J.; Lin, Z. Y.; Kolokolova, L.; Sierks, Holger; Naletto, G.; Lamy, P. L.; Rodrigo, R.; Koschny, D.; Davidsson, B.; Barucci, M. A.; Bertaux, J.-L.; Bodewits, D.; Cremonese, G.; Deppo, V. Da; Debei, S.; Cecco, M. De; Deller, Jakob; Fornasier, S.; Ip, W.-H.; Keller, H. U.; Lazzarin, M.; López-Moreno, J. J.; Marzari, F.; Shi, Xian

doi:10.3847/1538-3881/aae526

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Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

MPS-Authors

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Tubiana, Cecilia
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons160269

Güttler, Carsten
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons123097

Agarwal, Jessica
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons104212

Sierks, Holger
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons140545

Deller, Jakob
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons192389

Shi, Xian
Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society;

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http://adsabs.harvard.edu/abs/2018AJ....156..237M
(Abstract)

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Citation

Moreno, F., Guirado, D., Muñoz, O., Bertini, I., Tubiana, C., Güttler, C., et al. (2018). Models of Rosetta/OSIRIS 67P Dust Coma Phase Function. The Astronomical Journal, 156(5): 237. doi:10.3847/1538-3881/aae526.

Cite as: https://hdl.handle.net/21.11116/0000-0002-9404-2

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 ≳ 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.