Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

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...

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Detalles Bibliográficos
Autores: Moreno, Fernando, Guirado, Daniel, 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, Zhong-Yi, 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, Vania, 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.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2018
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/212823
Acceso en línea:http://hdl.handle.net/10261/212823
Access Level:acceso abierto
Palabra clave:Methods: numerical
Minor planets,asteroids: individual (67P/Churyumov-Gerasimenko)
Descripción
Sumario: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.© 2018. The American Astronomical Society. All rights reserved..

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