Rosetta/OSIRIS 对 67P 尘埃彗发的相函数建模
地球与行星天体物理
2018-11-07 v1
摘要
彗星 67P 尘埃彗发的相函数已由 Rosetta/OSIRIS 图像确定 \citep{Bertini17}。该函数在约 100 的相角附近呈现深极小值,并具有强烈的后向散射增强。这两个性质无法被常规的彗尘模型所复现,后者大多基于波长尺度且随机取向的聚集粒子。然而我们表明,一组取向一致的细长粒子,其长宽比多样、半径 10 m,且长轴垂直于太阳辐照方向,能够复现观测到的相函数。这些粒子必须是吸收性的,其折射率虚部约为 0.1 以匹配预期的几何反照率,且孔隙率在 60–70% 范围内。
引用
@article{arxiv.1809.10424,
title = {Models of Rosetta/OSIRIS 67P dust coma phase function},
author = {Fernando Moreno and Daniel Guirado and Olga Muñoz and Ivano Bertini and Cecilia Tubiana and Carsten Guttler and Marco Fulle and Alessandra Rotundi and Vincenzo Della Corte and Stavro Ivanovski and Giovanna Rinaldi and Dominique Bockelee-Morvan and Vladimir Zakharov and Jessica Agarwal and Stefano Mottola and Imre Toth and Elisa Frattin and Luisa Lara and Pedro Gutierrez and Zhong Yi Lin and Ludmilla Kolokolova and Holger Sierks and Giampiero Naletto and Philippe Lamy and Rafael Rodrigo and Detlef Koschny and Bjorn Davidsson and Maria Antonietta Barucci and Jean-Lup Bertaux and Dennis Bodewits and Gabriele Cremonese and Vania Da Deppo and Stefano Debei and Mariolino de Cecco and Jakob Deller and Sonia Fornasier and Wing Ip and Uwe Keller and Monica Lazzarin and Jose Juan Lopez-Moreno and Francesco Marzari and Xian Shi},
journal= {arXiv preprint arXiv:1809.10424},
year = {2018}
}
备注
Accepted by Astronomical Journal, September 26th, 2018. 21 pages, 5 figures