外太阳系中的对冲效应：相函数形貌的比较研究
The opposition effect in the outer Solar System: a comparative study of the phase function morphology
摘要：
本文描述了太阳系巨行星卫星和行星环的盘积分相函数的形态。我们发现相函数的形状可以用对数模型精确地表示（Bobrov，1970，在Surfaces and Interiors of Planets and Satellite，Academic，edited by A. Dollfus）。出于实际目的，我们还通过线性指数模型来参数化相位曲线（Kaasalainen等人，2001，Journal of Quantitative Spectroscopy and辐射转移，70，529-543）和简单的逐部分线性模型（Lumme和Irvine，1976，Astronomical Journal，81，865-893），其提供了三个形态参数：反向浪涌的幅度A和半峰半宽（HWHM），以及相位函数的线性部分在较大相位角处的斜率S。我们的分析表明，所有这些形态参数与表面的单次散射曲率相关。通过更精确地考虑太阳的有限角尺寸，我们发现伽利略、土星、天王星和海王星卫星具有相似的半高宽（0.5度），而它们具有宽范围的振幅A。月球具有最大的HWHM（2度）。我们认为这是太阳大小偏差的结果，因为太阳的大小有限，从地球到海王星变化很大。通过应用一种新的方法，试图形态反卷积的相位函数的太阳角的大小，我们发现，冰冷的和年轻的表面，与积极的表面重塑，具有最小的值的A和HWHM，而黑暗的对象（也许是旧的表面），如月球，海卫二和土星C环有最大的A和HWHM。
英文摘要：
In this paper, we characterize the morphology of the disk-integrated phase functions of satellites and rings around the giant planets of our Solar System. We find that the shape of the phase function is accurately represented by a logarithmic model (Bobrov, 1970, in Surfaces and Interiors of Planets and Satellites, Academic, edited by A. Dollfus). For practical purposes, we also parametrize the phase curves by a linear-exponential model (Kaasalainen et al., 2001, Journal of Quantitative Spectroscopy and Radiative Transfer, 70, 529-543) and a simple linear-by-parts model (Lumme and Irvine, 1976, Astronomical Journal, 81, 865-893), which provides three morphological parameters : the amplitude A and the Half-Width at Half-Maximum (HWHM) of the opposition surge, and the slope S of the linear part of the phase function at larger phase angles. Our analysis demonstrates that all of these morphological parameters are correlated with the single scattering albedos of the surfaces. By taking more accurately into consideration the finite angular size of the Sun, we find that the Galilean, Saturnian, Uranian and Neptunian satellites have similar HWHMs (0.5 degrees), whereas they have a wide range of amplitudes A. The Moon has the largest HWHM (2 degrees). We interpret that as a consequence of the solar size bias, via the finite size of the Sun which varies dramatically from the Earth to Neptune. By applying a new method that attempts to morphologically deconvolve the phase function to the solar angular size, we find that icy and young surfaces, with active resurfacing, have the smallest values of A and HWHM, whereas dark objects (and perhaps older surfaces) such as the Moon, Nereid and Saturn C ring have the largest A and HWHM.
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