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The opposition effect in the outer Solar system: A comparative study of the phase function morphology

机译:太阳系外层的对立效应:相函数形态的比较研究

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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, M.S., 1970. Physical properties of Saturn's rings. In: Dollfus, A. (Ed.), Surfaces and Interiors of Planets and Satellites. Academic, New York, pp. 376-461]. For practical purposes, we also parametrize the phase curves by a linear-exponential model [Kaasalainen, S., Muinonen, K., Piironen, J., 2001. Comparative study on opposition effect of icy solar system objects. Journal of Quantitative Spectroscopy and Radiative Transfer 70, 529-543] and a simple linear-by-parts model [Lumme, K., Irvine, W.M., 1976. Photometry of Saturn's rings. 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 slopes of the linear part of the phase function at larger phase angles.rnOur analysis demonstrates that all of these morphological parameters are correlated with the single-scattering albedos of the surfaces.rnBy 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°), whereas they have a wide range of amplitudes A. The Moon has the largest HWHM (~2°). We interpret that as a consequence of the "solar size bias", via the finite angular 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's C ring have the largest A and HWHM.rnComparison between multiple objects also shows that solar system objects belonging to the same planet have comparable opposition surges. This can be interpreted as a "planetary environmental effect" that acts to locally modify the regolith and the surface properties of objects which are in the same environment.
机译:在本文中,我们描述了太阳系巨大行星周围的卫星和环的圆盘积分相位函数的形态。我们发现,相位函数的形状可以用对数模型准确地表示出来[Bobrov,M.S.,1970.土星环的物理特性。在:Dollfus,A.(编辑),《行星和卫星的表面和内部》。纽约,学院,第376-461页]。出于实际目的,我们还通过线性指数模型对相位曲线进行参数化设置[Kaasalainen,S.,Muinonen,K.,Piironen,J.,2001。对冰冷太阳系物体的对立作用的比较研究。定量光谱与辐射传递杂志70,529-543]和简单的线性零件模型[Lumme,K.,Irvine,W.M.,1976。土星环的光度法。天文学报81,865-893],提供了三个形态学参数:对角波动的振幅A和半峰半宽(HWHM),以及在较大的相角下相位函数的线性部分的斜率我们的分析表明,所有这些形态参数都与表面的单散射反照率有关。通过更准确地考虑太阳的有限角度大小,我们发现伽利略,土星,天王星和海王星卫星具有相似的特征HWHM(<0.5°),但是它们的振幅A范围很宽。月亮具有最大的HWHM(〜2°)。我们认为这是“太阳大小偏差”的结果,是由于太阳的有限角度大小从地球到海王星的变化都很大。通过尝试将相位函数从形态上解卷积到太阳角大小的新方法,我们发现具有活跃表面重整的冰冷年轻表面具有最小的A和HWHM值,而深色物体(可能是较旧的表面)具有由于月球,尼雷德和土星的C环具有最大的A和HWHM.rn,多个天体之间的比较也表明,属于同一行星的太阳系天体具有可比的对角冲。这可以解释为一种“行星环境效应”,其作用是局部修改同一环境中物体的重凝灰岩和表面性质。

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