近红外波长处金星(盘)线偏振度的敏感性分析  

Sensitivity analysis of Venus(disk) linear polarization at near-infrared wavelengths

作　　者：李宜奇 孙晓兵 郑小兵 黄红莲[2,3] 刘晓 提汝芳[2,3] 韦祎晨 王宇轩[2,3] LI Yiqi;SUN Xiaobing;ZHENG Xiaobing;HUANG Honglian;LIU Xiao;TI Rufang;WEI Yichen;WANG Yuxuan(School of Environmental Science and Optoelectronic Technology,University of Science and Technology of China,Hefei 230026,China;Anhui Institute of Optics and Fine Mechanics,Hefei Institutes of Physical Science,Chinese Academy of Sciences,Hefei 230031,China;Key Laboratory of Optical Calibration and Characterization,Chinese Academy of Sciences,Hefei 230031,China)

机构地区：[1]中国科学技术大学环境科学与光电技术学院,合肥230026 [2]中国科学院合肥物质科学研究院安徽光学精密机械研究所,合肥230031 [3]中国科学院通用光学定标与表征技术重点实验室,合肥230031

出　　处：《物理学报》2025年第9期133-147,共15页Acta Physica Sinica

基　　金：航天科技创新应用研究项目(批准号:E23Y0H555S1);航空科技创新应用研究项目(批准号:62502510201)资助的课题。

摘　　要：通过对金星大气中云和霾进行详细的分层建模和辐射传输模拟,并结合金星快车SPICAV IR仪器的近红外观测数据,探讨了云和霾粒子的微物理性质及其对金星(盘)线偏振度的影响.结果表明,不同模式粒子的单次散射和线偏振特性在相位角和波长上呈现显著变化,上层霾和云粒子(Mode 1和Mode 2)的微物理性质对金星的线偏振度影响尤为显著.Mode 1粒子的柱密度减小或模态半径增大均会使线偏振峰值增大,而线偏振度对Mode 2粒子柱密度的变化与Mode 1趋势相反.复折射率实部的变化对偏振特性影响显著,而虚部影响较小.此外,线偏振度在金星盘上随波长、相位角及位置(中心与边缘)变化明显,盘积分的线偏振特性对粒子微物理性质和大气水平不均匀性(如云量分布)高度敏感,且光环现象清晰可见.多层模型的模拟结果与SPICAV IR中低纬数据拟合较好,这种详细分层建模为揭示金星大气中云和霾的微物理特性及其辐射传输特性提供了重要依据.The PyMieDAP radiative transfer model is used in this work to simulate the radiation characteristics of Venus clouds and haze,thereby investigating how their microphysical characteristics affect linear polarization by comparing near-infrared polarization data from the SPICAV IR instrument on the Venus Express.The results show that single-scattered fluxes of the four particle modes decrease in a phase angle range from 0°to 120°,but increase near 160°.Mode 1 particles(upper haze)exhibit Rayleigh scattering characteristics,with polarization changing from positive to negative as the wavelength increases.Mode 2 and Mode 2'particles display two positive polarization peaks near 15°and 160°,respectively,with polarization reversing in the near-infrared.Mode 3 particles show oscillations in polarization near 105°,flipping from positive to negative between 155°and 165°.The primary polarization peak occurs near 15°,corresponding to the main rainbow,while a secondary peak between 150°and 160°is attributed to anomalous diffraction.The microphysical properties of upper clouds and haze(Mode 1 and Mode 2)significantly affect the linear polarization of Venus,while those of lower clouds(Mode 2'and Mode 3)have a minimum influence.A reduction in Mode 1 column density increases the polarization peak at the main rainbow,while an increase in Mode 2 column density has the opposite effect.Changes in modal radius enhance polarization peaks for Mode 1 and Mode 2,while increasing geometric standard deviation reduces polarization peaks and shifts their phase angles.The real part of the complex refractive index has a greater influence on polarization than the imaginary part.Simulations using the multilayer model show better agreement with SPICAV IR data and consistency with the larger particle sizes in Venus’haze.The integrated linear polarization across the Venus disk varies with wavelength and phase angle,with the polarization being higher at the disk's edge.The variation in cloud coverage also influences polarization,with areas

关 键 词：金星云和霾 线偏振 敏感性分析 微物理特性 

分 类 号：P184[天文地球—天文学]