Scattering properties of irregularly shaped interstellar composite dust analogues consisting of graphite and fayalite (Fe₂SiO₄) were studied using discrete dipole approximation (DDA). Two dust models were developed to calculate the scattering and extinction efficiencies, single scattering albedo, asymmetry parameter, phase functions and degree of linear polarizations. Laboratory measurements were also performed at three incident wavelengths 543.5, 594.5 and 632.8 nm on chemically synthesized graphite and fayalite composite particles of sizes ranging from 0.3 to 5 μm. A comparative analysis of the theoretical and experimental results of shape- and size-averaged scattering parameters shows that changes in the percentage composition of a two-species mixture model has a pronounced effect on the light-scattering properties of dust particles. The developed computational models are successful in representing a two-species mixture of interstellar dust analogues considering diverse size, shapes and percentage composition. This technique can be applied to fit observed scattering and absorption peaks in the visible region produced by astrophysical dust, provided large number of particle species are included and the influence of more physical parameters (e.g., porosity, fluffiness, temperature, density, etc.) are considered. Further, this study is also applicable to remote sensing, atmospheric and planetary sciences. All the physical parameters employed as variables in the models influence the oscillations observed in theoretical curves and change the values of scattering parameters.

由石墨和铁橄榄石（Fe ₂ SiO _{4 ）}组成的不规则形状星际复合尘埃类似物的散射特性) 使用离散偶极近似 (DDA) 进行研究。开发了两种尘埃模型来计算散射和消光效率、单次散射反照率、不对称参数、相位函数和线性偏振度。还在三个入射波长 543.5、594.5 和 632.8 nm 下对尺寸范围为 0.3 至 5 μm 的化学合成石墨和铁橄榄石复合颗粒进行了实验室测量。对形状和尺寸平均散射参数的理论和实验结果的比较分析表明，两种物种混合模型的百分比组成变化对尘埃粒子的光散射特性有显着影响。考虑到不同的大小、形状和百分比组成，开发的计算模型成功地表示了星际尘埃类似物的两种混合物。如果包含大量粒子种类并且更多物理参数（例如孔隙率、蓬松度、温度、密度等）的影响，则该技术可用于拟合观测到的天体物理尘埃产生的可见光区域的散射和吸收峰。被考虑。此外，这项研究也适用于遥感、大气和行星科学。在模型中用作变量的所有物理参数都会影响理论曲线中观察到的振荡并改变散射参数的值。该技术可用于拟合观测到的天体物理尘埃产生的可见光区域的散射和吸收峰，前提是包含大量粒子种类，并且更多物理参数（例如孔隙率、蓬松度、温度、密度等）的影响可以用于计算。被考虑。此外，这项研究也适用于遥感、大气和行星科学。在模型中用作变量的所有物理参数都会影响理论曲线中观察到的振荡并改变散射参数的值。该技术可用于拟合观测到的天体物理尘埃产生的可见光区域的散射和吸收峰，前提是包含大量粒子种类，并且更多物理参数（例如孔隙率、蓬松度、温度、密度等）的影响可以用于计算。被考虑。此外，这项研究也适用于遥感、大气和行星科学。在模型中用作变量的所有物理参数都会影响理论曲线中观察到的振荡并改变散射参数的值。这项研究也适用于遥感、大气和行星科学。在模型中用作变量的所有物理参数都会影响理论曲线中观察到的振荡并改变散射参数的值。这项研究也适用于遥感、大气和行星科学。在模型中用作变量的所有物理参数都会影响理论曲线中观察到的振荡并改变散射参数的值。