盘状星系中的尘埃空间分布及尘埃减光过程

星系中的尘埃减光是一个复杂过程，除了与尘埃含量及其物理化学特征有关外，还与尘埃和辐射源的几何分布密切相关。本项目拟基于Sloan数字巡天中的低红移盘星系样本，结合多方面的观测数据，分析和比较不同尘埃减光特征参数的测量结果。我们将以不同倾角盘状星系的减光特征的差异为出发点，重点讨论盘状星系中不同成分的辐射源和尘埃的几何分布。我们将在尘埃和辐射源的几何分布模型基础上进一步构建盘星系的尘埃辐射转移模型，并利用该模型来探讨盘星系中尘埃减光曲线形状的变化及其背后的物理机制。本项目的研究将不仅能有助于获得更准确的星系尘埃减光特征，也将更有利于星系中其它基本物理参数的准确测量（如恒星质量，恒星形成率等）。更为重要的是，本项目的研究将能有助于更好的认识盘状星系中星族和尘埃成分的结构特征，从而加深对它们的形成和演化过程的理解。

The dust attenuation of galaxies is a complex process, which not only depends on the amount and physical properties of dust particles but is also closely related to the geometry of the radiation sources and dust components. This proposal aims to compare the different dust attenuation parameters of the disk galaxies in the Sloan Digital Sky Survey by taking advantages of their multifaceted data set. We will focus on the geometric distribution of the radiation sources and the dust components by studying the systematical variation of the dust attenuation of the disk galaxies with different inclinations. With the geometry models of dust and radiation components, we aims to build a general dust radiation transfer model of the disc galaxies. With this radiation transfer model, we further explore the variation of the shape of the dust attenuation curves in disc galaxies with different physical(geometric) properties. This study will not only help to obtain more accurate galactic dust attenuation features, but will also be very useful on accurate measurements of other basic parameters of disk galaxies(e.g., stellar mass, star formation rate, etc.). More importantly, this research will help us to better understand the structural features of the stellar populations and dust components of the disk galaxies, and thus deepen our understanding of their formation and evolution.