大部分的近地小天体是起源于主带小行星的近地小行星。近地小行星与人类有着密切的关系,地球在其形成的后期曾遭受了近地小行星的剧烈撞击。现在还有撞击事件不断发生，例如车里雅宾斯克火流星事件；未来，地球仍面临着被近地小行星撞击的危险。本项目就是通过测光监测一批近地小行星，尤其是那些对地球具有潜在威胁的目标；建立一个适合于近地小行星测光数据的分析的方法--Lommel-Seeliger椭球方法；反演分析监测目标近地小行星的基本物理参数--自转参数、形状和表面散射参数。依据Chandrasekhar的流体自转平衡理论以及测光反演得到近地小行星的形状和自转速率，开展近地小行星密度的估算。近地小行星的密度/质量是近地小行星撞碰危险评估准标--托里诺数（Torino Scale）所必需的除了轨道参数以外的重要物理参量。另外，近地小行星的空间姿态、形状以及密度也是未来我国深空探测近地小行星时所需要的数据。

The near earth objects(NEOs) are mostly composed of near earth asteroids(NEAs) which came from main belt asteroids. The NEAs have close relations with the Earth and human being. At the later stage of the formation of the Earth, it experienced violent bombardments of small objects. Nowadays, hitting events by NEOs often happen, for example, Chelyabinsk airburst in 2013. We have to face the collision risk by some NEOs in future. . One aim of this project is to do photometric observations for some NEAs, especially PHAs (Potentially Hazardous Asteroids). Another aim is to develop a efficient method (Namely the Lommel-Seeliger ellipsoid method) to inverse the spin parameters, shape and scatter parameters for NEAs. According to Chandrasekhar’s theory--ellipsoidal figures of equilibrium, the lower limit of density of a NEAs will be inferred from its spin rate and Jacobi ellipsoid shape assuming a rubble-pile structure of NEAs. The density or mass of NEAs, apart from the orbital elements, is the necessary data when the hazard index (Torino Scale) of NEAs is estimated. Furthermore, the space pose, shape and inner structure of NEAs are important for the Chinese deep space exploration mission.