微粒子動態系統用來研究岩屑盤的分佈密度。本文中，我們主要是研究β參數對織女星岩屑盤動態系統的影響。假設在內盤的粒子在運行過程中會因碰撞而爆炸變成許多更小的微粒子，然後受中心恆心的地心引力與輻射影響使得粒子外移形成外盤。我們利用β參數建立模擬系統且使用1/R函數檢驗其分佈密度。我們發現，使用多種β參數模擬系統所產生的結果最符合1/R函數。因為(1)不同的β參數的微粒子會用有不同的運行軌道和速度;(2)儘管部分微粒子被吹出外盤，系統仍產生新的微粒子以維持外盤的分佈密度。我們利用電腦模擬論證使用多樣β參數所模擬的結果會是最理想的情況。

The grains' dynamical models are employed to study the density distribution of debris discs. In this thesis, we investigate the effects of β, where β is the value of the ratio between the radiation pressure force and the gravitational, to simulate the Vega's outer disc. We set the particles, in the inner disc, would be collided with each other and be broken into many dust grains when them move. Those dust grains would be blown out, over a long period of time, then they would form the start's outer disc. In the end, we examine whether a model with an 1/R profile could be formed. We find that the model with multiple size of dust grains gives the best fit to the 1/R profile because that (1) the grains with distinct β have distinct radial velocities; (2) the new grains are generated frequently enough to replace those have been blown out. With the above two conditions, models can have a steady out-moving flow with an approximate 1/R profile.

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