Modeling the Planetesimal formation Process and Its Comparison to Observations of Vega-like stars

我们研究星子的形成过程。研究了气体盘中部形成的尘埃层引起的湍流、尘埃层的自重力、颗粒电荷和碰撞破碎等影响。我们推导出了星子形成所需的气体盘的性质。为了比较星子形成理论与类织女星恒星的观测结果，我们研究了受恒星辐射和盘状气体影响的尘埃盘结构。我们还进行了尘埃粒子高速碰撞的实验研究，并推导出碰撞碎片的大小分布。最后，我们通过对过渡盘的观测得出了气体盘的性质，过渡盘被认为是类织女星盘的前一阶段。

We study planetesimal formation processes. The following effects are studied : turbulence induced by the dust layer formed at the midplane of the gas disks, self-gravity of the dust layer, grain charges, and collisional fragmentation. We derived properties of the gas disks required for planetesimal formation. In order to compare the planetesimal formation theory to the observations of Vega-like stars, we study dust disk structure affected by the stellar radiation and the disk gas. We have also performed experimental studies of high velocity collisions of dust particles and derived the size distribution of collisional fragments. Finally, we derived the gas disk properties from the observation of the transitional disk, which is considered to be a former stage of Vega-like disks.