The settling times of solid silicate grains having initial radii of $5\times {10}^{-3}-{10}^{-1}$ cm have been investigated inside the protoplanets in the mass range of 0.3–5 $M_J$ ($M_J$= Jupiter mass, $1M_J=1.8986\times {10}^{30}\text{gm}$), formed via disk instability assuming the energy transport to be conductive-radiative. In this regard, initial distributions of the thermodynamic variables have been estimated. With this obtained distribution of the variables, grain radius spectrum has been attained. Finally, by means of the obtained distribution of the thermodynamic variables and grain radius, the settling times of the silicate grains present in the protoplanets have been estimated. The results received through this investigation were found to be consistent with those obtained in other investigations.

初始半径为的固体硅酸盐晶粒的沉降时间 $5\times {10}^{-3}-{10}^{-\mathrm{1个}}$ cm在原行星内部的质量范围为0.3–5 ${\mathrm{中号}}_{Ĵ}$ （${\mathrm{中号}}_{Ĵ}$木星质量 $\mathrm{1个}{\mathrm{中号}}_{Ĵ}=1.8986\times {10}^{30}\text{gm}$）是通过磁盘不稳定性而形成的，假设能量传输是传导辐射的。在这方面，已经估计了热力学变量的初始分布。利用变量的这种分布，已经获得了晶粒半径谱。最后，借助获得的热力学变量和晶粒半径分布，可以估算出存在于原行星中的硅酸盐晶粒的沉降时间。发现通过本次调查获得的结果与在其他调查中获得的结果一致。