CAJ | 학술논문

计算了粘滞演化阶段原太阳吸积盘结构.采用稳态标准吸积盘模型来描述盘中湍动粘滞；忽略其径向能量传输，将垂直结构作为一维问题处理.假设盘作Keplerian较差旋转，处于流体力学平衡和局域热平衡，盘由粘滞耗散加热，能量通过对流和辐射向外传输.结果表明，对温度敏感的不透明度是决定盘结构的重要因素；原太阳吸积盘为冷的薄盘，盘中热对流不稳定性由外而内，由上而下地终结；行星的形成应首先开始于对流终结的区域.
계산료점체연화계단원태양흡적반결구.채용은태표준흡적반모형래묘술반중단동점체；홀략기경향능량전수，장수직결구작위일유문제처리.가설반작Keplerian교차선전，처우류체역학평형화국역열평형，반유점체모산가열，능량통과대류화복사향외전수.결과표명，대온도민감적불투명도시결정반결구적중요인소；원태양흡적반위랭적박반，반중열대류불은정성유외이내，유상이하지종결；행성적형성응수선개시우대류종결적구역.
The structure of protosolar accretion disk during viscous diffusion stage is calculated. The standard α model is used to describe the viscosity in the optically thick protosolar accretion disc. The energy transport associated with radial motions is neglected and the vertical structure is constructed by assuming a Keplerian rotation and local hydrostatic and thermal equilibrium. The disk is heated by viscous dissipation and energy is transported by convection or radiation. It is found that the dependence of opacity on temperature is important to the disk structure. For the cold protosolar accretion disc,convective instability will gradually end from the outer region to the center and from the surface to central plane. So the formation of planets should first take place in the region where convection ends.