论文标题
原球门磁盘的热演化：从$β$冷却到脱钩的气体和灰尘温度
Thermal evolution of protoplanetary disks: from $β$-cooling to decoupled gas and dust temperatures
论文作者
论文摘要
目的：我们探索了年轻的原磁盘的长期演变，其方法是通过磁盘及其周围环境中各种冷却和加热过程确定的热结构的方法。方法：稀二盘极限中的数值流体动力学模拟与三种热进化方案相辅相成：一种简化的$β$冷却方法，有无辐射，磁盘冷却的速率与当地动力学时间成比例，并具有相等的尘埃和气温允许的速度和散热器的速度，并允许散发热量，并散发出散热的冷却，并进行放射的冷却，并放置散热，并散发出散热的冷却性，并散发出散热性的冷却，并散发出散热性的冷却，并散发出散热性的冷却性，灰尘和气温脱钩。结果：我们发现，由于在磁盘演化的早期阶段，幼体磁盘外部区域的尘埃温度可能会显着超过年轻盘外区域的灰尘，并且在低密度磁盘区域中气体和灰尘之间的能量交换缓慢。然而，外膜显示出逆趋势，气体温度下降到灰尘下方。全局磁盘的演化仅对温度解耦敏感较弱。然而，单独的灰尘和气体温度可能会影响化学成分，尘埃演化和磁盘质量估计。恒定的$β$模型没有出色的恒星和背景辐照，由于$β$ - 参数的本质可变性质，因此无法使用更复杂的热方案重现磁盘演化。恒定的$β$模型具有辐照可以更好地匹配动力学和热演化，但该一致性仍然不完整。结论：当将重点放在原月球磁盘的化学或尘埃演化上时，需要单独的灰尘和气温模型，尤其是在亚光金属环境中。
Aims: We explore the long-term evolution of young protoplanetary disks with different approaches to computing the thermal structure determined by various cooling and heating processes in the disk and its surroundings. Methods: Numerical hydrodynamics simulations in the thin-disk limit were complemented with three thermal evolution schemes: a simplified $β$-cooling approach with and without irradiation, in which the rate of disk cooling is proportional to the local dynamical time, a fiducial model with equal dust and gas temperatures calculated taking viscous heating, irradiation, and radiative cooling into account, and also a more sophisticated approach allowing decoupled dust and gas temperatures. Results: We found that the gas temperature may significantly exceed that of dust in the outer regions of young disks thanks to additional compressional heating caused by the infalling envelope material in the early stages of disk evolution and slow collisional exchange of energy between gas and dust in low-density disk regions. The outer envelope however shows an inverse trend with the gas temperatures dropping below that of dust. The global disk evolution is only weakly sensitive to temperature decoupling. Nevertheless, separate dust and gas temperatures may affect the chemical composition, dust evolution, and disk mass estimates. Constant-$β$ models without stellar and background irradiation fail to reproduce the disk evolution with more sophisticated thermal schemes because of intrinsically variable nature of the $β$-parameter. Constant-$β$ models with irradiation can better match the dynamical and thermal evolution, but the agreement is still incomplete. Conclusions: Models allowing separate dust and gas temperatures are needed when emphasis is placed on the chemical or dust evolution in protoplanetary disks, particularly in sub-solar metallicity environments.
