论文标题
带有磁盘风的不断发展的原球门磁盘的分析模型
An Analytic Model for an Evolving Protoplanetary Disk with a Disk Wind
论文作者
论文摘要
我们描述了一个由粘度和磁盘风驱动的不断发展的原月球磁盘的分析模型。磁盘是通过粘度产生的出色照射和能量加热的。进化由3个参数控制：（i）在参考距离和温度下向中心恒星的流入速度，（ii）磁盘风引起的这种流入的分数，以及（iii）通过风的质量损失率相对于磁盘内的内向磁带。该模型给出了磁盘中平面温度和表面密度，这是距离恒星时间和距离的函数。它旨在提供一种有效的方法来计算原星磁盘中的条件，以用于行星形成的模拟。在模型中，磁盘由粘度径向扩散，而质量却散布在恒星上。径向扩散是降低内盘表面密度的主要因素。圆盘质量在后期仍然很大。由于强烈的粘性加热，内部区域的温度在早期时期很高。由风中主导的磁盘会少得多的径向扩散和较弱的粘性加热。这些磁盘在晚期的质量比纯粘性磁盘要低得多。当通过风的质量损失很大时，内部磁盘中的表面密度梯度变浅，在极端情况下，斜率可能会呈正。
We describe an analytic model for an evolving protoplanetary disk driven by viscosity and a disk wind. The disk is heated by stellar irradiation and energy generated by viscosity. The evolution is controlled by 3 parameters: (i) the inflow velocity towards the central star at a reference distance and temperature, (ii) the fraction of this inflow caused by the disk wind, and (iii) the mass loss rate via the wind relative to the inward flux in the disk. The model gives the disk midplane temperature and surface density as a function of time and distance from the star. It is intended to provide an efficient way to calculate conditions in a protoplanetary disk for use in simulations of planet formation. In the model, disks dominated by viscosity spread radially while losing mass onto the star. Radial spreading is the main factor reducing the surface density in the inner disk. The disk mass remains substantial at late times. Temperatures in the inner region are high at early times due to strong viscous heating. Disks dominated by a wind undergo much less radial spreading and weaker viscous heating. These disks have a much lower mass at late times than purely viscous disks. When mass loss via a wind is significant, the surface density gradient in the inner disk becomes shallower, and the slope can become positive in extreme cases.
