论文标题
具有对流不稳定区域的粘性原月球磁盘的演变。 ii。增生制度和长期动态
Evolution of a Viscous Protoplanetary Disk with Convectively Unstable Regions. II. Accretion Regimes and Long-Term Dynamics
论文作者
论文摘要
在本文中，我们开始研究对流，这可能是原月球磁盘中情节增生的可能因素。在第i i条列出的模型中，积聚历史记录以不同的速度和物质流入的区域从信封到磁盘上进行分析。结果表明，爆发状态发生在广泛的参数中。还对磁盘的长期演变进行了建模，包括与信封的时间流入的减少。已经证明，磁盘变得对流不稳定，并在数百万年内保持了恒星的类似爆发的积聚。同时，不稳定性扩展到几十个天文单位的区域，并随时间逐渐减少。还表明，在磁盘演化的早期阶段，磁盘外部的重力不稳定性以及对流不稳定的内部区域中的尘埃蒸发出现。这项研究的总体结论是，对流可以用作Protostellar磁盘中情节增生的机制之一，但是需要使用更一致的流体动力学模型来验证该结论。
In this article, we proceed to study convection as a possible factor of episodic accretion in protoplanetary disks. Within the model presented in Article~I, the accretion history is analyzed at different rates and areas of matter inflow from the envelope onto the disk. It is shown that the burst-like regime occurs in a wide range of parameters. The long-term evolution of the disk is also modeled, including the decreasing-with-time matter inflow from the envelope. It is demonstrated that the disk becomes convectively unstable and maintains burst-like accretion onto the star for several million years. Meanwhile, the instability expands to an area of several tens of astronomical units and gradually decreases with time. It is also shown that at early stages in the disk evolution, conditions arise for gravitational instability in the outer parts of the disk and for dust evaporation in the convectively unstable inner regions. The general conclusion of the study is that convection can serve as one of the mechanisms of episodic accretion in protostellar disks, but this conclusion needs to be verified using more consistent hydrodynamic models.
