Abstract

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.

中文翻译：

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具有对流不稳定区域的粘性原行星盘的演变。二。增生制度和长期动态

摘要

在本文中，我们继续研究对流作为原行星盘中偶发积聚的可能因素。在第一条介绍的模型中，以不同的速率和从信封到磁盘的物质流入区域分析吸积历史。结果表明，类突发状态出现在很宽的参数范围内。还对磁盘的长期演变进行了建模，包括随着时间的推移从信封中流入的物质逐渐减少。事实证明，该盘对流变得不稳定，并在恒星上维持了爆发状增生几百万年。同时，不稳定性扩大到几十个天文单位的面积，并随时间逐渐减小。还表明，在磁盘开发的早期阶段，在盘的外部产生重力不稳定性，在对流不稳定的内部产生粉尘蒸发的条件。该研究的一般结论是，对流可以作为星际盘中偶发积聚的机制之一，但是需要使用更一致的流体动力学模型来验证这一结论。