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arXiv 2201.02388astro-ph.SRphysics.space-ph
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流光和伪流光与日球层的动力学耦合

The Dynamic Coupling of Streamers and Pseudostreamers to the Heliosphere

V. Aslanyan, D. I. Pontin, A. K. Higginson, P. F. Wyper, R. B. Scott, S. K. Antiochos

备注：
This article was submitted under duress from an unreasonable reviewer for a separate article
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摘要：

慢太阳风通常被认为是由开放和封闭的日冕磁通量在流光和伪流光相互作用的结果。我们使用3维磁流体动力学模拟来确定详细的结构和动力学的开闭相互作用，驱动光球对流。光球磁场模型包括一个全球偶极子产生的流光一起产生一个大的寄生极性区域的伪流光，分离卫星冕洞的主极孔。我们的数值域延伸到30个太阳半径，包括一个等温的太阳风，使日冕和日光层之间的耦合可以严格计算。这个系统是通过施加一个大的准随机表面流，捕获驱动的日冕通量在流光和pseudostreamer边界附近的超颗粒运动。我们描述了由此产生的结构和动力学。交换重联占主导地位的流光和pseudostreamer边界的演变，但由此产生的结构的细节是明显不同的。此外，我们计算在原位签名的重联，并确定从内日光层回到太阳的测试航天器轨道的动态映射。我们讨论了我们的研究结果的影响，解释观测从内日光层任务，如帕克太阳探测器和太阳轨道器，并为空间天气建模的缓慢太阳风。

英文摘要：

The slow solar wind is generally believed to result from the interaction of open and closed coronal magnetic flux at streamers and pseudostreamers. We use 3-dimensional magnetohydrodynamic simulations to determine the detailed structure and dynamics of open-closed interactions that are driven by photospheric convective flows. The photospheric magnetic field model includes a global dipole giving rise to a streamer together with a large parasitic polarity region giving rise to a pseudostreamer that separates a satellite coronal hole from the main polar hole. Our numerical domain extends out to 30 solar radii and includes an isothermal solar wind, so that the coupling between the corona and heliosphere can be calculated rigorously. This system is driven by imposing a large set of quasi-random surface flows that capture the driving of coronal flux in the vicinity of streamer and pseudostreamer boundaries by the supergranular motions. We describe the resulting structures and dynamics. Interchange reconnection dominates the evolution at both streamer and pseudostreamer boundaries, but the details of the resulting structures are clearly different from one another. Additionally, we calculate in situ signatures of the reconnection and determine the dynamic mapping from the inner heliosphere back to the Sun for a test spacecraft orbit. We discuss the implications of our results for interpreting observations from inner heliospheric missions, such as Parker Solar Probe and Solar Orbiter, and for space weather modeling of the slow solar wind.

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