Modeling the Effect of Mass-draining on Prominence Eruptions
Modeling the Effect of Mass-draining on Prominence Eruptions
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DOI：
10.3847/1538-4357/ab037a
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发表时间：
2019-01
期刊：
影响因子：
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通讯作者：
J. Jenkins;M. Hopwood;P. D'emoulin;G. Valori;G. Aulanier;D. Long;L. van Driel-Gesztelyi
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文献类型：
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作者：
J. Jenkins;M. Hopwood;P. D'emoulin;G. Valori;G. Aulanier;D. Long;L. van Driel-Gesztelyi
在太阳大气层中可以观测到静止的太阳双折射，持续时间长达几个太阳自转周期。它们的喷发通常是在高度缓慢增加之前，可以持续几个小时到几天。这种日珥高度的增加被认为是由于它们的宿主磁通量绳在驱动喷发的主要平衡丧失之前通过一系列邻近的准平衡过渡。最近的研究表明，日珥质量从一个稳定的，静止的通量绳中移走是这种高度变化的一个可能原因。然而，这些结论是从观察中得出的，可以解释。在这里，我们提出了一个简单的模型来量化的“质量排水”的影响，在爆发前的高度演变的太阳通量绳。磁通绳被建模为悬浮在背景势磁场中的线电流。我们首先表明，包括质量，高达1012公斤，可以修改的高度，在该线电流经历损失的平衡高达14%。接下来，我们表明，在失去平衡之前快速去除质量可以使磁通绳的高度急剧增加，并且在接近失去平衡点时没有上限。这表明，临界高度的平衡的损失可以发生在一个高度范围内，明确取决于磁通绳内的质量的量和演变。最后，我们证明，对于相同数量的排水质量，对磁通绳的高度的影响是两个数量级以上的静态磁共振比活动区磁共振。
Quiescent solar prominences are observed within the solar atmosphere for up to several solar rotations. Their eruption is commonly preceded by a slow increase in height that can last from hours to days. This increase in the prominence height is believed to be due to their host magnetic flux rope transitioning through a series of neighboring quasi-equilibria before the main loss of equilibrium that drives the eruption. Recent work suggests that the removal of prominence mass from a stable, quiescent flux rope is one possible cause for this change in height. However, these conclusions are drawn from observations and are subject to interpretation. Here, we present a simple model to quantify the effect of “mass-draining” during the pre-eruptive height evolution of a solar flux rope. The flux rope is modeled as a line current suspended within a background potential magnetic field. We first show that the inclusion of mass, up to 1012 kg, can modify the height at which the line current experiences loss of equilibrium by up to 14%. Next, we show that the rapid removal of mass prior to the loss of equilibrium can allow the height of the flux rope to increase sharply and without an upper bound as it approaches its loss-of-equilibrium point. This indicates that the critical height for the loss of equilibrium can occur at a range of heights depending explicitly on the amount and evolution of mass within the flux rope. Finally, we demonstrate that for the same amount of drained mass, the effect on the height of the flux rope is up to two orders of magnitude larger for quiescent prominences than for active region prominences.