低日冕中的离子温度：太阳极小期的极冕洞
Ion Temperatures in the Low Solar Corona: Polar Coronal Holes at Solar Minimum
摘要：
在目前的工作中，我们使用的深曝光光谱所采取的SUMER光谱仪在极冕洞在1996年测量的离子温度的大量离子在许多不同的高度以上的肢体之间的0.03和0.17太阳半径。我们发现，测量的离子温度几乎总是大于电子温度，并表现出非单调的荷质比的依赖性。我们使用这些测量提供经验约束的离子加热和加速的理论模型的基础上逐步补充离子回旋波。我们比较所需的波功率加热离子的观测水平的预测的基础上的各向异性磁流体动力学湍流模型。我们发现，经验加热模型和湍流级联模型同意彼此，并解释了测量的离子温度，为荷质比小于约0.25。然而，荷质比超过0.25的离子与模型不一致;它们需要被加热到测量的离子温度的波功率显示出随着荷质比的增加（即，随着频率的增加），这不能用传统的级联模型来解释。我们讨论了可能的额外的过程，可能是负责推断盈余的波能。
英文摘要：
In the present work we use a deep-exposure spectrum taken by the SUMER spectrometer in a polar coronal hole in 1996 to measure the ion temperatures of a large number of ions at many different heights above the limb between 0.03 and 0.17 solar radii. We find that the measured ion temperatures are almost always larger than the electron temperatures and exhibit a non-monotonic dependence on the charge-to-mass ratio. We use these measurements to provide empirical constraints to a theoretical model of ion heating and acceleration based on gradually replenished ion-cyclotron waves. We compare the wave power required to heat the ions to the observed levels to a prediction based on a model of anisotropic magnetohydrodynamic turbulence. We find that the empirical heating model and the turbulent cascade model agree with one another, and explain the measured ion temperatures, for charge-to-mass ratios smaller than about 0.25. However, ions with charge-to-mass ratios exceeding 0.25 disagree with the model; the wave power they require to be heated to the measured ion temperatures shows an increase with charge-to-mass ratio (i.e., with increasing frequency) that cannot be explained by a traditional cascade model. We discuss possible additional processes that might be responsible for the inferred surplus of wave power.
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