标题： 非WKB模型的FIP效应：对太阳日冕加热及日冕氦和氖丰度的影响 显示英文标题

标题： Non-WKB Models of the FIP Effect: Implications for Solar Coronal Heating and the Coronal Helium and Neon Abundances

摘要： 我们更详细地重新审视了太阳色球层中元素丰度分馏的模型，该模型导致太阳日冕和太阳风中出现“FIP效应”。那些第一电离势低于约10 eV的元素（即主要在色球层中被电离的元素）在日冕中的丰度比在色球层中高3到4倍。我们使用非WKB处理方法来模拟阿尔芬波在色球层中的传播，并评估与这些波相关的ponderomotive力。在太阳条件下，这种力通常在色球层中向上指向，并增强了色球层离子在日冕中的丰度。我们的新方法捕捉到了太阳日冕丰度异常的主要特征，包括氦相对于氢的耗尽，以及最近文献中讨论过的氖可能的耗尽。我们还提出，FIP效应为阿尔芬波的能量通量提供了迄今为止最有力的证据，足以加热日冕。然而，似乎为了维持在太阳日冕和低速太阳风中观察到的相对规则且无强烈变化的分馏模式，这些波也必须在日冕中产生。 显示英文摘要

摘要： We revisit in more detail a model for element abundance fractionation in the solar chromosphere, that gives rise to the "FIP Effect" in the solar corona and wind. Elements with first ionization potential below about 10 eV, i.e. those that are predominantly ionized in the chromosphere, are enriched in the corona by a factor 3-4. We model the propagation of Alfven waves through the chromosphere using a non-WKB treatment, and evaluate the ponderomotive force associated with these waves. Under solar conditions, this is generally pointed upwards in the chromosphere, and enhances the abundance of chromospheric ions in the corona. Our new approach captures the essentials of the solar coronal abundance anomalies, including the depletion of He relative to H, and also the putative depletion of Ne, recently discussed in the literature. We also argue that the FIP effect provides the strongest evidence to date for energy fluxes of Alfven waves sufficient to heat the corona. However it appears that these waves must also be generated in the corona, in order to preserve the rather regular fractionation pattern without strong variations from loop to loop observed in the solar corona and slow speed solar wind.