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首页> 外文期刊>Space Weather >Ionospheric electron density response to solar flares as viewed by Digisondes
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Ionospheric electron density response to solar flares as viewed by Digisondes

机译：Digisondes观察到的电离层电子密度对太阳耀斑的响应

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摘要

Solar flares are explosive events on the Sun that release energetic particles, X-rays, EUV, and radio emissions that have an almost immediate impact on Earth's ionosphere-thermosphere (IT) system and/or on operational systems that are affected by IT conditions. To assess such impacts, it is a key that we know how the ionosphere is modified. An objective of this paper is to evaluate how digisondes might serve in this role. Toward this end we utilize data from the Millstone Hill digisonde to reveal the height versus time bottomside F region responses to three X-class flares (X28, X8.3, and X1.7) at a middle latitude site. In terms of percent increase with respect to a preflare hourly mean, the long-lived (> 15–30 min) responses to these flares maximize between about 150 and 250 km and measurably last ∼0.75–1.5 h after flare maximum. The relative magnitudes of these responses are complicated by flare position on the solar disk, which determines how much of the EUV solar emissions are attenuated by the solar atmosphere. At Millstone Hill there was little measurable response to these flares near the F2 layer peak; however, at the magnetic equator location of Jicamarca, the F2 peak electron density increased by ∼15–40%. Herein, all of these flare response characteristics are interpreted in terms of available modeling results. We propose that such digisonde data, in combination with first-principles models and high-resolution measurements of solar EUV flux emissions (e.g., from Solar Dynamics Observatory/EUV Variability Experiment), can lead us to a deeper understanding of the ionospheric photochemistry and dynamics that underlies a predictive capability.
机译：太阳耀斑是太阳上的爆炸性事件，释放出高能粒子，X射线，EUV和无线电辐射，这些辐射几乎立即影响地球的电离层-热层（IT）系统和/或受IT条件影响的操作系统。要评估这种影响，关键是我们知道电离层如何被修改。本文的目的是评估洋地黄醛在这种作用中的作用。为此，我们利用Millstone Hill digisonde的数据揭示了中纬度站点对三个X级耀斑（X28，X8.3和X1.7）的底部F区域的高度与时间的关系。以相对于耀斑前小时平均值的百分比增加而言，对这些耀斑的长寿命（> 15–30分钟）响应在约150至250 km之间最大，并且可测量地在耀斑最大后持续0.75〜1.5 h。这些响应的相对大小会由于太阳圆盘上的耀斑位置而变得复杂，而耀斑的位置决定了太阳大气层会减弱多少EUV太阳辐射。在Millstone Hill，对F2层峰值附近的这些耀斑几乎没有可测量的响应。但是，在Jicamarca的磁赤道位置，F2峰值电子密度增加了约15-40％。在本文中，所有这些耀斑响应特征都是根据可用的建模结果来解释的。我们建议将这样的digisonde数据与第一性原理模型和太阳EUV通量排放的高分辨率测量结果（例如，来自太阳动力学天文台/ EUV变异性实验的结果）相结合，可以使我们对电离层光化学和动力学有更深入的了解。这是预测能力的基础。

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