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首页> 外文期刊>Annales Geophysicae >A potential lag between the open solar magnetic source flux and solar EUV and X-ray emissions as measured by the Earth's ionosphere during total solar eclipses
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A potential lag between the open solar magnetic source flux and solar EUV and X-ray emissions as measured by the Earth's ionosphere during total solar eclipses

机译：在日全食期间，由地球电离层测得的开放太阳磁场源通量与太阳EUV和X射线发射之间的潜在滞后

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Measurements of the ionospheric E-region during total solar eclipses havebeen used to provide information about the evolution of the solar magneticfield and EUV and X-ray emissions from the solar corona and chromosphere. Bymeasuring levels of ionisation during an eclipse and comparing thesemeasurements with an estimate of the unperturbed ionisation levels (such asthose made during a control day, where available) it is possible to estimatethe percentage of ionising radiation being emitted by the solar corona andchromosphere. Previously unpublished data from the two eclipses presentedhere are particularly valuable as they provide information that supplementsthe data published to date. The eclipse of 23 October 1976 over Australiaprovides information in a data gap that would otherwise have spanned theyears 1966 to 1991. The eclipse of 4 December 2002 over Southern Africa isimportant as it extends the published sequence of measurements. Comparingmeasurements from eclipses between 1932 and 2002 with the solar magneticsource flux reveals that changes in the solar EUV and X-ray flux lag theopen source flux measurements by approximately 1.5 years. We suggest thatthis unexpected result comes about from changes to the relative size of thelimb corona between eclipses, with the lag representing the time taken topopulate the coronal field with plasma hot enough to emit the EUV and X-raysionising our atmosphere.
机译：在日全食期间对电离层E区的测量已用于提供有关太阳磁场和EUV以及太阳日冕和色球层的X射线发射的演化信息。通过测量日食期间的电离水平并将这些测量结果与未干扰的电离水平（例如，在控制日制造的水平）的估计值进行比较，可以估计日冕和色球层所发射的电离辐射的百分比。此处介绍的两个月食之前未发布的数据特别有价值，因为它们提供了补充迄今为止发布的数据的信息。 1976年10月23日在澳大利亚的日食提供了一个数据缺口的信息，而该数据缺口本来可以跨越1966年至1991年。2002年12月4日在南部非洲的日食很重要，因为它扩展了已公布的测量顺序。将1932年至2002年的日食测量值与太阳磁通量进行比较后发现，太阳EUV和X射线通量的变化比开源磁通量测量晚了约1.5年。我们建议这种意外的结果是由于日食之间肢体日冕的相对大小发生变化而引起的，该滞后代表了用足以发射EUV和X射线辐照我们的大气的等离子体在冠状磁场中填充所花费的时间。

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