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首页> 外文期刊>Publications of the Astronomical Society of Japan >Suzaku detection of enigmatic geocoronal solar wind charge exchange event associated with coronal mass ejection
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Suzaku detection of enigmatic geocoronal solar wind charge exchange event associated with coronal mass ejection

机译：朱雀探测与日冕物质抛射有关的神秘地球日冕太阳风电荷交换事件

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Suzaku detected an enhancement of the soft X-ray background associated with solar eruptions on 2013 April 14–15. The solar eruptions were accompanied by an M6.5 solar flare and a coronal mass ejection with magnetic flux ropes. The enhanced soft X-ray background showed a slight variation over half a day and then a clear one in a few hours. The former spectrum was composed of oxygen emission lines, while the later one was characterized by a series of emission lines from highly ionized carbon to silicon. The soft X-ray enhancement originated from geocoronal solar wind charge exchange. However, there appeared to be no significant time correlation with the solar wind proton flux measured by the ACE and WIND satellites. From other solar wind signatures, we considered that an interplanetary shock associated with the coronal mass ejection and a turbulent sheath immediately behind the shock compressed the ambient solar wind ions and then resulted in the soft X-ray enhancement. Furthermore, the enriched emission lines were presumed to be due to an unusual set of ion abundances and ionization states within the coronal mass ejection. We found a better time correlation with the solar wind alpha flux rather than the solar wind proton flux. Our results suggest that the solar wind proton flux is not always a good indicator of geocoronal solar wind charge exchange, especially associated with coronal mass ejections. Instead, the solar wind alpha flux should be investigated when such a soft X-ray enhancement is detected in astronomical observations.
机译：朱雀在2013年4月14日至15日发现与太阳爆发有关的软X射线背景增强。太阳爆发伴随着M6.5太阳耀斑和带有磁通量绳索的日冕物质抛射。增强的软X射线背景在半天内显示出轻微变化，然后在数小时内显示出清晰的变化。前者的光谱由氧气发射线组成，而后者的特征是从高电离碳到硅的一系列发射线。柔和的X射线增强源自地球冠冕日的太阳风电荷交换。但是，与ACE和WIND卫星测得的太阳风质子通量似乎没有明显的时间相关性。从其他太阳风特征来看，我们认为与日冕物质抛射相关的行星际激波和紧接在激波后的湍流鞘压缩了周围的太阳风离子，然后导致了柔和的X射线增强。此外，据推测，富集的发射谱线是由于冠状物质抛射中的一组异常的离子丰度和电离状态所致。我们发现与太阳风α通量相比，与太阳风质子通量更好的时间相关性。我们的结果表明，太阳风的质子通量并不总是表明日冕太阳风电荷交换的良好指标，特别是与日冕物质的抛射有关。相反，当在天文观测中检测到这种软X射线增强时，应研究太阳风的α通量。

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