Radio, Hard X-Ray, and Gamma-Ray Emissions Associated with a Far-Side Solar Event
Radio, Hard X-Ray, and Gamma-Ray Emissions Associated with a Far-Side Solar Event
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DOI：
10.1007/s11207-018-1352-z
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发表时间：
2018-08
期刊：
影响因子：
2.8
通讯作者：
V. Grechnev;V. I. Kiselev;L. Kashapova;A. Kochanov;I. Zimovets;A. Uralov;B. Nizamov;I.Yu. Grigorieva;D. Golovin;M. Litvak;I. Mitrofanov;A. E. S. S. R. I. Ras-A.-E.-S.-S.-R.-I.-Ras-103293452;Irkutsk;Russia;Irkutsk State University;Space Research Institute Ras;Moscow;State Key Laboratory of Space Weather;Nssc Cas;Beijing;China;International Space Science Institute - Beijing;F. O. Physics;Lomonosov Moscow State University;Sternberg Astronomical Institute;Main Astronomical Observatory Ras;S. Petersburg
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文献类型：
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作者：
V. Grechnev;V. I. Kiselev;L. Kashapova;A. Kochanov;I. Zimovets;A. Uralov;B. Nizamov;I.Yu. Grigorieva;D. Golovin;M. Litvak;I. Mitrofanov;A. E. S. S. R. I. Ras-A.-E.-S.-S.-R.-I.-Ras-103293452;Irkutsk;Russia;Irkutsk State University;Space Research Institute Ras;Moscow;State Key Laboratory of Space Weather;Nssc Cas;Beijing;China;International Space Science Institute - Beijing;F. O. Physics;Lomonosov Moscow State University;Sternberg Astronomical Institute;Main Astronomical Observatory Ras;S. Petersburg
远侧太阳爆发事件SOL 2014 -09-01产生了硬电磁和无线电发射，这些发射是用近地Vantage位置的探测器观测到的。特别具有挑战性的是一个长时间> 100 MeV的射线爆发，可能是由加速超过300 MeV的质子产生的。这一观测提出了一个问题，即高能质子如何到达面向地球的太阳表面。一些先前的研究讨论了一种情况，即质子在日冕物质抛射的冲击下加速返回太阳表面。我们继续对这一具有挑战性的事件进行分析，涉及来自南赛射电日像仪的射电图像和来自位于火星附近的火星奥德赛太空观测站上的伽马射线光谱仪高能中子探测器（HEND）的硬X射线数据。HEND记录到未被遮蔽的耀斑发射。结果表明，从地球方向观测到的辐射是由耀斑加速的电子和质子捕获在静态的长日冕环产生的。它们可以在这些环中被喷发激发的冲击波重新加速，最初不是由日冕物质抛射驱动的。结果突出了解决其余问题的方法。
The far-side solar eruptive event SOL2014-09-01 produced hard electromagnetic and radio emissions that were observed with detectors at near-Earth vantage points. Especially challenging was a long-duration > 100 MeV-ray burst that was probably produced by accelerated protons exceeding 300 MeV. This observation raised the question how high-energy protons could reach the Earth-facing solar surface. Some preceding studies discussed a scenario in which protons accelerated by a shock driven by a coronal mass ejection high in the corona return to the solar surface. We continue with the analysis of this challenging event, involving radio images from theNançay Radioheliographand hard X-ray data from theHigh Energy Neutron Detector(HEND) of theGamma-Ray Spectrometeronboard theMars Odysseyspace observatory located near Mars. HEND recorded unocculted flare emission. The results indicate that the emissions observed from the Earth’s direction were generated by flare-accelerated electrons and protons trapped in static long coronal loops. They can be reaccelerated in these loops by a shock wave that was excited by the eruption, being initially not driven by a coronal mass ejection. The results highlight ways to address the remaining questions.