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Particle Acceleration and Propagation in Strong Flares without Major Solar Energetic Particle Events

机译：在没有主要太阳能粒子事件的情况下，强耀斑中的粒子加速和传播

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Solar energetic particles (SEPs) detected in space are statistically associated with flares and coronal mass ejections (CMEs). But it is not clear how these processes actually contribute to the acceleration and transport of the particles. The present work addresses the question why flares accompanied by intense soft X-ray bursts may not produce SEPs detected by observations with the GOES spacecraft. We consider all X-class X-ray bursts between 1996 and 2006 from the western solar hemisphere. 21 out of 69 have no signature in GOES proton intensities above 10 MeV, despite being significant accelerators of electrons, as shown by their radio emission at cm wavelengths. The majority (11/20) has no type III radio bursts from electron beams escaping towards interplanetary space during the impulsive flare phase. Together with other radio properties, this indicates that the electrons accelerated during the impulsive flare phase remain confined in the low corona. This occurs in flares with and without a CME. Although GOES saw no protons above 10 MeV at geosynchronous orbit, energetic particles were detected in some (4/11) confined events at Lagrangian point L1 aboard ACE or SoHO. These events have, besides the confined microwave emission, dm-m wave type II and type IV bursts indicating an independent accelerator in the corona. Three of them are accompanied by CMEs. We conclude that the principal reason why major solar flares in the western hemisphere are not associated with SEPs is the confinement of particles accelerated in the impulsive phase. A coronal shock wave or the restructuring of the magnetically stressed corona, indicated by the type II and IV bursts, can explain the detection of SEPs when flare-accelerated particles do not reach open magnetic field lines. But the mere presence of these radio signatures, especially of a metric type II burst, is not a sufficient condition for a major SEP event.
机译：在太空中检测到的太阳高能粒子（SEP）在统计上与耀斑和日冕物质抛射（CME）相关。但是尚不清楚这些过程实际上如何促进粒子的加速和传输。本工作解决了以下问题：为什么耀斑伴有强烈的软X射线爆发可能不会产生GOES航天器观测到的SEP。我们考虑了1996年至2006年之间来自西半球的所有X级X射线爆发。 69个中的21个在10 MeV以上的GOES质子强度中没有任何特征，尽管它们是电子的重要加速剂，如厘米波长处的无线电发射所示。大部分（11/20）在脉冲耀斑阶段没有从电子束逃逸到行星际空间的III型无线电脉冲。连同其他无线电特性，这表明在脉冲耀斑阶段加速的电子仍被限制在低电晕中。这发生在有或没有CME的耀斑中。尽管GOES在地球同步轨道上没有看到高于10 MeV的质子，但在ACE或SoHO上的拉格朗日L1点的某些（4/11）局限事件中检测到了高能粒子。这些事件除了局限的微波发射外，还有dm-m型II型和IV型脉冲，表明电晕中有独立的加速器。其中三个由CME陪同。我们得出结论，西半球的主要太阳耀斑与SEP不相关的主要原因是在冲动阶段加速了粒子的约束。由II型和IV型爆发指示的日冕冲击波或磁应力电晕的重组可以解释当耀斑加速的粒子未到达开放磁场线时检测到SEP的原因。但是，仅存在这些无线电签名，尤其是II型度量突发的无线电签名，不足以解决重大SEP事件。

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