Abstract

Two proton events (>100 MeV; GOES, ACS SPI) associated with weak flares (C1.2, GOES class) in the soft X-ray range that occurred on November 26, 2011, and September 29, 2013, are analyzed. These events were accompanied by significant fluxes of relativistic electrons (>1 MeV; SOHO EPHIN) in the interplanetary space. The time profiles of these protons and electron fluxes were similar during the growth phase, which suggested a common mechanism of their acceleration and propagation. The gradual increase in the flux intensities, in our opinion, shows a prolonged and gradual injection of particles into the interplanetary space, which may be the result of prolonged acceleration or capture. Since prolonged electron capture is unlikely, it is most probable that a prolonged acceleration took place. The prolonged proton acceleration is realized at the post-eruptive phase of solar flares or shock-wave coronal mass ejection. According to the existing theoretical concepts, the acceleration of solar electrons to ~10 MeV by a shock wave is hardly possible. In this case, relativistic electrons and protons were apparently accelerated in the post-eruptive phase of solar flares, where the stochastic acceleration by magnetohydrodynamic turbulence is considered the most probable mechanism.

中文翻译：

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长时间的弱C1.2耀斑：质子和电子的来源

摘要

分析了2011年11月26日和2013年9月29日发生的与软X射线范围内的弱耀斑（C1.2，GOES类）相关的两个质子事件（> 100 MeV； GOES，ACS SPI）。这些事件伴随着行星际空间中相对论电子的大量通量（> 1 MeV； SOHO EPHIN）。这些质子和电子通量的时间分布在生长阶段是相似的，这暗示了它们的加速和传播的共同机制。我们认为，通量强度的逐渐增加表明，向行星际空间的粒子被逐渐地逐渐注入，这可能是加速或捕获时间延长的结果。由于不可能长时间捕获电子，因此很可能会发生长时间加速。延长的质子加速度是在太阳耀斑爆发或激波日冕物质抛射后的阶段实现的。根据现有的理论概念，很难通过冲击波将太阳电子加速至〜10 MeV。在这种情况下，相对论电子和质子显然在太阳耀斑的喷发后阶段被加速，其中磁流体动力湍流的随机加速被认为是最可能的机制。