论文标题
阳光下的正面过程
Positron Processes in the Sun
论文作者
论文摘要
正电子在从几百keV到> 1 GEV的能量的太阳能伽马射线排放中起着重要作用。尽管导致太阳大气中正电子产生的过程是众所周知的，但与环境颗粒相互作用的基础能量颗粒的起源知之甚少。为了理解太阳的完整伽马射线光谱，我回顾了有助于观察到的伽马射线频谱的关键排放机制，重点是涉及正面的伽马射线。特别是，我审查了低能能下的0.511 MEV正电子歼灭线和阳性连续排放的过程，以及在太阳喷发中高能量下的Pion Continuum发射。据认为，在耀斑重新连接和受冠状质量驱动驱动的冲击时加速的颗粒负责观察到的伽马射线特征。根据最近的一些发展，我认为来自两种机制的能量颗粒可能在冲动期间有助于观察到的γ射线频谱，而冲击机制则导致了扩展相。
Positrons play a major role in the emission of solar gamma-rays at energies from a few hundred keV to >1 GeV. Although the processes leading to positron production in the solar atmosphere are well known, the origin of the underlying energetic particles that interact with the ambient particles is poorly understood. With the aim of understanding the full gamma-ray spectrum of the Sun, I review the key emission mechanisms that contribute to the observed gamma-ray spectrum, focusing on the ones involving positrons. In particular, I review the processes involved in the 0.511 MeV positron annihilation line and the positronium continuum emissions at low energies, and the pion continuum emission at high energies in solar eruptions. It is thought that particles accelerated at the flare reconnection and at the shock driven by coronal mass ejections are responsible for the observed gamma-ray features. Based on some recent developments I suggest that energetic particles from both mechanisms may contribute to the observed gamma-ray spectrum in the impulsive phase, while the shock mechanism is responsible for the extended phase.
