太阳中的正电子过程
Positron Processes in the Sun
摘要：
正电子在太阳伽马射线的发射中起着重要作用，能量从几百keV到>1 GeV。虽然太阳大气中产生正电子的过程是众所周知的，但与周围粒子相互作用的高能粒子的起源却知之甚少。为了了解太阳的完整伽马射线光谱，我回顾了对观测到的伽马射线光谱有贡献的关键发射机制，重点是涉及正电子的发射机制。特别是，我审查的过程中涉及的0.511 MeV的正电子湮没线和正电子素连续发射在低能量，和π介子连续发射在高能量的太阳爆发。人们认为，在耀斑重联和由日冕物质抛射驱动的冲击波中加速的粒子是观测到的伽马射线特征的原因。基于最近的一些发展，我建议，高能粒子从这两种机制可能有助于所观察到的伽玛射线谱在脉冲阶段，而冲击机制是负责扩展阶段。
英文摘要：
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.
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