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首页> 外文期刊>The Astrophysical journal >Hα POLARIZATION DURING A WELL-OBSERVED SOLAR FLARE: PROTON ENERGETICS AND IMPLICATIONS FOR PARTICLE ACCELERATION PROCESSES
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Hα POLARIZATION DURING A WELL-OBSERVED SOLAR FLARE: PROTON ENERGETICS AND IMPLICATIONS FOR PARTICLE ACCELERATION PROCESSES

机译：良好观测的太阳耀斑中的Hα极化：质子能量学及其对粒子加速过程的影响

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摘要

Observations of polarization of chromospheric lines in solar flares can constrain the energy flux in accelerated protons. In this paper we analyze recently reported observations of Hα linear polarization obtained during a rather well observed flare on 1989 June 20. Modeling of the magnitude and orienta- tion of the Ha polarization provides a constraint on the flux of low energy protons, while simultaneous gamma-ray and hard X-ray observations provide constraints on the fluxes of ≥l0 MeV protons and ≥50 keV electrons, respectively. These, plus information on the energetics of the low- temperature and high-temperature thermal emissions, permit evaluation of both the absolute and relative roles of electrons and protons in the flare energy budget. We find that accelerated protons with energies ≥200 keV can contain a significant portion of the total energy released during the flare, consistent with a steep extrapolation of the proton spectrum to such relatively low energies. We discuss these results in light of a unified electron/proton stochastic particle acceleration model and show that the energetics are indeed consistent with this large proton energy content.
机译：太阳耀斑中色球层极化的观察可以限制加速质子中的能量通量。在本文中，我们分析了最近报道的1989年6月20日在相当良好观察到的耀斑中获得的Hα线性极化的观察结果。Ha极化的大小和方向建模为低能质子的通量提供了约束，而同时存在伽马X射线和硬X射线观测分别对≥10MeV质子和≥50keV电子的通量提供了约束。这些，再加上有关低温和高温热辐射能量的信息，可以评估电子和质子在火炬能量预算中的绝对作用和相对作用。我们发现，能量≥200keV的加速质子可以包含耀斑释放的总能量的很大一部分，这与质子谱向如此低能量的陡峭外推相符。我们根据统一的电子/质子随机粒子加速模型讨论这些结果，并表明高能确实与这种大的质子能量含量一致。

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