太阳高能粒子中~ 3 He和~ 4 He的相对光谱和注量分布
Relative Spectra and Distributions of Fluences of 3He and 4He in Solar Energetic Particles
摘要：
太阳高能粒子（SEP）具有丰富的光谱和多种离子种类及其同位素的相对丰度。一个长期存在的难题是3 He离子的极度富集。最极端的浓缩现象是在低注量情况下观察到的，即所谓的脉冲事件，据信这种事件是在日冕的耀斑地点产生的，在向地球输送过程中几乎没有散射和加速。在之前的两篇论文（Liu et al. 2004和2006）中，我们展示了这种极端富集如何导致Petrosian和Liu（2004）开发的模型，其中离子被等离子体波或湍流随机加速。在本文中，我们解决的相对分布的3 He和4 He离子的能量密度的Ho等。（2005），这表明，虽然4 He的能量密度的分布像许多其他广泛的特点，太阳耀斑，是相当广泛的，3 He的能量密度是有限的，在一个狭窄的范围内。此外，注量的比率显示出与4 He注量的强相关性。我们的模型的预测之一是存在急剧变化的通量比与湍流的水平或加速率。我们在这里表明，这个功能的模型可以重现所观察到的分布的注量与非常少的自由参数。该模型在两个方面都取得成功的主要原因是完全电离的3 He离子具有独特的荷质比，可以与更多的等离子体模式共振相互作用，并且比4 He更容易加速。基本上在大多数耀斑中，所有的背景3 He离子都被加速到几MeV/核子的范围，而这只发生在非常强的事件中。在较弱的事件中，4 He离子的一小部分达到这样的能量。
英文摘要：
Solar Energetic Particles (SEPs) show a rich variety of spectra and relative abundances of many ionic species and their isotopes. A long standing puzzle has been the extreme enrichments of 3He ions. The most extreme enrichments are observed in low fluence, the so-called impulsive, events which are believed to be produced at the flare site in the solar corona with little scattering and acceleration during transport to the Earth. In two earlier papers (Liu et al. 2004 and 2006) we showed how such extreme enrichments can result in the model developed by Petrosian and Liu (2004), where ions are accelerated stochastically by plasma waves or turbulence. In this paper we address the relative distributions of the fluences of 3He and 4He ions presented by Ho et al. (2005) which show that while the distribution of 4He fluence like many other extensive characteristics of solar flare, is fairly broad, the 3He fluence is limited to a narrow range. Moreover, the ratio of the fluences shows a strong correlation with the 4He fluence. One of the predictions of our model was presence of steep variation of the fluence ratio with the level of turbulence or the rate of acceleration. We show here that this feature of the model can reproduce the observed distribution of the fluences with very few free parameters. The primary reason for the success of the model in both fronts is because fully ionized 3He ion, with its unique charge to mass ratio, can resonantly interact with more plasma modes and accelerate more readily than 4He. Essentially in most flares, all background 3He ions are accelerated to few MeV/nucleon range, while this happens for 4He ions only in very strong events. A much smaller fraction of 4He ions reach such energies in weaker events.
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