太阳风中氘和He3的异常
The Abundance of Deuterium and He3 in the Solar Wind
摘要：
氘（D）在太阳大气中的相对丰度是未知的。D不仅在恒星中被破坏，它也在活跃恒星的大气中被合成（Rumanovic & Fields 2003）。在几种情况下，当太阳耀斑发生时，通过高能粒子测量（Anglin 1975）和探测D发射的2.223 MeV伽马射线（Terekhov等人，1996; Shih等人，2009），已经探测到太阳中D的产生。我们描述了一个项目，以测量氘的丰度在太阳风，并监测其演变在几年的时间。该仪器由两个栅极、一个氚靶和半导体粒子探测器组成。半球形和同心的网格使用约80至100 kV的电势差加速入射的太阳风离子，并将离子集中在氚靶上。一小部分加速的太阳风氘核与目标相互作用产生3.6 MeV的α粒子，其中一些被相邻的半导体探测器记录下来。1975年，类似的仪器在太空中成功测试，以观察氢极光中的正极光离子。
英文摘要：
The relative abundance of deuterium (D) in the solar atmosphere is not known. D is not only destroyed in stars, it is also synthesized in the atmospheres of active stars (Prodanovic & Fields 2003). In several cases, production of D in the sun has been detected when solar flares occur, using both energetic particle measurements (Anglin 1975) and by detection of 2.223 MeV gamma rays emitted by D (Terekhov et al. 1996; Shih et al. 2009). We describe a project to measure the abundance of deuterium in the solar wind, and to monitor its evolution during a several-year period. The instrument consists of two grids, a tritium target, and semiconductor particle detectors. The grids, which are hemispherical and concentric, accelerate the incident solar wind ions using a potential difference on the order of ~80 to 100 kV and concentrate the ions on the tritium target. A fraction of the solar wind deuterons thus accelerated interact with the target to produce 3.6 MeV alpha particles, some of which are recorded by adjacent semiconductor detectors. A similar instrument was successfully tested in space in 1975 in order to observe positive auroral ions in a hydrogen aurora.
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