Solar Imaging Vector Magnetograph for MAX '91

在MAX91的报告《下一次太阳最大爆发时的耀斑研究》中，六个基本问题确定了第22太阳周期内最优先的耀斑研究：1.耀斑能量是如何存储的，存储在哪里？2.是什么原因耀斑能量释放？3.耀斑能量释放的机制是什么？4.高能粒子是如何加速的？5.耀斑能量传输的机制是什么？6.耀斑效应如何传播到地球？如果没有矢量磁场测量，这些问题都不能得到令人满意的回答。这类观测对理解太阳耀斑的重要性与伽玛射线、X射线或微波观测一样重要。过去两个太阳周期的集体研究经验表明，只有通过协调一致的多光谱观测，我们才有希望了解太阳耀斑是如何发生的以及为什么会发生。在Mees太阳天文台(毛伊岛哈利阿卡拉)使用高性能成像矢量磁强仪进行专门观测，将最大限度地提高MAX91期间(1991-1994年)太阳耀斑和活动区矢量磁场测量的连续性、频率和可靠性。这台仪器将提供必要的太阳矢量磁场数据：(1)了解矢量磁场、X射线和粒子加速的日冕结构和演化之间的关系；(2)测量活动区磁自由能的变化及其与主要太阳耀斑的关系；(3)绘制光球电流图，并将其与日冕X射线结构和高能粒子沉淀地点联系起来。该仪器将使用旋转四分之一波片、法布里-珀罗标准具和声光可调滤光器获得所需的窄带偏振图像，这是根据夏威夷大学望远镜使用这些部件的经验而建立的。它的高空间、光谱和时间分辨率、光谱敏捷性和在线数据简化能力将为MAX91期间的太阳研究带来好处。

In the MAX91 report Flare Research at the Next Solar Maximum, six fundamental questions identify the highest priority flare research during solar cycle 22: 1. How and where is flare energy stored? 2. What causes flare energy release? 3. What are the mechanisms of flare energy release? 4. How are energetic particles accelerated? 5. What are the mechanisms of flare energy transport? 6. How do flare effects propagate to Earth? None of these questions can be answered in a satisfactory manner without vector magnetic field measurements. Such observations are as important to understanding solar flares as are y-ray, X-ray, or microwave observations. The collective research experience during the last two solar cycles has shown that only through coordinated multispectral sets of observations can we hope to understand how and why solar flares occur. Dedicated observations with a high-performace imaging vector magnetograph at Mees Solar Observatory (Haleakala, Maui) will maximize the continuity, frequency, and reliability of vector magnetic field measurements of solar flares and active regions during the MAX91 time period (1991-1994). This instrument will provide solar vector magnetic field data that are necessary: (1) to understand the relationship between the coronal structure and evolution of vector magnetic fields, X-rays, and particle acceleration; (2) to measure the variation of magnetic free energy of active regions and its relationship to major solar flares; (3) to map photospheric electrical currents and relate them to coronal X-ray structures and the sites of energetic particle precipitation. The instrument will obtain the required narrow-band polarimetric images using a rotating quarter-wave plate, Fabry-Perot etalon, and acousto-optic tunable filter, building on experience with these components at the telescopes of the University of Hawaii. Its benefits to solar research during MAX91 will accrue from its high spatial, spectral, and temporal resolution, spectral agility, and on-line data reduction capabilities.