Solar Imaging Vector Magnetograph for MAX '91

MAX 91 太阳成像矢量磁仪

• 批准号: 8813157
• 负责人: Richard Canfield
• 金额: $ 23.22万
• 依托单位: University of Hawaii
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1988
• 资助国家: 美国
• 起止时间: 1988-08-01 至 1992-01-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=8813157&HistoricalAwards=false
• 关键词: Solar; Imaging; Vector; Magnetograph; MAX

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.

在MAX91报告下一个太阳活动极大期的耀斑研究中，六个基本问题确定了太阳活动周期22期间最优先的耀斑研究：耀斑能量是如何储存的？储存在哪里？2. 是什么导致耀斑能量释放？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. 耀斑效应是如何传播到地球的？没有矢量磁场测量，这些问题都不能得到满意的回答。这类观测与y射线、x射线或微波观测对了解太阳耀斑同样重要。过去两个太阳活动周期的集体研究经验表明，只有通过协调的多光谱观测，我们才有希望了解太阳耀斑发生的方式和原因。Mees太阳观测站（Maui, Haleakala）的高性能成像矢量磁仪将在MAX91期间（1991-1994）最大限度地提高太阳耀斑和活动区矢量磁场测量的连续性、频率和可靠性。该仪器将提供必要的太阳矢量磁场数据：(1)了解日冕结构与矢量磁场演化、x射线和粒子加速之间的关系；(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，并将其与日冕x射线结构和高能粒子沉淀的位置联系起来。该仪器将利用旋转的四分之一波片、法布里-佩罗标准子和声光可调滤波器获得所需的窄带偏振图像，并以夏威夷大学望远镜的这些组件的经验为基础。它在MAX91期间的太阳能研究将受益于其高空间、光谱和时间分辨率、光谱灵活性和在线数据缩减能力。