The EUV imaging spectrometer for Hinode
The EUV imaging spectrometer for Hinode
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DOI：
10.1007/s01007-007-0293-1
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发表时间：
2007-06-01
期刊：
影响因子：
2.8
通讯作者：
Wikstol, O.
中科院分区：
文献类型：
--
作者：
Culhane, J. L.;Harra, L. K.;Wikstol, O.
Hinode上的极紫外成像光谱仪将观测太阳日冕和上过渡区发射线，波长范围为170 - 210埃和250 - 290埃。线质心位置和轮廓宽度将允许测量等离子体速度和湍流或非热线加宽。我们将从谱线强度导出局部等离子体温度和密度。该光谱将允许精确测定各种日冕和过渡区结构内的差分发射测量和元素丰度。这些强大的光谱诊断将允许识别和表征在太阳上层大气中的磁重联和波传播过程。我们还将直接研究日冕环的详细演化和加热。EIS仪器采用独特的双元件法向入射设计。光学元件涂有优化的多层涂层。我们选择了高效、背照式、薄型CCD。这些设计特征使得仪器的有效面积比以前的轨道EUV光谱仪大得多，在最亮的谱线中典型的有源区曝光时间为2 - 5秒。EIS可以扫描6x8.5弧分的视野，空间和速度尺度为1弧秒和每像素25公里（-1）。本文详细介绍了仪器的设计、绝对校准和性能。EIS将与太阳光学望远镜（SOT）和X射线望远镜（XRT）一起沿着用于太阳大气的广泛研究。
The EUV Imaging Spectrometer (EIS) on Hinode will observe solar corona and upper transition region emission lines in the wavelength ranges 170 - 210 angstrom and 250 - 290 angstrom. The line centroid positions and profile widths will allow plasma velocities and turbulent or non-thermal line broadenings to be measured. We will derive local plasma temperatures and densities from the line intensities. The spectra will allow accurate determination of differential emission measure and element abundances within a variety of corona and transition region structures. These powerful spectroscopic diagnostics will allow identification and characterization of magnetic reconnection and wave propagation processes in the upper solar atmosphere. We will also directly study the detailed evolution and heating of coronal loops. The EIS instrument incorporates a unique two element, normal incidence design. The optics are coated with optimized multilayer coatings. We have selected highly efficient, backside-illuminated, thinned CCDs. These design features result in an instrument that has significantly greater effective area than previous orbiting EUV spectrographs with typical active region 2 - 5 s exposure times in the brightest lines. EIS can scan a field of 6x8.5 arc min with spatial and velocity scales of 1 arc sec and 25 kms(-1) per pixel. The instrument design, its absolute calibration, and performance are described in detail in this paper. EIS will be used along with the Solar Optical Telescope (SOT) and the X-ray Telescope (XRT) for a wide range of studies of the solar atmosphere.