论文标题
从2012年金星运输中测量的Hinode/eis和SDO/AIA仪器中的散射光
Scattered light in the Hinode/EIS and SDO/AIA instruments measured from the 2012 Venus transit
论文作者
论文摘要
从2012年转运的观察结果用于得出经验公式，用于在HINODE Extreme-Ultraviolet成像光谱仪（EIS）和太阳能动力学天文台大气成像组装（AIA）仪器中观察到的太阳盘上的长距离散射光的经验公式。整个太阳能磁盘来自整个太阳能磁盘，而后散射的光被认为是来自感兴趣区域50英寸以内的一个区域。该公式来自Fe XII 195.12 EIS和AIA 193 A频道所观察到的发射线。对弱Fe XIV 274.20 A的研究的研究和30个频道的研究和30 aia在AIA中，A和30 Aia aia在AIA中，AIA 199 AIA散布在AIA中，零散，AIA的散布零散。散射公式适用于EIS波段中的其他发射线。 EIS的公式用于估计Fe XII 195.12的散射光成分，以七个在2010年至2018年之间观察到的纵向冠状孔。发现了56％至100％的散射光贡献，这表明这些特征由散射的光支配，与Wendeln \＆Landi的早期工作一致。来自S X和Si X离子的发射线在与Fe XII相同的温度下形成，通常用于从EIS数据中获得第一个电离势（FIP）偏置 - 也有望由冠状孔中的散射光支配。
Observations from the 2012 transit of Venus are used to derive empirical formulae for long and short-range scattered light at locations on the solar disk observed by the Hinode Extreme ultraviolet Imaging Spectrometer (EIS) and the Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) instruments. Long-range scattered light comes from the entire solar disk, while short-range scattered light is considered to come from a region within 50" of the region of interest. The formulae were derived from the Fe XII 195.12 A emission line observed by EIS and the AIA 193 A channel. A study of the weaker Fe XIV 274.20 A line during the transit, and a comparison of scattering in the AIA 193 A and 304 A channels suggests the EIS scattering formula applies to other emission lines in the EIS wavebands. Both formulae should be valid in regions of fairly uniform emission such as coronal holes and quiet Sun, but not faint areas close (around 100") to bright active regions. The formula for EIS is used to estimate the scattered light component of Fe XII 195.12 for seven on-disk coronal holes observed between 2010 and 2018. Scattered light contributions of 56% to 100% are found, suggesting that these features are dominated by scattered light, consistent with earlier work of Wendeln \& Landi. Emission lines from the S X and Si X ions - formed at the same temperature as Fe XII and often used to derive the first ionization potential (FIP) bias from EIS data - are also expected to be dominated by scattered light in coronal holes.
