• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文学位 >The solar transition region: High resolution FUV-EUV imaging and modeling of unresolved coronal funnels as observed with the multi-spectral solar telescope array II: MSSTA II, the second flight.
【24h】

The solar transition region: High resolution FUV-EUV imaging and modeling of unresolved coronal funnels as observed with the multi-spectral solar telescope array II: MSSTA II, the second flight.

机译：太阳过渡区：高分辨率FUV-EUV成像和未解析的日冕漏斗建模，这是通过多光谱太阳望远镜阵列II：MSSTA II进行的第二次飞行。

获取原文
获取原文并翻译 | 示例
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

The Multi-Spectral Solar Telescope Array (MSSTA) is a sounding rocket-borne observatory composed of a set of normal-incidence, multilayer-coated telescopes that obtained selected bandpass spectroheliograms (44A--1550A) of the Solar atmosphere. These images were recorded on specially fabricated XUV and FUV 70mm Kodak film. Rocket launches of this instrument payload took place in 1991 (MSSTA I) and 1994 (MSSTA II) at the White Sands Missile Test Range in New Mexico. Immediately prior to the 1994 launch, visible light focusing tests of each telescope were performed in-situ using a 1951 Standard Air Force High Resolution Test-target to measure optical resolution performance. We determined that the MSSTA II telescopes performed at diffraction limited resolutions down to 0.70 arcsecond at visible wavelengths, and, based on these measurements, we calculate an upper-bound to the focusing errors that incorporate the sum of all uncorrelated system resolution errors that affect resolution performance. Coupling these upper-bound estimates with the in-band diffraction limits, surface scattering errors, and payload pointing jitter, I demonstrate that eleven of nineteen MSSTA II telescopes---having negligible figures of focus errors in comparison to the corresponding visible diffraction limits---performed at sub arcsecond resolution at their operational FUV/EUV/XUV wavelengths during flight. I estimate the in-band performance down to 0.14 +/- 0.08 second of arc. Careful digitizations were then made of selected spectroheliograms, noise-reduced and calibrated to yield energy flux measurements (171 A); and then deconvolved using a blind form of the Richardson-Lucy algorithm to recover the highest angular resolution possible. Using the 1550 A (C IV) and 171 A (Fe IX/X) images, a funnel model that is based on coronal back-heating was constructed and tested against the data. The analysis demonstrates that funnels can account for the quiescent, globally diffuse emission seen in 171 A spectroheliograms, suggesting this emission is mostly of upper transition region origin (T ∼ 650,000 K), and, simultaneously satisfy areal coverage constraints observed at both 171 (60--90%) and 1550 A (≤45%) wavelengths.
机译：多光谱太阳望远镜阵列（MSSTA）是一个探测火箭的天文台，由一组入射的多层镀膜望远镜组成，这些望远镜获得了太阳大气的选定带通光谱图（44A--1550A）。这些图像记录在特制的XUV和FUV 70毫米柯达胶片上。 1991年（MSSTA I）和1994年（MSSTA II）在新墨西哥州的白沙导弹试验场进行了火箭发射。在1994年发射之前，立即使用1951年“标准空军高分辨率”测试目标对每台望远镜进行了可见光聚焦测试，以测量光学分辨率性能。我们确定MSSTA II望远镜在可见光波长下的衍射极限分辨率低至0.70弧秒，并且基于这些测量，我们计算了聚焦误差的上限，该误差包括影响分辨率的所有不相关的系统分辨率误差的总和性能。将这些上限估计值与带内衍射极限，表面散射误差和有效载荷指向抖动相结合，我证明了19台MSSTA II望远镜中的11台-与相应的可见衍射极限相比，聚焦误差的数值可忽略不计- -在飞行过程中以其工作FUV / EUV / XUV波长以亚弧秒分辨率执行。我估计带内性能下降到弧度的0.14 +/- 0.08秒。然后，对选定的光谱辐射图进行仔细的数字化，降低噪声并进行校准，以产生能量通量测量值（171 A）；然后使用Richardson-Lucy算法的盲形式进行反卷积，以恢复可能的最高角分辨率。使用1550 A（C IV）和171 A（Fe IX / X）图像，构建了基于日冕回热的漏斗模型，并针对数据进行了测试。分析表明，漏斗可以解释171 A光谱图中显示的静态，全局弥散发射，这表明该发射主要来自上过渡区起源（T〜650,000 K），并且同时满足在171和171观测到的面覆盖限制（60 --90％）和1550 A（≤45％）的波长。

著录项

相似文献

  • 外文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号