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太阳极紫外He II 30.4 nm谱线层析成像及其光谱数据反演

邢阳光 彭吉龙 段紫雯 闫雷 李林 刘越

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太阳极紫外He II 30.4 nm谱线层析成像及其光谱数据反演

邢阳光, 彭吉龙, 段紫雯, 闫雷, 李林, 刘越

Tomographic imaging for solar extreme ultraviolet He II 30.4 nm and spectral data inversion

Xing Yang-Guang, Peng Ji-Long, Duan Zi-Wen, Yan Lei, Li Lin, Liu Yue
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  • 由磁场重联触发的发生在日冕和过渡区域上的具有高度动态的太阳爆发活动是灾害性空间天气的驱动源, 对太阳爆发活动的空间成像和光谱分光测量是实现精准空间天气预报的关键数据来源. 太阳大气上单离子氦的Lyman α跃迁产生波长30.4 nm的He II共振谱线, 相比于邻近的谱线强度至少高一个数量级, 因此能用来观测太阳爆发事件中的物质流动和能量输运过程. 本文针对传统的太阳极紫外成像仪和成像光谱仪的缺陷, 利用光线追迹方法设计了一款工作在He II 30.4 nm波长处的二维光谱层析成像仪器, 采用无狭缝的3个级次(–1, 0, +1)同时衍射成像架构, 单次快照可实现大视场的二维光谱瞬时成像. 由于3个级次图像的空间信息和光谱信息混叠, 利用有限层析投影角度的光谱数据反演算法, 重构了观测目标的三维数据立方体I (x, y, λ).
    Highly dynamic solar eruptive activities occurring over the corona and transition region, triggered off by magnetic field reconnection, are the driving source of disastrous space weather, and the space imaging and spectroscopic measurements of solar eruptive activities are a key data source for accurate space weather forecasting. The He II 30.4 nm resonance line comes from the Lyman α transition of singly ionized helium, which has an anomalous intensity, an order of magnitude higher than the intensities of other transition region lines. In this paper, we propose and design a two-dimensional spectroscopic tomographic imaging instrument operating at He II 30.4 nm wavelength to make up for the shortcomings of conventional solar extreme ultraviolet imager and imaging spectrometer, and adopt a slitless three-order (–1, 0, +1) simultaneous diffraction imaging configuration with a single snapshot to achieve two-dimensional spectroscopy instantaneous imaging with a large field of view. Owing to the confusion of spatial and spectral information of the three orders of images, the three-dimensional data cube I (x, y, λ) of the observed target is reconstructed using a spectral data inversion algorithm with a limited tomographic projection angle.
      通信作者: 李林, bit421@bit.edu.cn ; 刘越, liuyue@bit.edu.cn
    • 基金项目: 中国科学院战略性先导科技专项(批准号: XDA15018300)资助的课题.
      Corresponding author: Li Lin, bit421@bit.edu.cn ; Liu Yue, liuyue@bit.edu.cn
    • Funds: Project supported by the Strategic Pioneer Science and Technology Program of the Chinese Academy of Sciences (Grant No. XDA15018300)
    [1]

    王水, 魏奉思 2007 地球物理学进展 22 1025Google Scholar

    Wang S, Wei F S 2007 Prog. Geophys. 22 1025Google Scholar

    [2]

    汪景琇, 季海生 2013 中国科学: 地球科学 43 883Google Scholar

    Wang J X, Ji H S 2013 Sci. China Earth Sci. 43 883Google Scholar

    [3]

    Hurford G J, Schmahl E J, Schwartz R A, Conway A J, Aschwanden M J, Csillaghy A, Dennis B R, Johns-Krull C, Krucker S1, Lin R P, Mctiernan J, Metcalf T R, Sato J, Smith D M 2002 Solar Phys. 210 61Google Scholar

    [4]

    Milligan R O, Gallagher P T, Mathioudakis M, Bloomfield D S, Keenan F P, Schwartz R A 2006 Astrophys. J. 638 L117Google Scholar

    [5]

    Underwood J H, Neupert W M 1974 Solar Phys. 35 241Google Scholar

    [6]

    Tousey R, Bartoe J D F, Brueckner G E, Purcell J D 1977 Appl. Opt. 16 4Google Scholar

    [7]

    Neupert W M, Epstein G L, Thomas R J, Thompson W T 1992 Solar Physics 137 87Google Scholar

    [8]

    Brosius W, Davila J M, Thomas A. 1998 Astrophys. J. Suppl. Ser. 119 255Google Scholar

    [9]

    Brosius J W, Thomas R J, Davila J M 2000 Astrophys. J. 543 1016Google Scholar

    [10]

    Curdt W, Brekke P, Feldman U, Wilhelm K, Dwivedi B N, Schuhle U, Lemaire P 2001 Astron. Astrophys. 375 591Google Scholar

    [11]

    Thompson W T, Brekke P 2000 Solar Phys. 195 45Google Scholar

    [12]

    Kosugi T, Matsuzaki K, Sakao T, et al. 2007 Solar Phys. 243 3Google Scholar

    [13]

    Culhane J L, Harra L K, Doschek G A, Mariska J T, Watanabe T, Hara H 2005 Adv. Space Res. 36 1494Google Scholar

    [14]

    Pesnell W D, Thompson B J, Chamberlin P C 2012 Solar Phys. 275 3Google Scholar

    [15]

    Lemen J R, Title A M, Akin D J, et al. 2012 Solar Phys. 275 17Google Scholar

    [16]

    Müller D, Cyr O C S, Zouganelis I, et al. 2020 Astron. Astrophys. 642 A1Google Scholar

    [17]

    Anderson M, Appourchaux T, Auchère F, et al. 2020 Astron. Astrophys. 642 A14Google Scholar

    [18]

    甘为群, 黄宇, 颜毅华 2012 中国科学: 物理学 力学 天文学 42 1274Google Scholar

    Gan W Q, Huang Y, Yan Y H 2012 Sci. Sin. Phys. Mech. Astron. 42 1274Google Scholar

    [19]

    甘为群, 颜毅, 华黄宇 2019 中国科学: 物理学 力学 天文学 49 059602Google Scholar

    Gan W Q, Yan Y H, Huang Y 2019 Sci. Sin. Phys. Mech. Astron. 49 059602Google Scholar

    [20]

    Tu C Y, Schwenn R, Donovan E, Marsch E, Wang J S, Xia L D, Zhang Y M 2008 Adv. Space Res. 41 190Google Scholar

    [21]

    Wang J S, Zhang J 2007 Adv. Space Res. 40 1770Google Scholar

    [22]

    Zanna G D, Mason H E 2018 Living Rev. Sol. Phys. 15 5Google Scholar

  • 图 1  成像光谱仪的三维数据立方体I (x, y, λ)

    Fig. 1.  Three-dimensional data cube I (x, y, λ) for imaging spectrometers.

    图 2  太阳极紫外层析成像光谱仪的基础光学架构

    Fig. 2.  Fundamental optical configuration for solar EUV tomography imaging spectrometer.

    图 3  TVLS光栅示意图

    Fig. 3.  Schematic of toroidal varied line space grating.

    图 4  太阳极紫外层析成像光谱仪光路原理图

    Fig. 4.  Optical layout of solar EUV tomographic imaging spectrometer.

    图 5  –1级次像面上的均方根点列图

    Fig. 5.  RMS spot diagram in –1 order imaging surface

    图 6  0级次像面上的均方根点列图

    Fig. 6.  RMS spot diagram in 0 order imaging surface.

    图 7  +1级次像面上的均方根点列图

    Fig. 7.  RMS spot diagram in +1 order imaging surface.

    图 8  反演目标G(x, y0, λ)的有限角度层析投影

    Fig. 8.  Limited angle tomography projection for inversion object G(x, y0, λ).

    图 9  太阳极紫外光谱图 (a)仪器带宽内的谱线强度分布; (b) He II 30.4 nm谱线高斯轮廓分布

    Fig. 9.  Solar extreme ultraviolet spectrogram: (a) Spectral lines intensity distribution in instrument bandwidth; (b) Gaussian distribution of He II 30.4 nm spectral line profile.

    图 10  初始图像和重建图像对比 (a) 初始图像; (b) 重建图像

    Fig. 10.  Comparison of the initial image and the reconstructed image: (a) Initial image; (b) reconstructed image.

    图 11  谱线的中心位置

    Fig. 11.  Central position of line.

    图 12  谱线偏移误差

    Fig. 12.  Error of line shift.

    表 1  层析成像光谱仪的技术指标和系统参数表

    Table 1.  Specifications and system parameters for tomographic imaging spectrometer.

    参数取值
    SpecificationsSpectral range/nm29.4 — 31.4
    FOV/arcmin210 arcmin × 10 arcmin
    Spectral resolution/nm0.003
    Spatial resolution/arcsec0.42
    Line-of-sight velocity/(km·s–1)> 29.61
    System focal length/mm6500
    Pixel size/μm13
    Optical volume/mm31050 mm×
    330 mm×60 mm
    Telescope designRT/mm1888.190
    Conic–1
    Δ/mm80
    Spectral imaging system design1/d0/mm–13200
    rA/mm150
    β6.87×
    i/(°)5.56
    R/mm263.514
    ρ/mm259.940
    b20.0938
    Ruling area/mm220 mm × 20 mm
    下载: 导出CSV

    表 2  层析成像光谱仪的数据重建算法SMART

    Table 2.  Data reconstruction algorithm SMART for tomography imaging spectrometer.

    Smooth multiplicative algebraic reconstruction technique
    1. Initial guess: $G(x, \lambda ) = {I_0}(x){I_\infty }(\lambda )/N$
    2. Projection: $[{I'_{ - 1}}, {I'_0}, {I'_{ + 1}}, {I'_\infty }] = P[G]$
    3. Correction: $\begin{aligned} G = G{\left[ {\frac{ { {I_{ - 1} }(x - \lambda )} }{ { { {I'}_{ - 1} }(x - \lambda )} } } \right]^\gamma }{\left[ {\frac{ { {I_0}(x)} }{ { { {I'}_0}(x)} } } \right]^\gamma }\\ \times{\left[ {\frac{ { {I_{ + 1} }(x + \lambda )} }{ { { {I'}_{ + 1} }(x + \lambda )} } } \right]^\gamma }{\left[ {\frac{ { {I_\infty }(\lambda )} }{ { { {I'}_\infty }(\lambda )} } } \right]^\gamma }\end{aligned}$
    4. Smoothing: $G = G \otimes \displaystyle\frac{1}{ {1 + 2 t + 2 s} }\left[ {\begin{array}{*{20}{c} } 0& t & 0 \\ s& 1 & s \\ 0& t & 0 \end{array} } \right]$
    5. Reprojection: $[{I'_{ - 1}}, {I'_0}, {I'_{ + 1}}, {I'_\infty }] = P[G]$
    6. Evaluate goodness of fit: $\chi _m^2 = 1 + \displaystyle\sum\limits_{x, y} \dfrac{(I'_m - I_m)^2}{N}$
    7. Adjust smoothing parameters: $t = \dfrac{t}{\chi _{ - 1}^2\chi _{ + 1}^2},~~ s = \dfrac{s}{\chi _0^2}$
    8. Loop to step 3
    下载: 导出CSV

    表 3  反演效果评价指标

    Table 3.  Evaluation indicators for the reconstruction

    Quantized indicatorsτkδRMS
    Parametric inversion0.8620.6680.294
    下载: 导出CSV
  • [1]

    王水, 魏奉思 2007 地球物理学进展 22 1025Google Scholar

    Wang S, Wei F S 2007 Prog. Geophys. 22 1025Google Scholar

    [2]

    汪景琇, 季海生 2013 中国科学: 地球科学 43 883Google Scholar

    Wang J X, Ji H S 2013 Sci. China Earth Sci. 43 883Google Scholar

    [3]

    Hurford G J, Schmahl E J, Schwartz R A, Conway A J, Aschwanden M J, Csillaghy A, Dennis B R, Johns-Krull C, Krucker S1, Lin R P, Mctiernan J, Metcalf T R, Sato J, Smith D M 2002 Solar Phys. 210 61Google Scholar

    [4]

    Milligan R O, Gallagher P T, Mathioudakis M, Bloomfield D S, Keenan F P, Schwartz R A 2006 Astrophys. J. 638 L117Google Scholar

    [5]

    Underwood J H, Neupert W M 1974 Solar Phys. 35 241Google Scholar

    [6]

    Tousey R, Bartoe J D F, Brueckner G E, Purcell J D 1977 Appl. Opt. 16 4Google Scholar

    [7]

    Neupert W M, Epstein G L, Thomas R J, Thompson W T 1992 Solar Physics 137 87Google Scholar

    [8]

    Brosius W, Davila J M, Thomas A. 1998 Astrophys. J. Suppl. Ser. 119 255Google Scholar

    [9]

    Brosius J W, Thomas R J, Davila J M 2000 Astrophys. J. 543 1016Google Scholar

    [10]

    Curdt W, Brekke P, Feldman U, Wilhelm K, Dwivedi B N, Schuhle U, Lemaire P 2001 Astron. Astrophys. 375 591Google Scholar

    [11]

    Thompson W T, Brekke P 2000 Solar Phys. 195 45Google Scholar

    [12]

    Kosugi T, Matsuzaki K, Sakao T, et al. 2007 Solar Phys. 243 3Google Scholar

    [13]

    Culhane J L, Harra L K, Doschek G A, Mariska J T, Watanabe T, Hara H 2005 Adv. Space Res. 36 1494Google Scholar

    [14]

    Pesnell W D, Thompson B J, Chamberlin P C 2012 Solar Phys. 275 3Google Scholar

    [15]

    Lemen J R, Title A M, Akin D J, et al. 2012 Solar Phys. 275 17Google Scholar

    [16]

    Müller D, Cyr O C S, Zouganelis I, et al. 2020 Astron. Astrophys. 642 A1Google Scholar

    [17]

    Anderson M, Appourchaux T, Auchère F, et al. 2020 Astron. Astrophys. 642 A14Google Scholar

    [18]

    甘为群, 黄宇, 颜毅华 2012 中国科学: 物理学 力学 天文学 42 1274Google Scholar

    Gan W Q, Huang Y, Yan Y H 2012 Sci. Sin. Phys. Mech. Astron. 42 1274Google Scholar

    [19]

    甘为群, 颜毅, 华黄宇 2019 中国科学: 物理学 力学 天文学 49 059602Google Scholar

    Gan W Q, Yan Y H, Huang Y 2019 Sci. Sin. Phys. Mech. Astron. 49 059602Google Scholar

    [20]

    Tu C Y, Schwenn R, Donovan E, Marsch E, Wang J S, Xia L D, Zhang Y M 2008 Adv. Space Res. 41 190Google Scholar

    [21]

    Wang J S, Zhang J 2007 Adv. Space Res. 40 1770Google Scholar

    [22]

    Zanna G D, Mason H E 2018 Living Rev. Sol. Phys. 15 5Google Scholar

计量
  • 文章访问数:  2786
  • PDF下载量:  38
  • 被引次数: 0
出版历程
  • 收稿日期:  2022-01-12
  • 修回日期:  2022-04-01
  • 上网日期:  2022-07-21
  • 刊出日期:  2022-08-05

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