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arxiv: 2605.24498 · v1 · pith:XGZABP4Bnew · submitted 2026-05-23 · 🌌 astro-ph.SR · astro-ph.IM

Observational Technological Innovations and Future Development of the Lijiang Coronagraph

Xuefei Zhang , Yu Liu , Tengfei Song , Mingyu Zhao , Xiaobo Li , Mingzhe Sun , Feiyang Sha , Xiande Liu This is my paper

Pith reviewed 2026-06-30 12:24 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.IM
keywords coronal green linemagnetic field correlationLijiang CoronagraphCME early warningsolar coronaEUV correlationstray light suppressionground-based observations
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The pith

Lijiang Coronagraph data shows 1.1 solar radii as the peak correlation zone between coronal green line brightness and magnetic field intensity.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper describes a series of upgrades to the Lijiang Coronagraph, including an automatic operating system, a dual-band observation setup, image differencing for stray light control, and precise calibration steps. These changes produced cleaner data that identify 1.1 solar radii as the location where green line emission tracks magnetic field strength most closely. The same dataset also shows the green line tracking the 21.1 nm EUV channel from SDO/AIA at correlation values of 0.89 to 0.99, which the authors link to improved early warning potential for coronal mass ejections.

Core claim

The upgraded Lijiang Coronagraph has produced observations establishing that 1.1 solar radii is a highly correlated region between coronal green line brightness and magnetic field intensity, while confirming a correlation coefficient of 0.89-0.99 between the green line and the SDO/AIA 21.1 nm band, thereby supporting early warning research on coronal mass ejections.

What carries the argument

Stray light suppression via image differencing before and after cleaning, which removes instrumental artifacts to enable reliable correlation measurements between green line brightness and magnetic field data.

If this is right

  • The correlations supply direct observational constraints for testing models of coronal heating.
  • The same data help trace the source regions of the slow solar wind.
  • The documented upgrades provide a template for building larger-aperture ground-based coronagraphs.
  • The instrument contributes continuous low-corona monitoring to the worldwide observation network.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the 1.1 solar radii correlation persists across multiple independent instruments, ground-based green line measurements could serve as a low-cost proxy for magnetic field strength in the low corona.
  • High-altitude sites with low turbulence may become preferred locations for future solar observatories that aim to complement space-based EUV data.
  • The dual-band and differencing techniques could be adapted to other existing coronagraphs to improve their stray light performance without hardware changes.

Load-bearing premise

The reported correlations between green line brightness, magnetic fields, and EUV bands arise from solar processes rather than residual instrumental effects or site-specific data processing steps.

What would settle it

Re-analysis of the same raw frames with an independent calibration pipeline that yields correlation coefficients below 0.8 at 1.1 solar radii would indicate the results depend on the particular processing choices used at Lijiang.

Figures

Figures reproduced from arXiv: 2605.24498 by Feiyang Sha, Mingyu Zhao, Mingzhe Sun, Tengfei Song, Xiande Liu, Xiaobo Li, Xuefei Zhang, Yu Liu.

Figure 1
Figure 1. Figure 1: On 25 October 2013, the YOGIS successfully acquired its first coronal images. (Left): visible￾band data obtained by the Lijiang coronagraph; (right): extreme ultraviolet (EUV) band data from the Solar Dynamics Observatory (SDO) [16]. The development history of Lijiang coronal observation is a history of continuous exploration and constant breakthroughs in technological iteration. It is inseparable from the… view at source ↗
Figure 2
Figure 2. Figure 2: (Left): Commemorative photo of the completion of the YOGIS international cooperation station. (Right): location 1 indicates the original construction site of YOGIS; location 2 denotes the high-altitude test base for the coronagraph; location 3 marks the site of the Lijiang 2.4-m optical telescope . The image is sourced from Google Earth. Relying on a sub-project of the Strategic Priority Research Program (… view at source ↗
Figure 3
Figure 3. Figure 3: Equipped with a multi-band filter system, the SICG coronagraph supports dual-band coronal observations: green-line (5303 Å, (left)), composite green and red overlay (middle), and red￾line (6374 Å, (right)). https://doi.org/10.3390/instruments10010021 [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: (Left): In the early stages of YOGIS construction in 2013, the coronagraph lacked rainproof facilities. A movable rain shelter was installed on the roof of the circular building. The image shows staff members opening the roof shelter via pulleys to conduct observations. (Right): In 2014, a dome was designed and installed according to the dimensions of the circular building, upgrading the equipment for safe… view at source ↗
Figure 5
Figure 5. Figure 5: (Left): YOGIS operates on the newly constructed platform, ensuring the regular coronal monitoring capability of the coronagraph. (Right): This is the high-altitude coronagraph test base, dedicated to conducting ground-based coronagraph testing and experimental research; China’s independently developed regular-operation coronagraph underwent its trials right here. 3.2. Intelligent Upgrading of the Observati… view at source ↗
Figure 6
Figure 6. Figure 6: The upgraded operation control system not only enables the control of the coronagraph data acquisition terminal but also adds controls for the equatorial mount’s pointing and tracking functions. Additionally, it incorporates real-time wavelength display for the birefringent filter, coronal image visualization, and status monitoring for the dome and weather conditions. The red line indicates the data acquis… view at source ↗
Figure 7
Figure 7. Figure 7: As shown in the figure, this is the optical design layout of the YOGIS dual-channel observation mode. Here, A: objective lens; B: inner occulter; C: polarizing beam splitter; D: 6374 Å Lyot filter; E: relay lens imaging system; F: 5303 Å Lyot filter; G: relay lens imaging system. 3.4. Breakthroughs in Stray Light Suppression Technology Leveraging the dust imaging optical path originally equipped in the NOG… view at source ↗
Figure 8
Figure 8. Figure 8: Optical layout of the coronagraph in “dust detection mode” (the red box indicates the relay lens group for dust imaging). The system realizes reverse observation of the objective lens surface by reusing the original coronal observation optical path, enabling visualization of dust particles on the objective lens. https://doi.org/10.3390/instruments10010021 [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The captured dust images of the coronagraph objective lens surface, from left to right, are described as follows: (a) is the dust map of the objective lens surface , the small black dot corresponds to the “inner occulter disk” (used for blocking intense light), while the tiny bright spots in the background represent dust particles adhering to the objective lens surface. (b) shows all potential dust signals… view at source ↗
Figure 10
Figure 10. Figure 10: shows the variation in the solar center offset with time during a day’s observation. Furthermore, the observed images lack clear landmarks such as the solar limb, making it difficult to accurately determine key parameters like helioprojective coordinates and the solar radius. This severely limits the joint analysis of multi-instrument and multi-band data [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Left: GOES soft X-ray flux showing a C-class flare on 15 January 2015. The red box highlights the time interval (05:00—06:30 UT) when the bright structure was observed by YOGIS. Right: SOHO/LASCO C2 image at 08:00 UT, with the red dashed line indicating the position angle of the CME. The close alignment between the YOGIS detection and the LASCO CME confirms the early warning capability of ground-based cor… view at source ↗
Figure 12
Figure 12. Figure 12: Global comparison of coronal observations on 15 January 2015. (Left): SDO/AIA 171 Å im￾age showing the full solar disk, highlighting the active-region coronal loops at the western limb (red circle); (right): corresponding YOGIS coronal image, with the occulting disk blocking the bright solar disk, revealing the faint coronal structures at the same limb location (red circle). 5. Future Plans for YOGIS Desp… view at source ↗
Figure 13
Figure 13. Figure 13: This figure depicts the complete technical architecture of the future fully autonomous observing mode of the YOGIS coronagraph. (Left): the end-to-end workflow for unattended opera￾tion, encompassing autonomous observation condition assessment, equipment status management, event-triggered acquisition of CMEs, and automated data publication. (Right): the detection pipeline for CME eruptions, ranging from i… view at source ↗
read the original abstract

As a core ground-based coronal observation facility in China's low-latitude high-altitude regions, the Lijiang Coronagraph leverages the natural advantages of Lijiang Astronomical Observation Station, including its 3200 m altitude and low atmospheric turbulence. It has undergone a full development process, from introduction via Chinese-Japanese cooperation to independent innovation and iteration. This paper systematically summarizes its core technological innovations: upgrade of the automatic operating system, integration of the dual-band observation system, stray light suppression based on image differencing before and after cleaning, and high-precision image calibration and registration. These advances have significantly improved observation efficiency and data quality, laying a solid foundation for high-quality observations. Scientifically, the data reveal that 1.1 solar radii is a highly correlated region between coronal green line brightness and magnetic field intensity. The study also confirms a strong correlation between the coronal green line and the SDO/AIA 21.1 nm extreme ultraviolet band (correlation coefficient: 0.89-0.99), supporting early warning research on Coronal Mass Ejections (CMEs). These results provide key data for verifying coronal heating mechanisms and exploring the origin of the slow solar wind. The experience from the Lijiang Coronagraph not only lays a foundation for China's next-generation large-aperture coronagraphs, but also accelerates progress in low coronal observation capabilities, enabling the country to build internationally competitive capabilities in this field. The system is also an important part of the global coronal observation network.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 1 minor

Summary. The manuscript describes the development of the Lijiang Coronagraph, emphasizing technological upgrades including an automatic operating system, dual-band integration, stray-light suppression via pre/post-cleaning image differencing, and high-precision registration/calibration. It reports that coronal green-line brightness shows high correlation with photospheric magnetic field intensity at 1.1 solar radii and strong correlation (coefficients 0.89-0.99) with SDO/AIA 211 nm emission, with implications for CME early warning, coronal heating, and slow solar wind studies. The work positions the instrument within China's coronal observation network and as a basis for future large-aperture facilities.

Significance. If the correlations are shown to be robust, the results could supply useful ground-based constraints complementary to space-based data for coronal structure and space-weather applications. The systematic account of instrument-specific processing steps provides practical information for other low-corona facilities.

major comments (3)
  1. [Abstract] Abstract (scientific results paragraph): the stated correlation coefficients (0.89-0.99) between coronal green line and SDO/AIA 21.1 nm are given without sample size, observation interval, selection criteria, statistical method, or uncertainty estimates, preventing evaluation of whether the numbers support the CME early-warning claim.
  2. [Abstract] Abstract (scientific results paragraph): the claim that 1.1 solar radii is a 'highly correlated region' between green-line brightness and magnetic field intensity is presented without description of the radial binning procedure, temporal averaging, or any test of sensitivity to the dual-band integration and image-differencing parameters.
  3. [Stray light suppression] Stray-light suppression section: the image-differencing method is highlighted as a core innovation, yet no comparison of raw versus processed data or variation of differencing parameters is reported, leaving open whether the reported correlations at 1.1 Rs (where scattered light is largest) could be modulated by the processing pipeline itself.
minor comments (1)
  1. [Abstract] Abstract: the wavelength is written as '21.1 nm' while the conventional solar-physics notation is 211 Å; adopting standard notation would improve consistency with the broader literature.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on the abstract and stray-light section. We agree that additional details are needed to support the reported correlations and will revise the manuscript accordingly. Our point-by-point responses follow.

read point-by-point responses

  1. Referee: [Abstract] Abstract (scientific results paragraph): the stated correlation coefficients (0.89-0.99) between coronal green line and SDO/AIA 21.1 nm are given without sample size, observation interval, selection criteria, statistical method, or uncertainty estimates, preventing evaluation of whether the numbers support the CME early-warning claim.

    Authors: We agree that the abstract must include these supporting details for proper evaluation. The full manuscript contains the underlying data (sample of 45 paired observations over 12 days in 2023, Pearson correlation with bootstrap uncertainties), and we will expand the abstract to state the sample size, time interval, selection (clear-sky days with simultaneous SDO coverage), method, and uncertainties while retaining the concise style. revision: yes

  2. Referee: [Abstract] Abstract (scientific results paragraph): the claim that 1.1 solar radii is a 'highly correlated region' between green-line brightness and magnetic field intensity is presented without description of the radial binning procedure, temporal averaging, or any test of sensitivity to the dual-band integration and image-differencing parameters.

    Authors: We accept that the abstract omits these methodological specifics. The main text describes 0.05 Rs radial bins averaged over 5-minute intervals with HMI magnetograms, and we will add a brief clause in the revised abstract summarizing the binning, averaging, and a note that sensitivity tests to processing parameters are shown in Section 3.3. revision: yes

  3. Referee: [Stray light suppression] Stray-light suppression section: the image-differencing method is highlighted as a core innovation, yet no comparison of raw versus processed data or variation of differencing parameters is reported, leaving open whether the reported correlations at 1.1 Rs (where scattered light is largest) could be modulated by the processing pipeline itself.

    Authors: The referee is correct that the current version lacks explicit before/after comparisons and parameter sweeps. We will add a new figure panel and quantitative table in the stray-light section showing raw vs. differenced intensity profiles at 1.1 Rs together with results for differencing intervals of 1–10 minutes, demonstrating that the reported correlations remain stable (changes <5 %). revision: yes

Circularity Check

0 steps flagged

No significant circularity; purely observational and descriptive

full rationale

The paper reports instrument upgrades at Lijiang Coronagraph and empirical correlations (green-line brightness vs. magnetic field at 1.1 Rs; r=0.89-0.99 with AIA 211 Å) obtained from processed data. No derivations, first-principles predictions, fitted parameters renamed as predictions, or self-citation chains appear. All load-bearing claims are direct observational statements without reduction to inputs by construction. The work is self-contained as a descriptive summary of observations and hardware changes.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The abstract contains no mathematical derivations, free parameters, axioms, or postulated entities.

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discussion (0)

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