[논문]TOWARD A NEXT GENERATION SOLAR CORONAGRAPH: DIAGNOSTIC CORONAGRAPH EXPERIMENT

Cho, Kyung-Suk; Yang, Heesu; Lee, Jae-Ok; Bong, Su-Chan; Kim, Jihun; Choi, Seonghwan; Park, Jongyeob; Cho, Kyuhyoun; Baek, Ji-Hye; Kim, Yeon-Han; Park, Young-Deuk

doi:10.5303/jkas.2020.53.4.87

[국내논문] TOWARD A NEXT GENERATION SOLAR CORONAGRAPH: DIAGNOSTIC CORONAGRAPH EXPERIMENT 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.4, 2020년, pp.87 - 98

Cho, Kyung-Suk (Korea Astronomy and Space Science Institute) , Yang, Heesu (Korea Astronomy and Space Science Institute) , Lee, Jae-Ok (Korea Astronomy and Space Science Institute) , Bong, Su-Chan (Korea Astronomy and Space Science Institute) , Kim, Jihun (Korea Astronomy and Space Science Institute) , Choi, Seonghwan (Korea Astronomy and Space Science Institute) , Park, Jongyeob (Korea Astronomy and Space Science Institute) , Cho, Kyuhyoun (Astronomy Program, Department of Physics and Astronomy, Seoul National University) , Baek, Ji-Hye (Korea Astronomy and Space Science Institute) , Kim, Yeon-Han (Korea Astronomy and Space Science Institute) , Park, Young-Deuk (Korea Astronomy and Space Science Institute)

Abstract ▼ AI-Helper

The Korea Astronomy and Space Science Institute (KASI) has been developing a next-generation coronagraph (NGC) in cooperation with NASA to measure the coronal electron density, temperature, and speed simultaneously, using four different optical filters around 400 nm. KASI organized an expedition to demonstrate the coronagraph measurement scheme and the instrumental technology during the 2017 total solar eclipse (TSE) across the USA. The observation site was in Jackson Hole, Wyoming, USA. We built an eclipse observation system, the Diagnostic Coronal Experiment (DICE), composed of two identical telescopes to improve the signal-to-noise ratio. The observation was conducted at four wavelengths and three linear polarization directions in the limited total eclipse time of about 140 seconds. We successfully obtained polarization data for the corona but we were not able to obtain information on the coronal electron temperature and speed due to the low signal-to-noise ratio of the optical system and strong emission from prominences located at the western limb. In this study, we report the development of DICE and the observation results from the eclipse expedition. TSE observation and analysis with our self-developed instrument showed that a coronagraph needs to be designed carefully to achieve its scientific purpose. We gained valuable experience for future follow-up NASA-KASI joint missions: the Balloon-borne Investigation of the Temperature and Speed of Electrons in the Corona (BITSE) and the COronal Diagnostic EXperiment (CODEX).

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표/그림 (18)

그림 Figure 1. Layout of a single DICE (top panel) and two DICEs mounted on a tracking system (bottom panel).
그림 Figure 2. Optical layout of the DICE.
표 Table 1 Design requirements for the DICE optical system
그림 Figure 3. Spot diagram for different wavelengths (0.385, 0.395, and 0.41 μm).
그림 Figure 4. Ghost analysis before (upper) and after (lower) AR-coating on the polarization filter.
그림 Figure 5. Filter and polarizer units.
그림 Figure 6. Result of the polarizer angle accuracy test.
표 Figure 7. DICE control system.
표 Table 2 Times of total solar eclipse phases and corresponding Sun positions at the observation site
그림 Figure 8. Measured and simulated optical perfor-mance of lens, bandpass lters, and CCD includ-ing the coronal irradiance (I_cor) at 1:2R⊙ assuming an electron temperature of 10⁶ K and a solar wind speed of 400 km/s.
그림 Figure 9. Calculated uncertainty range of the filter ratio.
그림 Figure 10. Relationship between filter ratio and K-coronal temperature.
표 Table 3 Observation sequence of the DICE
그림 Figure 11. Simulated scatter of measured temperatures as function of number of stacked images, after 3×3 pixel binning.
그림 Figure 12. Images of the TSE.
그림 Figure 13. (a) Polarized brightness at 402.5 nm by DICE, (b) at 393.4 nm by DICE, and (c) at 735 nm by K-Cor. (d) Total brightness (tB), (e) degree of linear polarization (pD), and (f) linear polarization angle (pA) at 402.5 nm.
그림 Figure 14. (a) Ratio of the total intensity images obtained at 402.5 nm and 393.4 nm, used for determining the temperature. (b) Distribution of the ratio in the range R = 1.15 − 1.25R_⊙.
그림 Figure 15. Left: Coronal continuum intensity image. Right: Electron temperature map, overlaid on the intensity image.

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