[논문]A STUDY OF SMALL FLARES ASSOCIATED WITH PLASMA BLOBS OUTFLOWING ALONG POST-CME RAYS

Kim, Yoo Jung; Kwon, Ryun-Young; Chae, Jongchul

doi:10.5303/jkas.2020.53.1.1

A STUDY OF SMALL FLARES ASSOCIATED WITH PLASMA BLOBS OUTFLOWING ALONG POST-CME RAYS 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.1, 2020년, pp.1 - 7

Kim, Yoo Jung (Department of Physics and Astronomy, Seoul National University) , Kwon, Ryun-Young (Solar and Space Weather Group, Korea Astronomy and Space Science Institute) , Chae, Jongchul (Department of Physics and Astronomy, Seoul National University)

Abstract ▼ AI-Helper

The recent study of Chae et al. (2017) found a one-to-one correspondence between plasma blobs outflowing along a ray formed after a coronal mass ejection (CME) and small X-ray flares. In the present work, we have examined the spatial configuration and the eruption process of the flares that are associated with the blobs by analyzing EUV images and magnetograms taken by the SDO/AIA and HMI. We found that the main flare and the successive small flares took place in a quadrupolar magnetic configuration characterized by predominant magnetic fields of positive polarity, two minor magnetic fragments of negative polarity, and a curved polarity inversion line between them, which suggests that the formation process of the blobs may be similar to that of the parent CME. We also found that the successive flares resulted in a gradual change of the quadrupolar magnetic configuration, and the relevant migration of flaring kernels. The three-dimensional geometry and the property of the current sheet, that is often supposed to be embedded in an observed post-CME ray, seem to keep changing because of mutual feedback between the successive flares and the temporal change of the magnetic field configuration. Our results suggest that the observed post-CME rays may not reflect the characteristics of the current sheet responsible for the impulsive phase of the flare.

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표/그림 (5)

표 Table 1 Features identified from the coronagraph observations and the EUV flares.
그림 Figure 1. Left: The AIA 131Å image of AR11850 taken on September 21, 2013 at the time of the main flare. The diamond marks the location of the flare associated with feature 4. Center: Magnied view of the region where the main flare occurred. Right: SDO/HMI line-of-sight magnetogram of the same region.
그림 Figure 2. Upper eight images: SDO/HMI magnetograms at different epochs during the main flare. Lower eight images: AIA 131Å images and AIA 1600Å contours (in red) at the same epochs. Bottom diagram: The EUV light curves for the two wavelengths.
그림 Figure 3. Left: Magnetograms and EUV images of subflares 1 to 3 at different epochs. Right: EUV light curves of the same flares.
그림 Figure 4. Same as Figure 3, but for subflares 4 to 6.

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In this study, we investigate the development and magnetic configuration of the main flare and the subsequent small flares that are associated with the CME and the blobs studied by Chae et al. (2017), by examining the EUV images and magnetograms. This investigation allows us to correlate the blobs and outflows in the high corona region with the processes in the low corona region not only temporally but also spatially.
2010). These studies showed the existence of structures like current sheets, cusp-shaped flare loops, and plasma inflows. However, no clear connection has been made yet between such phenomena in the low corona, and blobs observed in the high corona with coronagraphs.
(2016). They studied two CMEs associated with two successive C-class flares observed on 21 September 2013 that were followed by several rays on the COR2 image of the STEREO Behind. It was found that the major ray was coaxial with the CME as expected, and had a cross section of 0.
(2017), by examining the EUV images and magnetograms. This investigation allows us to correlate the blobs and outflows in the high corona region with the processes in the low corona region not only temporally but also spatially. Previously, there have been several studies of the low region of the current sheet (formed after CME) by observing in EUV or X-ray wavelengths (Forbes & Acton 1996; Lin et al.

참고문헌 (18)

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DOI : 10.5303/JKAS.2020.53.1.1 [무료]
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