Formation of an Intermediate Filament Driven by Small-scale Magnetic Reconnection

Sun, Xia; Yan, Xiaoli; Liang, Hong-Fei; Xue, Zhike; Wang, Jincheng; Yang, Liheng; Xu, Zhe; Yang, Liping; Peng, Yang; Li, Qiaoling; li, Zihan; Zhang, Xinsheng

doi:10.3847/1538-4357/acaa3e

Cited by 3 publications

(2 citation statements)

References 62 publications

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“…In particular, OR has become one of the leading contenders for the origin of quasi-periodic pulsations from solar flares (McLaughlin et al 2018;Zimovets et al 2021;Kou et al 2022). OR has also become a potential theoretical explanation for the origin of other periodic solar phenomena, including periodicities within solar jets (Hong et al 2019), quasi-periodic flows (McLaughlin et al 2012), periodicities within Type III radio bursts (Cattell et al 2021), filament formation (Sun et al 2023), flux rope formation and disappearance (Xue et al 2019), stellar flare oscillations (Doyle et al 2018), and a possible explanation for spikes and switchbacks observed by the Parker Solar Probe (He et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The Effect of Resistivity on the Periodicity of Oscillatory Reconnection

Talbot,

McLaughlin,

Botha

et al. 2024

ApJ

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The oscillatory reconnection mechanism is investigated for a parameter study of eight orders of magnitude of resistivity, with a particular interest in the evolution of the oscillating current density at the null point and its associated periodicity. The resistive, nonlinear MHD simulations are solved in 2.5D for different levels of resistivity. Three methods (wavelet analysis, Fourier transform, and ANOVA) are used to investigate the effect of resistivity versus resultant period. It is found that there is an independence between the level of background resistivity and the period of the oscillatory reconnection mechanism. Conversely, it is found that resistivity has a significant effect on the maximum amplitude of the current density and the nature of its decay rate, as well as the magnitude of ohmic heating at the null.

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Section: Introductionmentioning

confidence: 99%

The Effect of Resistivity on the Periodicity of Oscillatory Reconnection

Talbot,

McLaughlin,

Botha

et al. 2024

ApJ

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“…During its years of operation, the NVST has accumulated over 2 petabytes of observational data. This facilitates research on solar observations, for example, for recording the formation of intermediate filaments (Sun et al 2023b), wave trains accompanying solar flares (Zhou et al 2022), and evolution of anti-Hale regions (Xu et al 2022b). Nevertheless, the continually growing data set poses significant challenges to data management, particularly in the area of data retrieval.…”

Section: Introductionmentioning

confidence: 99%

AstroSer: Leveraging Deep Learning for Efficient Content-based Retrieval in Massive Solar-observation Images

Wu,

Liu,

Yang

et al. 2023

PASP

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Rapid and proficient data retrieval is an essential component of modern astronomical research. In this paper, we address the challenge of retrieving astronomical image content by leveraging state-of-the-art deep learning techniques. We have designed a retrieval model, HybridVR, that integrates the capabilities of the deep learning models ResNet50 and VGG16 and have used it to extract key features of solar activity and solar environmental characteristics from observed images. This model enables efficient image matching and allows for content-based image retrieval (CBIR). Experimental results demonstrate that the model can achieve up to 98% similarity during CBIR while exhibiting adaptability and scalability. Our work has implications for astronomical research, data management, and education, and it can contribute to optimizing the utilization of astronomical image data. It also serves as a useful example of the application of deep learning technology in the field of astronomy.

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Preliminary Discussion on the Current Sheet

Ding,

Zhang,

Fang

et al. 2024

ApJ

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The current sheet is a characteristic structure of magnetic energy dissipation during the magnetic reconnection process. So far, the width and depth of the current sheet are still indefinite. Here we investigate 64 current sheets observed by four telescopes from 1999 to 2022, and all of them have been well identified in the previous literature. In each current sheet, three width values are obtained at the quartering points. Based on these investigated cases, we obtain 192 values, which are in a wide range from hundreds to tens of thousands of kilometers. By calculating the pixel width (PW: the ratio of the current sheet width to the pixel resolution of corresponding observed data) of these current sheets, we find that more than 80% of the PW values concentrate on 2–4 pixels, indicating that the widths of the current sheets are dependent strongly on the instrument resolutions and all the sheets have no observable three-dimensional information. To interpret this result, we suggest that there are two probabilities. One is that the width of the current sheet is smaller than the instrument resolution, and the other is that the detected current sheet is only a small segment of the real one. Furthermore, there is another possible scenario. The so-called current sheet is just an emission-enhanced region.

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Formation of an Intermediate Filament Driven by Small-scale Magnetic Reconnection

Cited by 3 publications

References 62 publications

The Effect of Resistivity on the Periodicity of Oscillatory Reconnection

The Effect of Resistivity on the Periodicity of Oscillatory Reconnection

AstroSer: Leveraging Deep Learning for Efficient Content-based Retrieval in Massive Solar-observation Images

Preliminary Discussion on the Current Sheet

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