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345 results on '"Li, You-ping"'

1. Correction to: Association Between a Failed Prominence Eruption and the Drainage of Mass from Another Prominence

Author

Xue, Jian-chao, Feng, Li, Li, Hui, Zhang, Ping, Chen, Jun, Shi, Guang-lu, Ji, Kai-fan, Qiu, Ye, Li, Chuan, Lu, Lei, Ying, Bei-li, Li, Ying, Huang, Yu, Li, You-ping, Li, Jing-wei, Zhao, Jie, Song, De-chao, Li, Shu-ting, Tian, Zheng-yuan, Su, Ying-na, Zhang, Qing-min, Ge, Yun-yi, Shan, Jia-hui, Li, Qiao, Li, Gen, Zhou, Yue, Tian, Jun, Liu, Xiao-feng, Jing, Zhi-chen, Chen, Bo, Song, Ke-fei, He, Ling-ping, Lei, Shi-jun, and Gan, Wei-qun

Published
2024
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2. Association Between a Failed Prominence Eruption and the Drainage of Mass from Another Prominence

Author

Xue, Jian-chao, Feng, Li, Li, Hui, Zhang, Ping, Chen, Jun, Shi, Guang-lu, Ji, Kai-fan, Qiu, Ye, Li, Chuan, Lu, Lei, Ying, Bei-li, Li, Ying, Huang, Yu, Li, You-ping, Li, Jing-wei, Zhao, Jie, Song, De-chao, Li, Shu-ting, Tian, Zheng-yuan, Su, Ying-na, Zhang, Qing-min, Ge, Yun-yi, Shan, Jia-hui, Li, Qiao, Li, Gen, Zhou, Yue, Tian, Jun, Liu, Xiao-feng, Jing, Zhi-chen, Chen, Bo, Song, Ke-fei, He, Ling-ping, Lei, Shi-jun, and Gan, Wei-qun

Published
2024
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6. On the Power-Law Distributions of X-ray Fluxes from Solar Flares Observed with GOES

Author

Li, You-ping, Feng, Li, Zhang, Ping, Liu, Siming, and Gan, Weiqun

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Power-law frequency distributions of the peak flux of solar flare X-ray emission have been studied extensively and attributed to a system of self-organized criticality (SOC). In this paper, we first show that, so long as the shape of the normalized light curve is not correlated with the peak flux, the flux histogram of solar flares also follows a power-law distribution with the same spectral index as the power-law frequency distribution of the peak flux, which may partially explain why power-law distributions are ubiquitous in the Universe. We then show that the spectral indexes of the histograms of soft X-ray fluxes observed by GOES satellites in two different energy channels are different: the higher energy channel has a harder distribution than the lower energy channel, which challenges the universal power-law distribution predicted by SOC models and implies a very soft distribution of thermal energy content of plasmas probed by the GOES. The temperature ($T$) distribution, on the other hand, approaches a power-law distribution with an index of 2 for high values of $T$. Application of SOC models to statistical properties of solar flares needs to be revisited., Comment: 6 figures, to appear on RAA

Published
2016
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14. Statistical Studies on Modified Neupert Effect

Author

YU Wen-hui, Gan Wei-qun, and LI You-ping

Subjects
Physics, High energy, Solar flare, 010308 nuclear & particles physics, Bremsstrahlung, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Loop length, law.invention, Pulse (physics), Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, Chromosphere, Microwave, Flare
Abstract

The qualitative description of the Neupert effect is that there is a causal relationship between the pulse component (hard X-ray, microwave burst) and the gradual component (soft X-ray emission) in a flare. The initial energy of the flare is released in the form of accelerating particles. The energetic particles produce HXR (hard X-ray) via nonthermal electron-ion bremsstrahlung as they lose their energies in the chromosphere. The SXR (soft X-ray) emission of the flare is the response of energetic particles injected into the chromosphere. According to the quantitative description of the classic Neupert effect, SXR should reach maximum instantly at the end of HXR emission (sign of nonthermal electron injection). However, previous observations have found that for quite a number of flares the SXR peak time ( t 2 ) is significantly later than the end time of HXR ( t 1 ) ( τ = t 2 − t 1 , τ > 0 ), deviating from the classic Neupert effect. In order to study the events deviating from the classic Neupert effect or not, we checked the RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) and GOES (Geostationary Operational Environmental Satellites) events list from 2002 to 2015, and found out flare samples that have simple lightcurves at 25–50 keV together with other criteria. A total of 276 flare samples were finally selected. We have analysed the τ distribution of these flares, as well as the relationship between the loop length (represented by the distance between two footpoint sources d ) and τ . We found that: (1) 227 sample flares present τ > 0 , which means that about 82% of total samples deviate from the classical Neupert effect; (2) there is a roughly linear correlation between τ and d , that is, the longer the loop is, the later the maximum time of SXR with respect to the end of HXR; (3) there seems to have a critical distance, within which the classic Neupert effect works. These results confirm the necessity of modifying Neupert effect, and expound its physical significance.

Published
2021

16. In-flight Low Energy X-ray Calibration of POLAR Detector on TianGong2

Author

Hajdas Wojtek, Chen Wei, Su Yang, LI You-ping, Zhang Ping, and Liu Si-ming

Subjects
Physics, Photon, Solar flare, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Linear polarization, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astronomy and Astrophysics, Polarimeter, Scintillator, 01 natural sciences, Optics, Space and Planetary Science, 0103 physical sciences, Calibration, Polar, business, 010303 astronomy & astrophysics
Abstract

POLAR is a γ -ray burst polarimeter on board the TianGong2 space lab, which was launched into a near earth orbit in 2016 September 15. It is designed to measure the linear polarization of hard X-ray in the 50–500 keV energy range. The detector has 25 modules, and each module has 64 plastic scintillator bars. With a total number of 1600 plastic scintillator bars, POLAR has a very large effective detection area and field of view. During its on-orbit operation, POLAR has detected multiple small flares. Their hard X-ray photon energies are usually less than 50 keV, and can not be analyzed directly by using the on-orbit and ground-based high-energy calibration results. By combining the RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) observation of the flare SOL2016112907 with the Monte Carlo simulation, this paper calibrates the response of POLAR in the energy band lower than 50 keV. We find that the energy threshold ( ∼ 10 keV) and conversion factor obtained by calibration are relatively stable, but they are quite different from the values obtained via calibration in the high-energy range, and that the differences for the different scintillator bars have no evident regularity.

Published
2020

32. Simulations and software development for the Hard X-ray Imager onboard ASO-S

Author

Su, Yang, primary, Liu, Wei, additional, Li, You-Ping, additional, Zhang, Zhe, additional, Hurford, Gordon J., additional, Chen, Wei, additional, Huang, Yu, additional, Li, Zhen-Tong, additional, Jiang, Xian-Kai, additional, Wang, Hao-Xiang, additional, Xia, Fan-Xiao-Yu, additional, Chen, Chang-Xue, additional, Yu, Wen-Hui, additional, Yu, Fu, additional, Wu, Jian, additional, and Gan, Wei-Qun, additional

Published
2019
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33. Advanced Space-based Solar Observatory (ASO-S): an overview

Author

Gan, Wei-Qun, primary, Zhu, Cheng, additional, Deng, Yuan-Yong, additional, Li, Hui, additional, Su, Yang, additional, Zhang, Hai-Ying, additional, Chen, Bo, additional, Zhang, Zhe, additional, Wu, Jian, additional, Deng, Lei, additional, Huang, Yu, additional, Yang, Jian-Feng, additional, Cui, Ji-Jun, additional, Chang, Jin, additional, Wang, Chi, additional, Wu, Ji, additional, Yin, Zeng-Shan, additional, Chen, Wen, additional, Fang, Cheng, additional, Yan, Yi-Hua, additional, Lin, Jun, additional, Xiong, Wei-Ming, additional, Chen, Bin, additional, Bao, Hai-Chao, additional, Cao, Cai-Xia, additional, Bai, Yan-Ping, additional, Wang, Tao, additional, Chen, Bing-Long, additional, Li, Xin-Yu, additional, Zhang, Ye, additional, Feng, Li, additional, Su, Jiang-Tao, additional, Li, Ying, additional, Chen, Wei, additional, Li, You-Ping, additional, Su, Ying-Na, additional, Wu, Hai-Yan, additional, Gu, Mei, additional, Huang, Lei, additional, and Tang, Xue-Jun, additional

Published
2019
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34. The Science Operations and Data Center (SODC) of the ASO-S mission

Author

Huang, Yu, primary, Li, Hui, additional, Gan, Wei-Qun, additional, Li, You-Ping, additional, Su, Jiang-Tao, additional, Deng, Yuan-Yong, additional, Feng, Li, additional, Su, Yang, additional, Chen, Wei, additional, Lei, Shi-Jun, additional, Li, Ying, additional, Ge, Yun-Yi, additional, Su, Ying-Na, additional, Liu, Si-Ming, additional, Zang, Jing-Jing, additional, Xu, Zun-Lei, additional, Bai, Xian-Yong, additional, and Li, Jing-Wei, additional

Published
2019
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46. Monitoring and research of high-energy solar flare emissions with GECAM

Author

Su Yang, Zhu Yue, Gan Wei-qun, Xiong Shao-Lin, LI You-ping, Peng Wen-Xi, and Chen Wei

Subjects
Explosive material, Solar flare, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, NASA Deep Space Network, Space weather, Light curve, Solar physics, law.invention, law, Physics::Space Physics, Environmental science, Flare
Abstract

The dual-satellite GECAM (Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor) project was developed by China for monitoring high-energy astrophysical phenomena. The expected launch date of GECAM is the end of 2020. The main scientific objectives are to observe high-energy emissions from gravitational wave events, gamma-ray bursts, and other explosive energy releases in deep space. Among the most important objectives is monitoring the high-energy events in the solar-terrestrial system. GECAM has a conjugated dual-satellite configuration, with 25 wide-angle gamma-ray detectors (6 keV$-$5 MeV) installed on each platform. With this configuration, GECAM can perform nearly all-sky and full-time observations, and is ideally suited to the monitoring of X-ray and gamma-ray bursts in solar flares. This paper first introduces the background and current status of research on high-energy flare emissions, including the major scientific questions in high-energy solar physics, general features of high-energy flare emissions, as well as research on solar X-ray bursts and Gamma-ray bursts. We focus on analysis of light curves and spectra, and also discuss the important research prospects of GECAM solar data in solar physics.

Published
2020

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