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Where do flare ribbons stop?

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Chinese Science Bulletin 2012年第12期57卷 1393-1396页

作者： CHEN PengFei SU JiangTao GUO Yan deng yuanyong Department of Astronomy Nanjing University Nanjing 210093 China Key Laboratory of Solar Physics National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China

The standard flare model,which was proposed based on observations and magnetohydrodynamic theory,can successfully explain many observational features of solar ***,this model is just a framework,with many details awaiting to be filled in, including how reconnection is *** this paper,we address an unanswered question:where do flare ribbons stop?With the data analysis of the 2003 May 29 flare event,we tentatively confirmed our conjecture that flare ribbons finally stop at the intersection of separatrices(or quasi-separatrix layer in a general case)with the solar *** verified,such a conjecture can be used to predict the final size and even the lifetime of solar flares.

关键词：太阳耀斑丝带数据分析太阳表面界线层

Algorithm Development of Cloud Removal from Solar Images Based on Pix2Pix Network

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Computers, Materials & Continua 2022年第5期71卷 3497-3512页

作者： Xian Wu Wei Song Xukun Zhang Ganghua Lin Haimin Wang yuanyong deng School of Information Engineering Minzu University of ChinaBeijing100081China Key Laboratory of Solar Activity Chinese Academy of Sciences(KLSACAS)Beijing100101China National Language Resource Monitoring and Research Center of Minority Languages Minzu University of ChinaBeijing100081China National Astronomical Observatories Chinese Academy of Sciences(NAOCCAS)Beijing100101China Center for Solar-Terrestrial Research New Jersey Institute of TechnologyUniversity HeightsNewark07102-1982USA Institute for Space Weather Sciences New Jersey Institute of TechnologyUniversity HeightsNewark07102-1982USA Big Bear Solar Observatory New Jersey Institute of Technology40386North Shore LaneBig Bear City92314-9672USA

Sky clouds affect solar observations *** shadows obscure the details of solar features in observed ***-covered solar images are difficult to be used for further research without *** this paper,the solar image cloud removing problem is converted to an image-to-image translation problem,with a used algorithm of the Pixel to Pixel Network(Pix2Pix),which generates a cloudless solar image without relying on the physical scattering ***2Pix is consists of a generator and a *** generator is a well-designed *** discriminator uses PatchGAN structure to improve the details of the generated solar image,which guides the generator to create a pseudo realistic solar *** image generation model and the training process are optimized,and the generator is jointly trained with the *** the generation model which can stably generate cloudless solar image is *** experiment results on Huairou Solar Observing Station,National Astronomical Observatories,and Chinese Academy of Sciences(HSOS,NAOC and CAS)datasets show that Pix2Pix is superior to the traditional methods based on physical prior knowledge in peak signal-to-noise ratio,structural similarity,perceptual index,and subjective visual *** result of the PSNR,SSIM and PI are 27.2121 dB,0.8601 and 3.3341.

关键词： Pix2Pix solar image cloud removal

Near infrared spectral and polarization imaging observation of coronal emission lines during the 2008 total solar eclipse

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Science China(Physics,Mechanics & Astronomy) 2009年第11期52卷 1794-1798页

作者： BAO XingMing ZHANG ZhiYong deng Jian HU KeLiang XUAN WeiJia LIU YangBing ZHANG HongQi deng yuanyong WANG DongGuang WANG XiaoFan Key Laboratory of Solar Activity National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100012China

During the 2008 total solar eclipse, the coronal emission lines were observed by using optical fibre spectrometric and polarization imaging system in near infrared waveband. The profiles of the coronal emission lines including Fe XIII 10747 , 10798  and He I 10830  were obtained with dispersion of 0.5 /pix. The intensity of Fe XIII 10747  remained unchanged in the two different coronal regions while the intensity of He I 10830  varied considerably in the two coronal locations no matter whether the prominence appeared or not. The coronal polarization images were observed at Fe XI 7892  with a bandpass of 30  in a series of exposure times.

关键词： solar corona total solar eclipse coronal emission line polarization near infrared

Solar Observation with the Fourier Transform *** Results of Solar Spectrum near the CO 4.66μm and Mg I 12.32μm

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Research in Astronomy and Astrophysics 2023年第12期23卷 128-137页

作者： Xianyong Bai Zhiwei Feng Zhiyong Zhang yuanyong deng Xiaoming Zhu Kaifan Ji Song Feng Xiao Yang Yongliang Song National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 101408China Yunnan Observatories Chinese Academy of SciencesKunming 650011China Faculty of Information Engineering and Automation/Yunnan Key Laboratory of Computer Technology Application Kunming University of Science and TechnologyKunming 650500China

An infrared solar spectrum observed by ground-based telescopes is seriously affected by the background radiation both from the telescope and sky,relative to the visible *** accuracy is also influenced by the spectral resolution of the Fourier transform *** the paper,we developed a CO_(2)gas cell and installed it in the sample compartment to calibrate the spectral resolution of the Bruker IFS-125HR at infrared *** measured spectral resolution is 0.00342±0.00086 cm^(-1)and 0.0059±0.00024 cm^(-1)at the wavenumbers of798 cm^(-1)and 2136 cm^(-1),*** also updated a fully reflective sunlight feeding system to observe the solar spectrum near CO 4.66μm and Mg I 12.32μ*** quickly pointing the sunlight feeding system about1 degree away from the solar disk center,we are able to measure the background radiation from the telescope and the sky at Huairou Solar Observing *** removing the background radiation,our observed solar spectrum at CO 4.66μm is consistent with that from the National Solar *** Mg I 12.32μm working line selected by the Accurate Infrared Magnetic Field Measurements of the Sun(AIMS)project is also *** method is helpful not only for the spectral resolution calibration and background radiation correction of AIMS but also for other infrared astronomical telescopes.

关键词： Sun infrared-methods observational-instrumentation interferometers

Long-term Variation of the Solar Polar Magnetic Fields at Different Latitudes

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Research in Astronomy and Astrophysics 2024年第7期24卷 190-197页

作者： Shuhong Yang Jie Jiang Zifan Wang Yijun Hou Chunlan Jin Qiao Song Yukun Luo Ting Li Jun Zhang Yuzong Zhang Guiping Zhou yuanyong deng Jingxiu Wang National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China State Key Laboratory of Solar Activity and Space Weather National Space Science CenterChinese Academy of SciencesBeijing 100190China School of Space and Environment Beihang UniversityBeijing 102206China Key Laboratory of Space Weather National Satellite Meteorological Center(National Center for Space Weather)China Meteorological AdministrationBeijing 100081China Innovation Center for FengYun Meteorological Satellite(FYSIC) Beijing 100081China School of Physics and Materials Science Anhui UniversityHefei 230601China

The polar magnetic fields of the Sun play an important role in governing solar activity and powering fast solar ***,because our view of the Sun is limited in the ecliptic plane,the polar regions remain largely *** the high spatial resolution and polarimetric precision vector magnetograms observed by Hinode from 2012 to 2021,we investigate the long-term variation of the magnetic fields in polar caps at different *** Hinode magnetic measurements show that the polarity reversal processes in the north and south polar caps are *** variation of the averaged radial magnetic flux density reveals that,in each polar cap,the polarity reversal is completed successively from the 70°latitude to the pole,reflecting a poleward magnetic flux migration *** results clarify the polar magnetic polarity reversal process at different latitudes.

关键词： dynamo-Sun magnetic fields-Sun photosphere

The calibration and initial results of the HeI D3 line flash spectrum obtained during the 2008 total solar eclipse

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Science China(Physics,Mechanics & Astronomy) 2009年第11期52卷 1799-1805页

作者： LI Hui JI HaiSheng NI HouKun ZHANG HaiYing ZHANG YaNan LIU HongRui deng yuanyong WANG DongGuang DU QiuSheng ZHOU TuanHui LI JingWei SHEN JinHua Purple Mountain Observatory 2 Nanjing 210008China Nanjing Institute of Astronomical Optics&Technology Nanjing 210042China National Astronomical Observatories of China Beijing 100012China

The flash spectra in the HeI D3 line were obtained during the 2008 total solar eclipse. This paper describes the instrument and the calibration of the obtained flash spectrum, and presents our initial results. The average integrated intensity is Eave = 8.13×1013 erg·cm-1· s-1·ster-1 at h = 1100 km, which confirms that the HeI D3 emission is negatively correlated with the solar activity. The surface brightness reaches a maximum of F ave = 8.25×105 erg·cm-2·s-1·ster-1 at about h ≈ (1290 ± 75) km and then decreases exponentially with height when h >1800 km with an exponential index β = 1.63×10-8 cm-1.

关键词： total solar eclipse flash spectrum spectral line

A New Post-hoc Flat Field Measurement Method for the Solar X-Ray and Extreme Ultraviolet Imager Onboard the FengYun-3E Satellite

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Research in Astronomy and Astrophysics 2022年第10期22卷 1-10页

作者： Qiao Song Xianyong Bai Bo Chen Xiuqing Hu Yajie Chen Zhenyong Hou Xiaofan Zhang Lingping He Kefei Song Peng Zhang Jing-Song Wang Xiaoxin Zhang Weiguo Zong Jinping Dun Hui Tian yuanyong deng Key Laboratory of Space Weather National Satellite Meteorological Center(National Center for Space Weather)China Meteorological AdministrationBeijing 100081China State Key Laboratory of Space Weather Chinese Academy of SciencesBeijing 100190China Innovation Center for Fengyun Meteorological Satellite China Meteorological AdministrationBeijing 100081China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Changchun Institute of Optics Fine Mechanics and PhysicsChinese Academy of SciencesChangchun 130033China Key Laboratory of Radiometric Calibration and Validation for Environmental Satellites National Satellite Meteorological Center(National Center for Space Weather)China Meteorological AdministrationBeijing 100081China School of Earth and Space Sciences Peking UniversityBeijing 100871China

Extreme ultraviolet(EUV)observations are widely used in solar activity research and space weather forecasting since they can observe both the solar eruptions and the source regions of the solar *** field processing is indispensable to remove the instrumental non-uniformity of a solar EUV imager in producing high-quality scientific data from original observed ***-3E(FY-3E)is a meteorological satellite operated in a Sunsynchronous orbit,and the routine EUV imaging data from the Solar X-ray and Extreme Ultraviolet Imager(X-EUVI)onboard FY-3E has the characteristic of concentric *** advantage of the concentric rotation,we propose a post-hoc flat field measurement method for its EUV 195A channel in this *** method removes the small-scale and time-varying component of coronal activities by taking the median value for each pixel along the time axis of a concentric rotation data cube,and then derives the large-scale and invariable component of the quiet coronal radiation,and finally generates a flat field *** flat field can be generated with cadences from hundreds of minutes(one orbit)to several *** flat field accuracy can be achieved by employing more *** analysis shows that our method is able to measure the instrumental spot-like nonuniformity possibly caused by contamination on the detector,which mostly disappears after the in-orbit selfcleaning *** can also measure the quasi-periodic grid-like non-uniformity,possibly from the obscuration of the support mesh on the rear *** flat field correction,these instrumental non-uniformities from the original data are effectively ***,the X-EUVI 195A data after dark and flat field corrections are consistent with the 193A imaging data from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory,verifying the suitability of the *** post-hoc method does not occupy observation time,which is advantageous for space weather operatio

关键词： Sun corona-techniques image processing-methods data analysis-methods observational

Design and application of an autonomous Master Control System for a multi-layer magnetic and helioseismic telescope

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Astronomical Techniques and Instruments 2024年第3期1卷 187-196页

作者： Liyue Tong Yingzi Sun Xiao Yang Jiaben Lin yuanyong deng Xianyong Bai Bingxiang Wang Xiaoming Zhu Yang Bai Yi Shang Hui Wang National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Key Laboratory of Solar Activity and Space Weather National Space Science CenterChinese Academy of SciencesBeijing 100190China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China School of Electrical and Electronic Engineering Wuhan Polytechnic UniversityWuhan 430023China

With the growing significance of space weather forecasting,multi-layer magnetic and helioseismic telescopes are emerging as a key area of ***,owing to the diverse operational processes and sophisticated hardware configurations of these devices,there is an urgent need for efficient autonomous observation *** autonomous Master Control System(MCS)can ensure efficient performance,data consistency,and stability,and the prototype presented here adopts a microservices architecture,breaking down the hardware into multiple subsystems and converting their functions into individual services.A central decision-making system leads the operations,supported by three auxiliary systems and three device control *** inter-subsystem service calls,it achieves rapid imaging and spectroscopic *** verify system stability and observation efficiency,the system was tested on the Solar Full-disk Multi-layer *** results verify this system can operate automatically for 4 consecutive months,acquire photospheric vector magnetic and Doppler velocity fields within a 15-minute interval,and measure chromospheric longitudinal magnetic and Doppler velocity fields in under 180 *** ensures consistent and stable solar monitoring and serves as a practical methodological benchmark for the development of similar devices.

关键词： Astronomical instrumentation Telescopes Solar optical telescopes Automated telescopes

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天文望远镜无偏消旋镜装调方案设计及验证

中国激光 2020年第6期47卷 205-213页

作者：周明尧侯俊峰王东光邓元勇中国科学院国家天文台太阳活动重点实验室北京100101 中国科学院大学天文与空间科学学院北京100049

地平式天文望远镜在跟踪观测过程中,因方位轴与地球自转轴不重合及库徳光路中的折轴反射镜在望远镜跟踪过程中相对转动,会引入物方及像方视场旋转。传统的消旋K镜可以消除视场旋转,但会带来较大的仪器偏振,不利于望远镜实现高精度偏振... 详细信息

地平式天文望远镜在跟踪观测过程中,因方位轴与地球自转轴不重合及库徳光路中的折轴反射镜在望远镜跟踪过程中相对转动,会引入物方及像方视场旋转。传统的消旋K镜可以消除视场旋转,但会带来较大的仪器偏振,不利于望远镜实现高精度偏振测量。无偏消旋镜由5块反射镜组成,通过优化设计可以保证在消除像旋的同时减小仪器偏振,但其不规则的结构设计使装调过程面临新的挑战。针对无偏消旋镜提出双光路自准直装调方案,基于MATLAB仿真分析了镜面误差及光轴偏差对装调结果的影响,并对无偏消旋镜进行实验室装调及偏振检测。结果表明:无偏消旋镜经装调后倾斜误差可控制在15 arcsec以内,其仪器偏振明显低于传统K镜。

关键词：测量偏振测量无偏消旋镜装调方案双光路天文望远镜