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Using machine learning to aid treatment decision and risk assessment for severe three-vessel coronary artery disease

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Journal of Geriatric Cardiology 2022年第5期19卷 367-376页

作者： Liu JIE Xin-Xing FENG Yan-Feng DUAN jun-Hao LIU Ce ZHANG lin JIANG Lian-jun XU Jian TIAN Xue-Yan ZHAO Yin ZHANG Kai SUN Bo XU Wei ZHAO Ru-Tai HUI Run-lin GAO Ji-Zheng WANG Jin-Qing YUAN Xin HUANG Lei SONG State Key Laboratory of Cardiovascular Disease Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina Endocrinology and Cardiovascular Disease Centre Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina Department of Endocrinology Fuwai HospitalChinese Academy of Medical SciencesShenzhenChina Nanjing TooBoo Technology Co. Ltd.NanjingChina Department of Cardiology Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina Cardiomyopathy Ward Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina Medical Research Center Peking Union Medical College HospitalChinese Academy of Medical Sciences&Peking Union Medical CollegeBeijingChina Information Center Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina National Clinical Research Center for Cardiovascular Diseases Fuwai HospitalNational Center for Cardiovascular DiseasesChinese Academy of Medical Sciences and Peking Union Medical CollegeBeijingChina Solar activity Prediction Center National Astronomical ObservatoriesChinese Academy of SciencesBeijingChina

BACKGROUND Three-vessel disease(TVD)with a SYNergy between PCI with TAXus and cardiac surgery(SYNTAX)score of≥2. is one of the most severe types of coronary artery *** aimed to take advantage of machine learning to help in de-cision-making and prognostic evaluation in such *** We analyzed 3786 patients who had TVD with a SYNTAX score of≥2.,had no history of previous revascularization,and underwent either coronary artery bypass grafting(CABG)or percutaneous coronary intervention(PCI)after *** patients were randomly assigned to a training group and testing *** C4.5 decision tree algorithm was applied in the training group,and all-cause death after a median follow-up of 6.6 years was regarded as the class *** The decision tree algorithm selected age and left ventricular end-diastolic diameter(LVEDD)as splitting features and divided the patients into three subgroups:subgroup 1(age of≤67 years and LVEDD of≤53 mm),subgroup 2.age of≤67 years and LVEDD of>53 mm),and subgroup 3(age of>67 years).PCI conferred a patient survival benefit over CABG in sub-group *** was no significant difference in the risk of all-cause death between PCI and CABG in subgroup 1 and subgroup 3 in both the training data and testing *** the total study population,the multivariable analysis revealed significant dif-ferences in the risk of all-cause death among patients in three *** The combination of age and LVEDD identified by machine learning can contribute to decision-making and risk assessment of death in patients with severe *** present results suggest that PCI is a better choice for young patients with severe TVD characterized by left ventricular dilation.

关键词： coronary testing treatment

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A digital pulsar backend based on FPGA

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Research in Astronomy and Astrophysics 2017年第1期17卷 97-102页

作者： Jin-Tao Luo Lan Chen Jin-lin Han Ali Esamdin Ya-jun Wu Zhi-Xuan Li Long-Fei Hao Xiu-Zhong Zhang National Time Service CenterChinese Academy of SciencesXi'an 710600China Key Laboratory of Time and Frequency Primary Standards Chinese Academy of SciencesXi'an 710600China National astronomical observatories Chinese Academy of SciencesBeijing 100012China Xinjiang astronomical observatory Chinese Academy of SciencesUrumqi 830011China Shanghai Institute of Technology Shanghai 200235China yunnan observatories Chinese Academy of SciencesKunming 650011China Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China

A digital pulsar backend based on a Field Programmable Gate Array （FPGA） is developed. It is designed for incoherent de-dispersion of pulsar observations and has a maximum bandwidth of 512.Hz. The channel bandwidth is fixed to 1 MHz, and the highest time resolution is 10 p.s. Testing observations were carried out using the Urumqi 2.-m telescope administered by Xinjiang astronomical observatory and the {2. 40-m telescope administered by yunnan observatories, targeting PSR J0332.5434 in the L band and PSR J0437-4715 in the S band, respectively. The successful observation of PSR J0437-4715 demonstrates its ability to observe millisecond pulsars.

关键词： instrumentation miscellaneous - methods data analysis - pulsars general

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The THU-NAOC transient survey: the performance and results from the first year

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Research in Astronomy and Astrophysics 2015年第2期15卷 215-224页

作者： Tian-Meng Zhang Xiao-Feng Wang jun-Cheng Chen Ju-Jia Zhang Li Zhou Wen-Xiong Li Qing Liu jun Mo Kai-Cheng Zhang Xin-Yu Yao Xu-{2. Zhao Xu Zhou jun-Dan Nie Fang Huang Zhao-Ji Jiang jun Ma {2.g-Zhi Wang Chao Wu Zhi-Min Zhou Hu Zou Li-Fan Wang Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Physics Department and Tsinghua Center for Astrophysics Tsinghua University yunnan observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of chinese academy of sciences Purple Mountain observatory Chinese Academy of Sciences Astronomy Department Beijing Normal University National astronomical observatories Chinese Academy of Sciences

The Tsinghua University-National astronomical observatories,{2. （NAOC） Transient Survey is an automatic survey that conducts a systematic exploration of optical transients. This project utilizes a 60/90 cm Schmidt telescope at the Xinglong Station of NAOC. This survey repeatedly covers - 1000 square degrees of the northern sky with a cadence of 34 d. With an exposure of 60 s, the survey reaches a limiting unfiltered magnitude of about 19.5 mag, which enables us to discover supernovae in their relatively young stages. We describe the overall performance of our survey during the first year and present some preliminary results.

关键词： supernovae quasars and active galactic nuclei stars

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Nucleonic ~1S_0 Superfluidity Induced by a Soft Pion in Neutron Star Matter with Antikaon Condensations

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chinese Physics Letters 2019年第6期36卷 12-16页

作者： Yan Xu Qi-jun Zhi Yi-Bo Wang Xiu-lin Huang Wen-Bo Ding Zi Yu Cheng-Zhi Liu Changchun observatory National Astronomical Observatories Chinese Academy of Sciences Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing College of Mathematics and Physics Bohai University College of Science Nanjing Forestry University

The nucleonic ~1S_0 superfluidity is investigated by solving the gap equation for the Reid soft-core potential as the nucleon-nucleon interaction in neutron star(NS) matter which is considered to be made up of p, e, μ and condensed antikaon matter. We mainly study the influence of the soft pion-induced potential on the nucleonic^1S_0 pairing gaps in the above NS matter. It is found that the intensities of the nucleonic ~1S_0 pairing gaps including the soft pion-induced potential are smaller than those calculated in the case of not including the soft pion-induced potential. Furthermore, the nucleonic ~1S_0 pairing gaps with the soft pion-induced potential fall into decline with the deepening of the optical potential of antikaons in the above NS matter, whereas they increase with the parameter η for the fixed optical potential of antikaons. Due to the appearance of the soft pion-induced potential, the maximum values of nucleonic ~1S_0 pairing gaps at parameter η = 0.2.,0.55 are suppressed by1.7%-6.8% with respect to the case without soft pion-induced potential in the above NS matter.

关键词： neutron star(NS) Antikaon Condensations Soft Pion

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The correction of diurnal effects on CSTAR photometry

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Research in Astronomy and Astrophysics 2014年第3期14卷 345-356页

作者： Song-Hu Wang Xu Zhou Hui Zhang Ji-lin Zhou Hui-Gen Liu Ze-Yang Meng jun Ma Tian-Meng Zhang Zhou Fan Hu Zou Department of Astronomy & Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education Nanjing University National astronomical observatories Chinese Academy of Sciences

In January, 2.08 the chinese Small Telescope ARray （CSTAR） was suc-cessfully deployed at Dome A, Antarctica. Because CSTAR consists of four static14.5 cm telescopes pointing at the same 4.5° x 4.5° field around the south celestialpole, diurnal motion can be seen in its field of view. The stars are centered at differentpositions in different exposure frames. During four months of continuous observationsduring the polar night of 2.08, about 0.3 million/-band images were obtained. In thelatest version of the released photometric catalog, the effects of diurnal motion of thestars on the static CSTAR optical system can be obviously found. In this work, weupdate the CSTAR catalog by carefully analyzing and correcting the systematic errorscaused by diurnal motion of stars on imperfectly flat-fielded frames.

关键词： methods: data analysis techniques: photometric

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Chemical mixing by turbulent convection in the overshooting region below the convective envelope of RGB stars

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Research in Astronomy and Astrophysics 2011年第11期11卷 1351-1370页

作者： Xiang-jun Lai Yan Li National astronomical observatories / {2. observatory Chinese Academy of SciencesKunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy ofSciences Kunming 650011 China Graduate University of chinese academy of sciences Beijing 100049 China

Based on the turbulent convection model （TCM）, we investigate chemical mixing in the bottom overshooting region of the convective envelope of intermediatemass stars, focusing on its influence on the formation and extension of blue loops in the Hertzsprung-Russell （HR） diagram. A diffusive mixing model is adopted during the Red Giant Branch （RGB） phase. The properties of the blue loop are changed by modification of the element profiles above the H-burning shell, which results from the incomplete mixing in the bottom overshooting region when the stellar model evolves up along the RGB. Such modification of the element profiles will lead to an increase of opacity in the region just above the H-burning shell and a decrease of opacity in the outer homogeneous convection zone, which will result in a quick decrease of the H-shell nuclear luminosity LH when the stellar model evolves from the RGB tip to its bottom and, finally, a much weaker and smaller convection zone will be obtained in the stellar envelope. This helps to form a longer blue loop. The extension of the blue loop is very sensitive to the parameters （Cx and αTCM） of the diffusive mixing model and of the TCM. The results mainly show that： 1） comparing the results of the classical model with the mixing-length theory, the lengths of the obtained blue loops with different combinations of the values of Cx and αTCM are all increased and the length of the blue loop increases with the values of parameters Cx and αTCM; 2. the diffusive mixing model can significantly extend the time of stellar models lingering on the blue side of the HR diagram, even though the length of the blue loop for the 7M⊙ star has a less prominent difference between the classical and diffusive mixing model; 3） both the observations referring to the location of the Cepheid instability strip and the number ratio NB/NR of blue to red evolved stars in the Galactic open clusters can confine the two parameters in a range of 0.5 ≤ αLTCM ≤ 0.9 and 10-5 ≤

关键词： stars convection-star interiors-star HR diagram-blue loops-Cepheids-Galactic open clusters

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Characteristics of convection and overshooting in RGB and AGB stars

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Research in Astronomy and Astrophysics 2011年第10期11卷 1143-1157页

作者： Xiang-jun Lai Yan Li National astronomical observatories / {2. observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy ofSciences Kunming 650011 China Graduate University of chinese academy of sciences Beijing 100049 China.

Based on the turbulent convection model （TCM） of Li ＆ Yang, we have studied the characteristics of turbulent convection in the envelopes of 2.and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convective unstable zone, we find that the turbulent correlations are proportional to functions of a common factor （V - V^d）T, which explains similar distributions in those correlations. For the TCM we find that if the obtained stellar temperature structure is close to that of the mixing length theory （MLT）, the convective motion will have a much larger velocity and thus be more violent. However, if the turbulent velocity is adjusted to be close to that of the MLT, the superadiabatic convection zone would be much more extended inward, which would lead to a lower effective temperature of the stellar model. For the overshooting distance, we find that the e-folding lengths of the turbulent kinetic energy k in both the top and bottom overshooting regions decrease as the stellar model is progressively located farther up along the Hayashi line, but both the extents of the decrease are not obvious. The overshooting distances of the turbulent correlation /u＇rT＂ are almost the same for the different stellar models with the same set of TCM parameters. For the decay modes of the kinetic energy k, we find that they are very similar for different stellar models based on the same set of TCM parameters, and there is a nearly linear relationship between lg k and In P for different stellar models. When Cs or α increases while the other parameters are fixed, the obtained linearly decaying distance will become longer.

关键词： stars RGB and AGB -- convection of stars -- turbulent convection model convective overshooting

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The In-Flight Realtime Trigger and Localization Software of GECAM

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Research in Astronomy and Astrophysics 2024年第10期24卷 11-24页

作者： Xiao-Yun Zhao Shao-lin Xiong Xiang-Yang Wen Xin-Qiao Li Ce Cai Shuo Xiao Qi Luo Wen-Xi Peng Dong-Ya Guo Zheng-Hua An Ke Gong Jin-Yuan Liao Yan-Qiu Zhang Yue Huang Lu Li Xing Wen Fei Zhang Jing Duan Chen-Wei Wang Dong-Li Shi Peng Zhang Qi-Bin Yi Chao-Yang Li Yan-Bing Xu Xiao-Hua Liang Ya-Qing Liu Da-Li Zhang Xi-Lei Sun Fan Zhang Gang Chen Huan-Yu Wang Sheng Yang Xiao-Jing Liu Min Gao Mao-Shun Li Jin-Zhou Wang Xing Zhou Yi Zhao Wang-Chen Xue Chao Zheng Jia-Cong Liu Xing-Bo Han Jin-ling Qi Jia Huang Ke-Ke Zhang Can Chen Xiong-Tao Yang Dong-Jie Hou Yu-Sa Wang Rui Qiao Xiang Ma Xiao-Bo Li Ping Wang Xin-Ying Song Li-Ming Song Shi-Jie Zheng Bing Li Hong-Mei Zhang Yue Zhu Wei Chen Jian-Jian He Zhen Zhang Jin Hou Hong-{2. Wang Yan-Chao Hao Xiang-Yu Wang Zong-Yuan Yang Zhi-Long Wen Zhi Chang Yuan-Yuan Du Rui Gao Xiao-Fei Lan Yan-Guo Li Gang Li Xu-Fang Li Fang-{2. Lu Hong Lu Bin Meng Feng Shi Hui Wang Hui-Zhen Wang Yu-Peng Xu Jia-Wei Yang Xue-Juan Yang Shuang-Nan Zhang Chao-Yue Zhang Cheng-Mo Zhang Zhi-Cheng Tang Cheng Cheng Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Chinese Academy of SciencesBeijing 100049China School of Information Science and Technology Southwest Jiaotong UniversityChengdu 611756China Key Laboratory of Stellar and Interstellar Physics and Department of Physics Xiangtan UniversityXiangtan 411105China Physics and Space Science College China West Normal UniversityNanchong 637002China Department of Astronomy Beijing Normal UniversityBeijing 100875China Innovation academy for Microsatellites of CAS Shanghai 201203China Changchun University of Science and Technology Changchun 130022China chinese academy of {2. South America Center for Astronomy National Astronomical ObservatoriesCASBeijing 100101China

Realtime trigger and localization of bursts are the key functions of GECAM,an all-sky gamma-ray monitor launched on 2.2. December *** developed a multifunctional trigger and localization software operating in the CPU of the GECAM Electronic *** onboard software has the following features:high trigger efficiency for real celestial bursts with a suppression of false triggers caused by charged particle bursts and background fluctuation,dedicated localization algorithm optimized for both short and long bursts,and low time latency of the trigger information which is downlinked through the Global Short Message Communication service of the global BeiDou navigation *** paper provides a detailed description of the design and development of the trigger and localization software system for *** covers the general design,workflow,the main functions,and the algorithms used in the *** paper also includes on-ground trigger tests using simulated gamma-ray bursts generated by a dedicated X-ray tube,as well as an overview of the performance for real celestial bursts during its in-orbit operation.

关键词： telescopes instrumentation:detectors methods:observational

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Breaking of Large-Scale Filament due to Magnetic Reconnection and Consequent Partial Eruption

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天文和天体物理学研究:英文版 2023年第9期23卷 194-206页

作者： Kaifeng Kang Yang Guo Yan Li Jingxing Wang jun lin yunnan observatories Chinese Academy of SciencesKunming 650216China University of chinese academy of sciences Beijing 100049China Center for astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China yunnan Key Laboratory of Solar Physics and Space Science Kunming 650216China School of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics Nanjing UniversityNanjing 210023China

Following our previous work,we studied the partial eruption of a large-scale horse-shoe-like filament that had beenobserved in a decaying active region on the solar disk for more than 4.5 *** filament became active after itwas broken into two pieces,P1 and P2.seen in Hα,by magnetic reconnection between the magnetic field around itand that of a newly emerging active region nearby.P1 eventually erupted 13 hr after the breaking and escaped fromthe Sun,developing to a fast coronal mass ejection,and P2.*** the mass in P1 falling down to P2.in theeruption suggests that the global magnetic fields over P1 and P2.were still connected to each other prior to *** reconnection process breaking the filament occurred outside the filament,and P1 and P2.were locatedalmost at the same altitude,so the fashion of the filament partial eruption studied here differs from that of the“double-decker model”and that of reconnection inside the *** the decay indices of thebackground fields above P1 and P2.n_(1)and n_(2.,showed that the altitude where n_(1)exceeds the critical value of n_(c)=1.5 for the loss of equilibrium or the torus instability is lower than that where n_(2.>nc,and that n_(1)>n_(2. alwaysholds at all *** this fact with that the eruption occurred 13 hr after filament was broken byreconnection,we conclude that the eruption of P1 was triggered by the loss of equilibrium or the torus instability inthe configuration,and magnetic reconnection breaking the filament helped weaken the confinement of thebackground field on P1,allowing P1 to *** features of the eruption and the corresponding physicalscenario were also discussed.

关键词： Sun activity-Sun filaments-prominences-Sun coronal mass ejections(CMEs)-Sun flares-Sun magnetic fields

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日冕准周期快模磁声波的研究进展

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天文学进展 2024年第2期42卷 224-239页

作者：苗玉虎邓林华苏江涛管明祥夏林中华韵之曹雪梅袁丁深圳信息职业技术学院信息与通信学院深圳518172 哈尔滨工业大学(深圳)空间科学与应用技术研究院深圳518055 云南省太阳物理与空间目标监测重点实验室昆明650216 云南民族大学数学与计算机科学学院昆明650504 中国科学院国家天文台北京100101 中国科学院大学北京100049

日冕准周期快模磁声波是日冕中较常见的一种波动现象,这种波动现象通常与耀斑和日冕物质抛射等太阳活动爆发相关。根据准周期快模磁声波列的特征,还可以细分为窄准周期快模磁声波和宽准周期快模磁声波。研究表明,准周期快模磁声波包含... 详细信息

日冕准周期快模磁声波是日冕中较常见的一种波动现象,这种波动现象通常与耀斑和日冕物质抛射等太阳活动爆发相关。根据准周期快模磁声波列的特征,还可以细分为窄准周期快模磁声波和宽准周期快模磁声波。研究表明,准周期快模磁声波包含的关键物理信息可以用来诊断耀斑核心区域特征、测量日冕磁场以及探测能量释放和传输等。简单叙述了准周期快模磁声波相关的主要观测特征和模拟结果,重点介绍准周期快模磁声波的最新研究进展及冕震学应用,讨论了准周期快模磁声波的激发机制,展望了未来需要研究的问题,并提供相关研究方法作为参考。

关键词：磁流体力学波耀斑磁场日冕物质抛射

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