In this paper a fully parametrized finite element simulation model of the stator bar end is created using the COMSOL Multiphysics.The model allows conducting the comparison of different corona protection structures’d...In this paper a fully parametrized finite element simulation model of the stator bar end is created using the COMSOL Multiphysics.The model allows conducting the comparison of different corona protection structures’design,various materials properties,and finally optimizing the corona protection system.Several samples of SiC based nonlinear conductivity materials for corona protection were fabricated in laboratory and then investigated.The conductivity dependencies on electric field(0.05 to 1 kV/mm)and temperature(20 to 155℃)were measured.By comparing the heat-resistant grades of the corona protection material and the insulating material,the maximum working temperature of the corona protection material corresponds to the heat-resistant grade F of the insulating material.As the temperature increases,the nonlinear characteristics of the corona protection material in the experiment decrease dramatically,reducing the heat-resistant grade of the corona protection material.The decrease in the nonlinear characteristics of the corona protection material at the maximum operating temperature causes the maximum electric field strength at the end of the HV rotating machines end corona protection(ECP)exceeding the corona discharge electric field strength,resulting in corona phenomenon.展开更多
Heating mechanism in the solar atmosphere(from chromosphere to corona)is one of the top-challenges in modern astronomy.The classic mechanisms can be divided into two categories:wave heating(W)and magnetic reconnection...Heating mechanism in the solar atmosphere(from chromosphere to corona)is one of the top-challenges in modern astronomy.The classic mechanisms can be divided into two categories:wave heating(W)and magnetic reconnection heating(X).Both of them still face some problems currently difficult to overcome.Recently,we proposed a new mechanism,called magnetic-gradient pumping heating(MGP,or P)which seems to overcome those difficulties,but still lacks sufficient observational evidence.Which one really explained the physics of hot corona exactly?How can observations be used to identify and verify the heating mechanism?Since different heating mechanisms will generate non-thermal particles from different accelerations and experience different propagations,they will have different responses in the broadband spectral radio observations.Among them,the non-thermal electrons from W mechanisms are closely related to shock-wave acceleration,and their radio response should be a group of spike bursts with random distribution of drifting rates;the non-thermal electrons from X mechanisms are accelerated by reconnecting electric field with bidirectional flow,and their radio response should be type III pairs or spike pairs;P mechanism will produce energetic particle upflows,and their radio response should be unidirectional fiber bursts with moderate negative drifting rates.Therefore,the heating mechanism can be identified and verified from the broadband dynamic spectral radio observations.Additionally,using high-resolution radioheliographs and spectral-imaging observations,the heating mechanisms in different regions can be identified and verified separately,thereby demonstrating the physical essence of the hot corona.展开更多
Two-dimensional(2 D) solar coronal magnetogram is difficult to be measured directly until now.From the previous knowledge,a general relation has been noticed that the brighter green-line brightness for corona,the high...Two-dimensional(2 D) solar coronal magnetogram is difficult to be measured directly until now.From the previous knowledge,a general relation has been noticed that the brighter green-line brightness for corona,the higher coronal magnetic field intensity may correspond to.To try to further reveal the relationship between coronal green line brightness and magnetic field intensity,we use the 2 D coronal images observed by Yunnan Observatories Greenline Imaging System(YOGIS) of the 10 cm Lijiang coronagraph and the coronal magnetic field maps calculated from the current-free extrapolations with the photospheric magnetograms taken by Helioseismic and Magnetic Imager(HMI) on board the Solar Dynamics Observatory(SDO) spacecraft.In our analysis,we identified the coronal loop structures and construct two-dimensional maps of the corresponding magnetic field intensity in the plane of the sky(POS) above the limb.We derive the correlation coefficients between the coronal brightness and the magnetic field intensity for different heights of coronal layers.We further use a linear combination of a Gaussian and a quadratic profile to fit the correlation coefficients distribution,finding a largest correlation coefficient of 0.82 near 1.1 R(solar radii) where is almost the top of the closed loop system.For the small closed loop system identified,the correlation coefficient distributions crossing and covering the loop are calculated.We also investigate the correlation with extended heliocentric latitude zones and long period of one whole Carrington Rotation,finding again that the maximum correlation coefficient occurs at the same height.It is the first time for us to find that the correlation coefficients are high(all are larger than 0.8) at the loop-tops and showing poor correlation coefficients with some fluctuations near the feet of the coronal loops.Our findings indicate that,for the heating of the low-latitude closed loops,both DC(dissipation of currents) and AC(dissipation of Alfvén and magnetosonic waves) mechanisms should act simultaneously on the whole closed loop system while the DC mechanisms dominate in the loop-top regions.Therefore,in the distributions of the correlation coefficients with different heights of coronal layers,for both large-and small-scale latitude ranges,the coefficients can reach their maximum values at the same coronal height of 1.1 R,which may indicate the particular importance of the height of closed loops for studying the coupling of the local emission mechanism and the coronal magnetic fields,which maybe helpful for studying the origin of the low-speed solar wind.展开更多
利用解密的美国CORONA卫星影像,在库车冲断褶皱带,开展大面积地表构造调查,获取地区的地表产状.通过建立有理函数模型(rational function model,RFM)校正CORONA影像的全景变形,利用JX-4C数字摄影测量系统进行CORONA影像的立体观测和测量...利用解密的美国CORONA卫星影像,在库车冲断褶皱带,开展大面积地表构造调查,获取地区的地表产状.通过建立有理函数模型(rational function model,RFM)校正CORONA影像的全景变形,利用JX-4C数字摄影测量系统进行CORONA影像的立体观测和测量,确定岩层面的高程值,并采用三点法在MATLAB软件中计算岩层的倾角和走向,获取地表产状.通过和野外实测数据对比,测量误差小于3°,满足了构造定量解析的精度要求.应用获取的构造产状结合二维地震反射资料,根据断层相关褶皱原理定量地提取库车地区褶皱和断层的几何学特征.展开更多
The corona current pulses generated by corona discharge are the sources of the radio interference from transmission lines and the detailed characteristics of the corona current pulses from conductor should be investig...The corona current pulses generated by corona discharge are the sources of the radio interference from transmission lines and the detailed characteristics of the corona current pulses from conductor should be investigated in order to reveal their generation mechanism.In this paper,the line-to-plane electrodes are designed to measure and analyze the characteristics of corona current pulses from positive corona discharges.The influences of inter-electrode gap and line diameters on the detail characteristics of corona current pulses,such as pulse amplitude,rise time,duration time and repetition frequency,are carefully analyzed.The obtained results show that the pulse amplitude and the repetition frequency increase with the diameter of line electrode when the electric fields on the surface of line electrodes are same.With the increase of inter-electrode gap,the pulse amplitude and the repetition frequency first decrease and then turn to be stable,while the rise time first increases and finally turns to be stable.The distributions of electric field and space charges under the line electrodes are calculated,and the influences of inter-electrode gap and line electrode diameter on the experimental results are qualitatively explained.展开更多
Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold t...Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold the key to understanding the physical mechanisms of solar eruptions,which impact the heliosphere and planetary atmospheres.The strongest disturbances in the Earth’s space environments are often associated with large-scale flux ropes from the Sun colliding with the Earth’s magnetosphere,leading to adverse,sometimes catastrophic,space-weather effects.However,it remains elusive as to how a flux rope forms and evolves toward eruption,and how it is structured and embedded in the ambient field.The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer’s perspective,with an emphasis on their structures and nascent evolution toward solar eruptions,as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation.This paper highlights an initiation mechanism for coronal mass ejections(CMEs)in which plasmoids in current sheets coalesce into a’seed’flux rope whose subsequent evolution into a CME is consistent with the standard model,thereby bridging the gap between microscale and macroscale dynamics.展开更多
A novel two-dimensional （2D） simulation method of positive corona current pulses is proposed. A control-volume- based finite element method （CV-FEM） is used to solve continuity equations, and the Galerkin finite e...A novel two-dimensional （2D） simulation method of positive corona current pulses is proposed. A control-volume- based finite element method （CV-FEM） is used to solve continuity equations, and the Galerkin finite element method （FEM） is used to solve Poisson＇s equation. In the proposed method, photoionization is considered by adopting an exact Helmholtz photoionization model. Furthermore, fully implicit discretization and variable time step are used to ensure the time-efficiency of the present method. Finally, the method is applied to a positive rod-plane corona problem. The numerical results are in agreement with the experimental results, and the validity of the proposed method is verified.展开更多
The Advanced Space-based Solar Observatory(ASO-S) mission aims to explore the two most spectacular eruptions on the Sun: solar flares and coronal mass ejections(CMEs), and their magnetism.For the study of CMEs, the pa...The Advanced Space-based Solar Observatory(ASO-S) mission aims to explore the two most spectacular eruptions on the Sun: solar flares and coronal mass ejections(CMEs), and their magnetism.For the study of CMEs, the payload Lyman-alpha Solar Telescope(LST) has been proposed. It includes a traditional white-light coronagraph and a Lyman-alpha coronagraph which opens a new window to CME observations. Polarization measurements taken by white-light coronagraphs are crucial for deriving fundamental physical parameters of CMEs. To make such measurements, there are two options for a Stokes polarimeter which have been applied by existing white-light coronagraphs for space missions. One uses a single or triple linear polarizer, the other involves both a half-wave plate and a linear polarizer. We find that the former option is subject to less uncertainty in the derived Stokes vector propagating from detector noise.The latter option involves two plates which are prone to internal reflections and may have a reduced transmission factor. Therefore, the former option is adopted as our Stokes polarimeter scheme for LST. Based on the parameters of the intended linear polarizer(s) colorPol provided by CODIXX and the half-wave plate 2-APW-L2-012 C by Altechna, it is further shown that the imperfect maximum transmittance of the polarizer significantly increases the variance amplification of Stokes vector by at least about 50% when compared with the ideal case. The relative errors of Stokes vector caused by the imperfection of colorPol polarizer and the uncertainty due to the polarizer assembly in the telescope are estimated to be about 5%. Among the considered parameters, we find that the dominant error comes from the uncertainty in the maximum transmittance of the polarizer.展开更多
It is well known that graph spectra store a lot of structural information about a graph,and it is more difficult to compute the spectra of corona graphs. In this paper two classes of new corona graphs,the corona-verte...It is well known that graph spectra store a lot of structural information about a graph,and it is more difficult to compute the spectra of corona graphs. In this paper two classes of new corona graphs,the corona-vertex of the subdivision graph G1◇G2and corona-edge of the subdivision graph G1☆G2were defined. Then,by using the coronal of a graph and some knowledge of linear algebra,the adjacency spectra and the signless Laplacian spectra of the two new graphs were explicitly computed in terms of the corresponding spectra of G1 and G2. As the application,some Aintegral graphs were constructed.展开更多
The corona discharge from transmission lines in high-altitude areas is more severe than at lower altitudes. The radio interference caused thereby is a key factor to be considered when designing transmission lines. To ...The corona discharge from transmission lines in high-altitude areas is more severe than at lower altitudes. The radio interference caused thereby is a key factor to be considered when designing transmission lines. To study the influence of altitude on negative corona characteristics, an experimental platform comprising a movable small corona cage was established: experiments were conducted at four altitudes in the range of 1120-4320 m, and data on the corona current pulse and radio interference level of 0.8-mm diameter fine copper wire under different negative voltages were collected. The experimental results show that the average amplitude, repetition frequency and average current of the corona current pulse increase with increasing altitude. The dispersion of pulse amplitude increases with increase in altitude, while the randomness of the pulse interval decreases continuously. Taking the average current as an intermediate variable,the relationship between radio interference level and altitude is obtained. The result of this research has some significance for understanding the corona discharge characteristics of ultra-highvoltage lines.展开更多
文摘In this paper a fully parametrized finite element simulation model of the stator bar end is created using the COMSOL Multiphysics.The model allows conducting the comparison of different corona protection structures’design,various materials properties,and finally optimizing the corona protection system.Several samples of SiC based nonlinear conductivity materials for corona protection were fabricated in laboratory and then investigated.The conductivity dependencies on electric field(0.05 to 1 kV/mm)and temperature(20 to 155℃)were measured.By comparing the heat-resistant grades of the corona protection material and the insulating material,the maximum working temperature of the corona protection material corresponds to the heat-resistant grade F of the insulating material.As the temperature increases,the nonlinear characteristics of the corona protection material in the experiment decrease dramatically,reducing the heat-resistant grade of the corona protection material.The decrease in the nonlinear characteristics of the corona protection material at the maximum operating temperature causes the maximum electric field strength at the end of the HV rotating machines end corona protection(ECP)exceeding the corona discharge electric field strength,resulting in corona phenomenon.
基金supported by the Strategic Priority Research Program of the Chinese Academy of Sciences XDB0560000the National Key R&D Program of China 2021YFA1600503,2022YFF0503001,2022YFF0503800+1 种基金the National Natural Science Foundation of China(NSFC,Grant No.12173050)the International Partnership Program of the Chinese Academy of Sciences 183311KYSB20200003。
文摘Heating mechanism in the solar atmosphere(from chromosphere to corona)is one of the top-challenges in modern astronomy.The classic mechanisms can be divided into two categories:wave heating(W)and magnetic reconnection heating(X).Both of them still face some problems currently difficult to overcome.Recently,we proposed a new mechanism,called magnetic-gradient pumping heating(MGP,or P)which seems to overcome those difficulties,but still lacks sufficient observational evidence.Which one really explained the physics of hot corona exactly?How can observations be used to identify and verify the heating mechanism?Since different heating mechanisms will generate non-thermal particles from different accelerations and experience different propagations,they will have different responses in the broadband spectral radio observations.Among them,the non-thermal electrons from W mechanisms are closely related to shock-wave acceleration,and their radio response should be a group of spike bursts with random distribution of drifting rates;the non-thermal electrons from X mechanisms are accelerated by reconnecting electric field with bidirectional flow,and their radio response should be type III pairs or spike pairs;P mechanism will produce energetic particle upflows,and their radio response should be unidirectional fiber bursts with moderate negative drifting rates.Therefore,the heating mechanism can be identified and verified from the broadband dynamic spectral radio observations.Additionally,using high-resolution radioheliographs and spectral-imaging observations,the heating mechanisms in different regions can be identified and verified separately,thereby demonstrating the physical essence of the hot corona.
基金supported by the National Natural Science Foundation of China under grants 11873090, 12173086, 11873092, U2031148the CAS “Light of West China” Program。
文摘Two-dimensional(2 D) solar coronal magnetogram is difficult to be measured directly until now.From the previous knowledge,a general relation has been noticed that the brighter green-line brightness for corona,the higher coronal magnetic field intensity may correspond to.To try to further reveal the relationship between coronal green line brightness and magnetic field intensity,we use the 2 D coronal images observed by Yunnan Observatories Greenline Imaging System(YOGIS) of the 10 cm Lijiang coronagraph and the coronal magnetic field maps calculated from the current-free extrapolations with the photospheric magnetograms taken by Helioseismic and Magnetic Imager(HMI) on board the Solar Dynamics Observatory(SDO) spacecraft.In our analysis,we identified the coronal loop structures and construct two-dimensional maps of the corresponding magnetic field intensity in the plane of the sky(POS) above the limb.We derive the correlation coefficients between the coronal brightness and the magnetic field intensity for different heights of coronal layers.We further use a linear combination of a Gaussian and a quadratic profile to fit the correlation coefficients distribution,finding a largest correlation coefficient of 0.82 near 1.1 R(solar radii) where is almost the top of the closed loop system.For the small closed loop system identified,the correlation coefficient distributions crossing and covering the loop are calculated.We also investigate the correlation with extended heliocentric latitude zones and long period of one whole Carrington Rotation,finding again that the maximum correlation coefficient occurs at the same height.It is the first time for us to find that the correlation coefficients are high(all are larger than 0.8) at the loop-tops and showing poor correlation coefficients with some fluctuations near the feet of the coronal loops.Our findings indicate that,for the heating of the low-latitude closed loops,both DC(dissipation of currents) and AC(dissipation of Alfvén and magnetosonic waves) mechanisms should act simultaneously on the whole closed loop system while the DC mechanisms dominate in the loop-top regions.Therefore,in the distributions of the correlation coefficients with different heights of coronal layers,for both large-and small-scale latitude ranges,the coefficients can reach their maximum values at the same coronal height of 1.1 R,which may indicate the particular importance of the height of closed loops for studying the coupling of the local emission mechanism and the coronal magnetic fields,which maybe helpful for studying the origin of the low-speed solar wind.
文摘利用解密的美国CORONA卫星影像,在库车冲断褶皱带,开展大面积地表构造调查,获取地区的地表产状.通过建立有理函数模型(rational function model,RFM)校正CORONA影像的全景变形,利用JX-4C数字摄影测量系统进行CORONA影像的立体观测和测量,确定岩层面的高程值,并采用三点法在MATLAB软件中计算岩层的倾角和走向,获取地表产状.通过和野外实测数据对比,测量误差小于3°,满足了构造定量解析的精度要求.应用获取的构造产状结合二维地震反射资料,根据断层相关褶皱原理定量地提取库车地区褶皱和断层的几何学特征.
基金supported by National Natural Science Foundation of China under Grant No.51707066by the Fundamental Research Funds for the Central Universities under Grant No.2017 MS004 and No.XCA17003-04
文摘The corona current pulses generated by corona discharge are the sources of the radio interference from transmission lines and the detailed characteristics of the corona current pulses from conductor should be investigated in order to reveal their generation mechanism.In this paper,the line-to-plane electrodes are designed to measure and analyze the characteristics of corona current pulses from positive corona discharges.The influences of inter-electrode gap and line diameters on the detail characteristics of corona current pulses,such as pulse amplitude,rise time,duration time and repetition frequency,are carefully analyzed.The obtained results show that the pulse amplitude and the repetition frequency increase with the diameter of line electrode when the electric fields on the surface of line electrodes are same.With the increase of inter-electrode gap,the pulse amplitude and the repetition frequency first decrease and then turn to be stable,while the rise time first increases and finally turns to be stable.The distributions of electric field and space charges under the line electrodes are calculated,and the influences of inter-electrode gap and line electrode diameter on the experimental results are qualitatively explained.
基金supported by the National Natural Science Foundation of China(Grant Nos.41761134088,41774150,and 11925302)CAS Key Research Program(Grant No.KZZD-EW-01-4)the fundamental research funds for the central universities,and the Strategic Priority Program of the Chinese Academy of Sciences(Grant No.XDB41000000)。
文摘Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold the key to understanding the physical mechanisms of solar eruptions,which impact the heliosphere and planetary atmospheres.The strongest disturbances in the Earth’s space environments are often associated with large-scale flux ropes from the Sun colliding with the Earth’s magnetosphere,leading to adverse,sometimes catastrophic,space-weather effects.However,it remains elusive as to how a flux rope forms and evolves toward eruption,and how it is structured and embedded in the ambient field.The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer’s perspective,with an emphasis on their structures and nascent evolution toward solar eruptions,as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation.This paper highlights an initiation mechanism for coronal mass ejections(CMEs)in which plasmoids in current sheets coalesce into a’seed’flux rope whose subsequent evolution into a CME is consistent with the standard model,thereby bridging the gap between microscale and macroscale dynamics.
基金Project supported by the National Basic Research Program of China(Grant No.2011CB209402)the National Natural Science Foundation of China(Grant No.51177041)the Fundamental Research Funds for the Central Universities,China(Grant No.12QX01)
文摘A novel two-dimensional （2D） simulation method of positive corona current pulses is proposed. A control-volume- based finite element method （CV-FEM） is used to solve continuity equations, and the Galerkin finite element method （FEM） is used to solve Poisson＇s equation. In the proposed method, photoionization is considered by adopting an exact Helmholtz photoionization model. Furthermore, fully implicit discretization and variable time step are used to ensure the time-efficiency of the present method. Finally, the method is applied to a positive rod-plane corona problem. The numerical results are in agreement with the experimental results, and the validity of the proposed method is verified.
基金supported by NSFC (Grant Nos. 11522328, 11473070, 11427803 and U1731241)CAS Strategic Pioneer Program on Space Science (Grant Nos. XDA15010600, XDA15052200, XDA15320103 and XDA15320301)the National Key Research and Development Program of China (2018YFA0404202)
文摘The Advanced Space-based Solar Observatory(ASO-S) mission aims to explore the two most spectacular eruptions on the Sun: solar flares and coronal mass ejections(CMEs), and their magnetism.For the study of CMEs, the payload Lyman-alpha Solar Telescope(LST) has been proposed. It includes a traditional white-light coronagraph and a Lyman-alpha coronagraph which opens a new window to CME observations. Polarization measurements taken by white-light coronagraphs are crucial for deriving fundamental physical parameters of CMEs. To make such measurements, there are two options for a Stokes polarimeter which have been applied by existing white-light coronagraphs for space missions. One uses a single or triple linear polarizer, the other involves both a half-wave plate and a linear polarizer. We find that the former option is subject to less uncertainty in the derived Stokes vector propagating from detector noise.The latter option involves two plates which are prone to internal reflections and may have a reduced transmission factor. Therefore, the former option is adopted as our Stokes polarimeter scheme for LST. Based on the parameters of the intended linear polarizer(s) colorPol provided by CODIXX and the half-wave plate 2-APW-L2-012 C by Altechna, it is further shown that the imperfect maximum transmittance of the polarizer significantly increases the variance amplification of Stokes vector by at least about 50% when compared with the ideal case. The relative errors of Stokes vector caused by the imperfection of colorPol polarizer and the uncertainty due to the polarizer assembly in the telescope are estimated to be about 5%. Among the considered parameters, we find that the dominant error comes from the uncertainty in the maximum transmittance of the polarizer.
基金National Natural Science Foundation of China(No.11361033)Natural Science Foundation of Gansu Province,China(No.1212RJZA029)
文摘It is well known that graph spectra store a lot of structural information about a graph,and it is more difficult to compute the spectra of corona graphs. In this paper two classes of new corona graphs,the corona-vertex of the subdivision graph G1◇G2and corona-edge of the subdivision graph G1☆G2were defined. Then,by using the coronal of a graph and some knowledge of linear algebra,the adjacency spectra and the signless Laplacian spectra of the two new graphs were explicitly computed in terms of the corresponding spectra of G1 and G2. As the application,some Aintegral graphs were constructed.
基金supported by the Science and Technology Project of State Grid Corporation of China (No.5200202155587A-0-5-GC)。
文摘The corona discharge from transmission lines in high-altitude areas is more severe than at lower altitudes. The radio interference caused thereby is a key factor to be considered when designing transmission lines. To study the influence of altitude on negative corona characteristics, an experimental platform comprising a movable small corona cage was established: experiments were conducted at four altitudes in the range of 1120-4320 m, and data on the corona current pulse and radio interference level of 0.8-mm diameter fine copper wire under different negative voltages were collected. The experimental results show that the average amplitude, repetition frequency and average current of the corona current pulse increase with increasing altitude. The dispersion of pulse amplitude increases with increase in altitude, while the randomness of the pulse interval decreases continuously. Taking the average current as an intermediate variable,the relationship between radio interference level and altitude is obtained. The result of this research has some significance for understanding the corona discharge characteristics of ultra-highvoltage lines.
