The characteristics of negative corona discharge and radio interference at different altitudes based on coaxial wire-cylinder gap

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.

Observation of Standing Slow Magneto-acoustic Waves in a Flaring Active Region Corona Loop

Intensity fluctuations are frequently observed in different regions and structures of the solar corona.These fluctuations may be caused by magneto-hydrodynamic(MHD)waves in coronal plasma.MHD waves are prime candidates for the dynamics,energy transfer,and anomalous temperature of the solar corona.In this paper,analysis is conducted on intensity and temperature fluctuations along the active region coronal loop(NOAA AR 13599)near solar flares.The intensity and temperature as functions of time and distance along the loop are extracted using images captured by the Atmospheric Imaging Assembly(AIA)instrument onboard the Solar Dynamics Observatory(SDO)space telescope.To observe and comprehend the causes of intensity and temperature fluctuations,after conducting initial processing,and applying spatial and temporal frequency filters to data,enhanced distance-time maps of these variables are drawn.The space-time maps of intensities show standing oscillations at wavelengths of 171,193,and 211A with greater precision and clarity than earlier findings.The amplitude of these standing oscillations(waves)decreases and increases over time.The average values of the oscillation period,damping time,damping quality,projected wavelength,and projected phase speed of standing intensity oscillations are in the range of 15-18 minutes,24-31 minutes,1.46″-2″,132″-134″,and 81-100 km s^(-1),respectively.Also,the differential emission measure peak temperature values along the loop are found in the range of 0.51-3.98 MK,using six AIA passbands,including 94,131,171,193,211,and 335?.Based on the values of oscillation periods,phase speeds,damping time,and damping quality,it is inferred that the fluctuations in intensity are related to standing slow magneto-acoustic waves with weak damping.

Non-thermal atmospheric-pressure positive pulsating corona discharge in degradation of textile dye Reactive Blue 19 enhanced by Bi_(2)O_(3) catalyst

In this work,monoclinic Bi_(2)O_(3) was applied for the first time,to the best of our knowledge,as a catalyst in the process of dye degradation by a non-thermal atmospheric-pressure positive pulsating corona discharge.The research focused on the interaction of the plasma-generated species and the catalyst,as well as the role of the catalyst in the degradation process.Plasma decomposition of the anthraquinone reactive dye Reactive Blue 19(RB 19) was performed in a selfmade reactor system.Bi_(2)O_(3) was prepared by electrodeposition followed by thermal treatment,and characterized by x-ray diffraction,scanning electron microscopy and energy-dispersive xray techniques.It was observed that the catalyst promoted decomposition of plasma-generated H_(2)O_(2) into ·OH radicals,the principal dye-degrading reagent,which further attacked the dye molecules.The catalyst improved the decolorization rate by 2.5 times,the energy yield by 93.4%and total organic carbon removal by 7.1%.Excitation of the catalyst mostly occurred through strikes by plasma-generated reactive ions and radical species from the air,accelerated by the electric field,as well as by fast electrons with an energy of up to 15 eV generated by the streamers reaching the liquid surface.These strikes transferred the energy to the catalyst and created the electrons and holes,which further reacted with H_(2)O_(2) and water,producing ·OH radicals.This was indentified as the primary role of the catalyst in this process.Decolorization reactions followed pseudo first-order kinetics.Production of H_(2)O_(2) and the dye degradation rate increased with increase in the input voltage.The optimal catalyst dose was 500 mg·dm^(-3).The decolorization rate was a little lower in river water compared with that in deionized water due to the side reactions of ·OH radicals with organic matter and inorganic ions dissolved in the river water.

Electromagnetic Ion Beam Instability in the Solar Corona

Remote-sensing measurements indicate that heavy ions in the corona undergo an anisotropic and mass-charge dependent energization.A popular explanation to this phenomenon is the damping of the Alfven/ion cyclotron waves.In this paper,we propose that the ion beam instability can be an important source of the Alfven/ion cyclotron waves,and we study the excitation of the ion beam instability in the corona at the heliocentric distance~3R_(⊙)and the corresponding energy transfer process therein ba sed on plasma kinetic theory.The results indicate that the existence of the motionless heavy ions inhibits the ion beam instability.However,the anisotropic beams of heavy ions promote the excitation of the ion beam instability.Besides,the existence ofαbeams can provide a second energy source for exciting beam instability.However,when both the proton beam and the a beam reach the instability excitation threshold,the proton beam driven instability excites preferentially.Moreover,the excitation threshold of the Alfven/ion cyclotron instability driven by ion beam is of the local Alfven speed or even less in the corona.

End-to-end computational design for an EUV solar corona multispectral imager with stray light suppression

An extreme ultraviolet solar corona multispectral imager can allow direct observation of high temperature coronal plasma,which is related to solar flares,coronal mass ejections and other significant coronal activities.This manuscript proposes a novel end-to-end computational design method for an extreme ultraviolet(EUV)solar corona multispectral imager operating at wavelengths near 100 nm,including a stray light suppression design and computational image recovery.To suppress the strong stray light from the solar disk,an outer opto-mechanical structure is designed to protect the imaging component of the system.Considering the low reflectivity(less than 70%)and strong-scattering(roughness)of existing extreme ultraviolet optical elements,the imaging component comprises only a primary mirror and a curved grating.A Lyot aperture is used to further suppress any residual stray light.Finally,a deep learning computational imaging method is used to correct the individual multi-wavelength images from the original recorded multi-slit data.In results and data,this can achieve a far-field angular resolution below 7",and spectral resolution below 0.05 nm.The field of view is±3 R_(☉)along the multi-slit moving direction,where R☉represents the radius of the solar disk.The ratio of the corona's stray light intensity to the solar center's irradiation intensity is less than 10-6 at the circle of 1.3 R_(☉).

Corona渲染技术在室内效果图仿真制作中的应用教学——以“教研室办公空间”效果图制作为例

Corona是一款建筑可视化渲染器,可作为插件集成在3ds Max中,它渲染设置简单,可在浮动视口开启交互式渲染并实时观察渲染结果,可以渲染出照片级写实的室内效果图。以“教研室办公空间”Corona渲染为例,基于3ds Max通过硬装材质赋予、硬装场景灯光设置、硬装场景摄影机创建及视口设置,完成软装和渲染输出,从而阐明Corona渲染器在室内设计项目、室内设计专业教学中的应用,为其他室内效果图仿真提供技术参考。

On the Relation Between Coronal Green Line Brightness and Magnetic Fields Intensity

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.

基于Corona和Spot-5影像的图们江下游敬信湿地变化研究

采用1964年的Corona影像和2004年的Spot-5影像作为数据源,结合"3S"技术与实地考查资料,对图们江下游敬信湿地信息进行了提取与分类,分别得到了研究区1964年和2004年的湿地分类图;通过建立研究区的湿地动态变化特征模型,从各类型湿地的面积变化和斑块变化两个角度,研究敬信湿地的变化特征及其成因。结果表明,研究区各类型湿地在气候变化、人类活动等因素的影响下发生了不同程度的变化,与1964年相比,2004年研究区人工湿地面积增加了16.923km2,这主要是修建龙山水库以及水田、养鱼池和孵化池面积大量增加所致;而自然湿地受到严重破坏,面积减少了17.33km2,河流和沼泽面积都减少了50%以上。研究区河流的斑块数急剧减少,沼泽湿地的斑块破碎化程度加剧,河流和沼泽湿地的斑块分维值明显下降,大面积沼泽被开发成水田,这两种湿地的空间自我相似性逐渐变差。研究区部分湖泊被开发利用,人为束水使得水面面积扩大,当地居民为了发展经济,在湖泊中从事鱼类养殖以及用湖泊水进行农业灌溉等活动,研究区人类活动干扰日趋严重。

基于Corona和Spot影像的近40年黑土典型区侵蚀沟动态变化

沟状侵蚀是我国东北黑土区一种比较常见的土壤侵蚀类型。当前国内外学者对侵蚀沟动态变化的研究多采用GPS或摄影测量的方法监测某些侵蚀沟的短期变化,由于缺少早期高分辨率的卫星影像,对于较大时空尺度上侵蚀沟分布格局变化的研究很少报道。本文选择克拜东部地区作为典型区,以1965年的美国高分辨率侦察卫星Corona影像和2005年的Spot-5卫星影像为主要数据源,结合野外实地调查,建立了黑土区侵蚀沟的遥感解译标志,阐述了不同类型侵蚀沟的遥感影像特征,通过对遥感影像的人机交互解译,获取了克拜东部地区1965年和2005年两个时期的侵蚀沟分布图,在此基础上,探讨了1965年以来克拜东部黑土区侵蚀沟分布的格局变化和区域差异。研究结果表明:近40年来克拜东部侵蚀沟密度高值区范围不断扩大,且呈集中连片分布趋势;沿通垦河分水岭两侧受地貌发育自然过程的影响,侵蚀沟密度变化存在明显的东西差异;土地利用方式的转变是促成侵蚀沟形成的重要因素,特别是林地向耕地和草地的转化过程中,侵蚀沟密度迅速增加。

Corona Mortis血管解剖学研究及其临床意义

目的:探讨闭孔血管和髂外血管在腹股沟区的分支,为减少髂腹股沟入路术中出血提供解剖学基础。方法:对25具新鲜中国成人尸体标本共50侧半骨盆进行解剖学研究,观测闭孔血管和髂外血管在腹股沟区的分支及其吻合支(CoronaMortis血管)的大小、出现率、吻合血管行径和吻合血管至耻骨联合的距离。结果:72%(36侧)耻骨上支表面至少存在1条血管吻合支,其中28%(14侧)存在2条或3条血管吻合支,24%(12侧)同时存在动脉吻合支和静脉吻合支。耻骨上支表面的血管吻合支平均直径2.6mm(2.0～4.2mm)。血管吻合支紧贴耻骨上支或髂耻隆起,几乎垂直地下行于髋臼窝壁或耻骨支后方,经闭膜管出盆腔,血管吻合支与耻骨联合的平均距离52mm(38～68mm)。在此区域手术以及髋臼或骨盆前环骨折极易损伤CoronaMortis血管。结论:闭孔血管和髂外血管的吻合支较粗,出现率高,位于耻骨上支表面。髂腹股沟手术入路应特别注意CoronaMortis血管的存在。

一些与圈图构成的Corona图的b-染色

图G的一个(k)b-染色是一个正常k染色,且满足在每一个色类中至少存在一个顶点,使得该顶点与其他每个色类中至少一个顶点是邻接的.图G的b-染色数用b(G)来表示,b(G)为最大的正整数k,且用k种颜色能够对G进行b-染色.对于任意的k:χ(G)≤k≤b(G),若用k种颜色能对图G进行b-染色,称图G是b-连续.通过设计具体b-染色方案,研究了Corona图CnoPm、CnoK1,m以及CnoWm+1的m-度与b-染色数,且证明这些图都是b-连续的.

基于CORONA影像的浅层地层信息定量提取

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.

一些特殊Corona图的b-连续性

图G的b-染色是一个正常顶点染色,且在每两个色类之间至少存在一条边.图G的b-染色数是最大的整数k,满足用k种颜色能对G进行b-染色,记为b(G).一个图G称为b-连续的当且仅当对于每个正整数k,χ(G)≤k≤b(G),图G存在一个(k)b-染色.本文根据Corona图的结构性质,通过设计具体染色方案的方法,证明了一些特殊Corona图的b-连续性.

Corona图P_nｏF_(1,m)、C_nｏC_m与C_nｏF_(1,m)的b-染色数

在图G=(V,E)的一个正常染色{V_1,V_2,…,V_k}中,若i,j,1≤i≠j≤k,■u∈V_i,v∈V_j,使得uv∈E,称该染色为b-染色.令b(G)=max{k|V_1,V_2,…,V_k:i,j,1≤i≠j≤k,■u∈V_i,v∈V_j,uv∈E},称b(G)为图G的b-染色数.一个图G是b-连续的,如果k:χ(G)≤k≤b(G),用k种颜色可实现对G进行b-染色.通过构造特殊染色方案,研究了Corona图P_noF_(1,m)、C_noC_m与CnoF_(1,m)的b-染色数与b-连续性.

几类Corona图的b-染色数

设{V_1,V_2,···,V_k}为图G=(V,E)的一个正常顶点染色,满足对任意的i,j:1≤i≠j≤k,存在于u∈V_i,v∈V_j,使得uv∈E,称该点染色为G的一个b-染色.一个图G的b-染色数是最大的整数k,满足用k种颜色能对G进行b-染色,用b(G)来表示.如果对任意的k:χ(G)≤k≤b(G),图G都存在一个(k)b-染色{V_1,V_2,···,V_k},称G是b-连续的.根据Corona图的结构特点,设计循环染色方案,通过对Corona图中两种类型的顶点进行循环染色,得出几类Corona图的b-染色数等于其m-度,且这些Corona图满足b-连续性.

基于CoroNa^(TM) Green检测细胞内Na^+浓度的流式细胞术分析方法的建立和评价

目的:建立并评价以CoroNa Green检测细胞内Na+含量变化的流式细胞术方法。方法:完全生长培养基培养的H9c2心肌细胞分别给予Na+通道阻断剂TTX(最终作用浓度分别为10、50 nmol/L)和Na+通道激动剂Veratridine(最终作用浓度分别为5、10μmol/L),加CoroNa Green后用流式细胞仪对其信号进行检测;H9c2心肌细胞在含有NaCl(最终作用浓度分别为25、50、100、150 mmol/L)的完全生长培养基中培养24 h,加CoroNa Green后用流式细胞仪对其信号进行检测。结果:与阳性对照组相比,等渗状态给予Na+通道阻断剂TTX大于10 nmol/L时胞内荧光信号强度明显减少(P<0.05),而Na+通道激动剂Veratridine对胞内荧光信号强度无明显影响(P>0.05);在高渗状态下,随着NaCl浓度的增高,细胞内荧光信号明显增强(P<0.05),提示Na+内流明显增多。结论:CoroNa Green作为新型的荧光Na+指示剂,与流式细胞术结合,可以简便、有效的检测细胞内游离Na+含量。

A novel simulation method for positive corona current pulses

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.

On the error analyses of polarization measurements of the white-light coronagraph aboard ASO-S

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.

The detailed characteristics of positive corona current pulses in the line-to-plane electrodes

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.

A-Spectra and Q-Spectra of Two Classes of Corona Graphs

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.