High resolution UV solar spectroscopy

The advantages of high resolution UV spectroscopy for the investigation of the solar atmosphere are stressed while the limitations in the areas of instrumentation and diagnosis are discussed. The recent achievements (made essentially by Skylab, OSO-8 and rocket instruments) are reviewed and discussed.It is shown that high resolution UV solar spectroscopy has improved our knowledge of the dynamics of the upper layers of the solar atmosphere. Within the present instrument capabilities the birth of coronal expansion is shown to take place at the top of the transition region. The existence of downward flows over the bright regions of the network is evidenced from redshifts or transition region and chromospheric optically thin lines: velocities as large as 22 km s^-1 have been measured in O vi. Short period waves (95 s) have been detected in lines of Si ii at chromospheric levels in addition to the well known 300s and 180 s photospheric and chromospheric oscillations. There is strong evidence that optically thin chromospheric and transition region lines are broadened by a nonthermal velocity component which is maximum at 1.3 × 10⁵ K and decreases at higher temperatures. This may indicate the presence of unresolved acoustic or magnetohydrodynamic waves so oftenly set fourth as the source of chromospheric and coronal heating.Contradictions between the various results are pointed out and discussed. They might be attributed to the different angular resolution of the instruments, a key parameter for future space observations. It is suggested that the Solar Optical Telescope (SOT) and the Grazing Incidence Solar Telescope (GRIST) which are presently under phase A studies at NASA and ESA be considered as a tandem of instruments to fly on Spacelab in the 1980's. Both their angular and spectral resolution appear sufficient to resolve most of the problems under discussion today.Review presented at the Vth Conference on UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, London, July 4–7, 1977.     

Stellar coronae—Evidence for their existence from X- and UV observations

Stellar coronae were among the first predicted X-ray sources. Because of their relatively low X-ray luminosities, however, they have been discovered only during the last few years.In the present paper the current state of stellar coronal X- and UV observations has been reviewed, including some preliminary observational results from the HEAO-1 and IUE satellites, but still without any result from the recently launched X-ray satellite HEAO-2.Late 1978 about two dozens of stellar soft X-ray sources have been detected, e.g., normal stars like the Sun (e.g., Cen), very active stars (RS CVn systems), and possibly a corona around an intermediately hot white dwarf (Sirius B).The observational results of various objects have been discussed and compared with X-ray luminosity predictions based on minimum-flux coronal models.     

UV spectral lines from coronal transients

We investigated the UV emission expected from solar coronal transients, selecting some spectral lines which will be observed with the UVCS spectrocoronagraph onboard the SOHO spacecraft. The line intensities were calculated starting from a representative, simplified model of coronal transient. We discuss how the considered intensities depend on the physical parameters of the examined structures. This work is aimed to give a contribution in defining and preparing the future observations of coronal transients and coronal mass ejections by the UVCS/SOHO.     

一种可紫外光固化新型耐烧蚀涂料研究

基于巯基-乙烯基光引发逐步聚合机理,以含有乙烯基的液态硅氮烷预聚物与多元巯基化舍物为基体,辅以某种陶瓷微粉作为填料,研制了一种可紫外光固化的新型耐烧蚀涂料.采用等温差示光量热扫描(DPC)和测试固化度研究了填料添加量对紫外光固化放热行为和一次成型厚度的影响关系.结果表明:在制备0.5 mm厚的涂层时,填料添加量逐渐从0增至5%(质量分数,下同),固化放热峰值和放热量随添加量的增大而逐渐减小,且固化放热峰从尖锐逐渐趋于平坦,这是由于填料的加入使得涂料变为不透明,对入射的紫外光线产生了衍射/反射作用,从而减弱了辐照强度;填料添加量大于10%时,明显阻碍光固化反应的发生,涂层的一次成型厚度随填料添加量的增加而降低,可采用多次涂敷的措施解决涂层厚度不足的问题.当填料添加量从0增至20%,对于1.0 mm厚的涂层而言,在800℃质量保持率从61.2%增至73.5%.填料含量20%的涂层具有较为优异的耐烧蚀性能,氧-乙炔烧蚀的线烧蚀率为0.252 inm/s,质量烧蚀率为61.7 mg/s.     

UV studies and the solar wind

The solar wind carves a cavity in the flow of interstellar H atoms through the solar system by charge-exchange ionization. The resulting Ly- sky pattern depends on the latitude distribution of the solar wind flux and velocity. We review how the solar wind characteristics (mass flux latitude distribution) can be retrieved from Ly- observations, yielding a new remote sensing method of solar wind studies, through UV optical measurements.     

Hierarchy of spatial scales in UV prominences

Ultraviolet spectra of a quiescent prominence observed with theHigh Resolution Telescope and Spectrograph (HRTS) are analyzed. Different techniques lead to greatly different spatial scales for the prominence structures. The UV spectra show strong variations in intensity and Doppler shift on scales larger than 1700 km. Spectroscopic diagnostics employing line intensity ratios indicate the existence of scales between 400 m to some hundred kilometers. We attempt to interpret various aspects of the prominence intensities and velocities with a multiple thread model.     

Optical and UV Diagnostics of Supernova Remnant Shocks

The relatively faint optical and UV emission from non-radiative shock waves provides diagnostics for processes related to cosmic ray acceleration in collisionless shocks. Emission line profiles and intensities can be used to determine the efficiencies of electron-ion and ion-ion thermal equilibration, which influence the population of fast particles injected into the acceleration process. It is found that T _e/T _p declines with shock speed and that T _i is roughly proportional to mass in fast shocks. Important information about cosmic ray precursors may be available, but the interpretation is still somewhat ambiguous. The compression ratios in shocks which efficiently accelerate cosmic rays are predicted to be substantially larger than the factor of 4 expected for a strong shock in a = 5/3 perfect gas, and some limits may be available from observations.     

原位光固化复合材料纤维铺放制造工艺

通过调整紫外光参数和铺放速度参数,制备了相应的NOL环测试件和层合板样件。研究结果表明紫外光原位固化纤维铺放制造工艺是可行的。复合材料具有比强度高、比模量高、抗疲劳性能和耐腐蚀性能优良等优点。随着复合材料的广泛使用,各种高效低成本的制造方法也不断出现。如纤维铺放成型技术、树脂     

紫外辐照下透明聚氨酯胶片老化机理

针对高端夹层玻璃的老化问题,选用荧光紫外灯,对其主要粘结材料——透明聚氨酯胶片分别进行0/200/300/500 h的照射,借助紫外/可见光分光光度计、傅里叶红外光谱仪、扫描电镜等设备,研究照射过程中材料颜色、结构、微观形貌的变化。扫描电镜显示照射时间延长到500 h,材料表面出现龟裂。实验发现胶片的老化起始于硬段及软段部位与N,O相连的α位置的碳原子,在紫外光及氧气的联合作用下产生氢过氧化物;该过氧化合物一部分继续氧化成CO,一部分通过β分裂,使C—N,C—O键断裂,致使材料龟裂。     

Discussion of the Solar UV/Planetary Wave Mechanism

Of all the suggested mechanisms for solar activity influences on climate, the solar UV/planetary wave mechanism has been investigated most carefully in a manner that allows comparison with observations. Some historical background, the observations, and modeling investigations of this mechanism are briefly discussed in this review so that the following more detailed papers can be put into context.     

MSM结构ZnO紫外探测器的制备及光电性能研究

采用磁控溅射方法,在石英衬底上制备了光电性能优良的ZnO紫外探测器。通过紫外光电性能测试、扫描电子显微镜(SEM)观察及X射线衍射(XRD)分析,研究了ZnO紫外探测器的光电特性。结果表明:探测器的光电流高出暗电流近3个数量级,紫外波段的光响应高出可见光波段近2个数量级,所制备ZnO紫外探测器达到了高辐射灵敏度和可见盲特性的要求。     

WSO／UV（世界空间紫外天文台）的轨道特征与轨道保持

WSOO／UV(世界空间紫外天文台)需要发射到日-地(月)系的共线平动点L1附近进行巡天观测，相对日-地(月)要求其几何位置几乎不变，因此有必要阐明共线平动点的动力学特征及其附近的运动状况。本文基于这一点，对限制性三体模型下，日-地(月)系中共线平动点附近扰动运动的稳定性作了理论分析，给出了WSO／UV轨道保持的条件及其在运行阶段的轨控措施。     

The Effect of Solar UV Irradiance Variations on the Earth's Atmosphere

The response of the lower and middle atmosphere to variations in solar irradiance typical of those observed to take place over the 11-year activity cycle has been investigated. The effects on radiative heating rates of changing total solar irradiance, solar spectral irradiance and two different assumptions concerning stratospheric ozone have been studied with a radiative transfer code. The response in the stratosphere depends on the changes specified in the ozone distribution which is not well known. A general circulation model (GCM) of the atmosphere up to 0.1 mbar (about 65 km) has been used to study the impacts of these changes on the thermodynamical structure. The results in the troposphere are very similar to those reported by Haigh99 using a quite different GCM. In the middle atmosphere the model is able to reproduce quite well the observed seasonal evolution of temperature and wind anomalies. Calculations of radiative forcing due to solar variation are presented. These show that the thermal infrared component of the forcing, due to warming of the stratosphere, is important but suggest a near balance between the longwave and shortwave effects of the increased ozone so that ozone change may not be important for net radiative forcing. However, the structure of the ozone change does affect the detailed temperature response and the spectral composition of the radiation entering the troposphere.     

Solar EUV and UV Emission Line Observations Above a Polar Coronal Hole

The roll manoeuvre of SOHO on September 3, 1997 provided the opportunity to study the northern coronal hole with SUMER slits in east-west orientation, so that polar plumes and inter-plume lanes could be observed simultaneously. A preliminary analysis of the observations shows that lines emitted by ions with the lowest formation temperatures (with the exceptions of Ne⁷⁺ and Ar⁷⁺) have the largest ratios of plume to lane radiances at heights between 35 000 km and 70 000 km above the photosphere. All lines have narrower widths inside plumes than outside. Electron densities have been deduced in plumes and lanes from Si VIII and Mg VIII line radiance ratios. The Mg IX pair was used to determine the corresponding electron temperatures. Neon (with a high first-ionization potential) is found to be less abundant relative to magnesium (with low FIP) in a plume compared to an inter-plume lane, but the variation is smaller than previously determined Ne/Mg abundance ratios in a plume relative to the photosphere. This revised version was published online in June 2006 with corrections to the Cover Date.     

Spectroscopic diagnostics applicable to the UV and EUV spectra of astrophysical sources

A bibliography is provided of the most reliable emission and absorption line ratio diagnostic calculations currently available for application to the spectra of astrophysical sources in the UV and EUV wavelength region (50–3000 Å). References are listed containing diagnostics for species in the Li through P isoelectronic sequences, as well as the iron ions Feii-Fexxiii and nickel ions Nixvii-Nixxv. Also given is the wavelength range for which diagnostic calculations are presented in each reference, along with the type of diagnostic considered. These include, for example, emission line ratios for determining electron temperatures and densities, and absorption line diagnostics for evaluating hydrogen densities.     

自来水中的TOC、UV254和浊度的相关性研究

通过应用回归分析方法,对西安市某水厂的出水、管网中间水和管网末梢水的TOC、UV254和浊度的监测数据进行了相关性分析。结果表明：随着供水管网的延长,浊度和UV254的线性相关系数明显增加;随着供水管网的延长,浊度和TOC的线性相关系数明显降低。