Analysis of the 9th November 1990 flare

In this paper we present complete two-dimensional measurements of the observed brightness of the 9th November 1990Hα flare, using a PDS microdensitometer scanner and image processing software MIDAS. The resulting isophotal contour maps, were used to describe morphological-cum-temporal behaviour of the flare and also the kernels of the flare. Correlation of theHα flare with SXR and MW radiations were also studied.     

The role of non-thermal electrons in the optical continuum of stellar flares

The continuum emission of stellar flares in UV and visible bands can be enhanced by two or even three orders of magnitude relative to the quiescent level and is usually characterized by a blue colour. It is difficult for thermal atmospheric models to reproduce all these spectral features. If the flaring process involves the acceleration of energetic electrons which then precipitate downwards to heat the lower atmosphere, collisional excitation and ionization of ambient hydrogen atoms by these non-thermal electrons could be important in powering the continuum emission. To explore such a possibility, we compute the continuum spectra from an atmospheric model for a dMe star, AD Leo, at its quiescent state, when considering the non-thermal effects by precipitating electron beams. The results show that if the electron beam has an energy flux large enough (for example, ℱ₁∼10¹² erg cm⁻² s⁻¹), the U -band brightening and, in particular, the U − B colour are roughly comparable with observed values for a typical large flare. Moreover, for electron beams with a moderate energy flux ℱ₁≲10¹¹ erg cm⁻² s⁻¹, a decrease of the emission at the Paschen continuum appears. This can explain at least partly the continuum dimming observed in some stellar flares. Adopting an atmospheric model for the flaring state can further raise the continuum flux, but it yields a spectral colour incomparable with observations. This implies that the non-thermal effects may play the chief role in powering the continuum emission in some stellar flares.     

通辽地区风力发电机组综合防雷的探讨

风电的风力发电机防雷需重点解决叶片、机舱、发电机、电气部分、控制系统等雷电防护问题。针对这些不同的需要保护设备,对风力发电机防雷综合防护做简单探讨。     

人工消除冷雾的个例模拟分析

本文在中尺度数值模式MM5的Reisner2方案中引入了液氮粒子与云相互作用的过程,在中尺度模式MM5中实现了催化功能.利用加人催化方案的中尺度模式针对2007年12月26日北京地区的一次冷雾天气过程进行了消雾的数值模拟研究,探讨了消雾的效果和机理,并针对催化剂的播撒量和播撒位置进行了两组敏感性试验.结果表明:在此次模...     

基于多变量非线性DAE子系统模型的同步发电机励磁汽门综合控制

同步发电机励磁汽门综合控制由多变量非线性DAE子系统模型来描述.本文扩展了非线性常微分方程系统的反步控制方法,研究了其镇定控制问题.首先若被控系统的向量相对阶存在,那么可通过一个微分同胚和反馈控制实现系统的解耦和等价转化.然后基于等价系统,利用反步方法设计其镇定控制器,使得整个闭环系统渐近稳定.最后基于MATLAB进行了仿真,仿真结果验证了本文所提方法的有效性.     

Airborne measurements of the impact of ground-based glaciogenic cloud seeding on orographic precipitation

Data from in situ probes and a vertically-pointing mm-wave Doppler radar aboard a research aircraft are used to study the cloud microphysical effect of glaciogenic seeding of cold-season orographic clouds. A previous study (Geerts et al., 2010) has shown that radar reflectivity tends to be higher during seeding periods in a shallow layer above the ground downwind of ground-based silver iodide (AgI) nuclei generators. This finding is based on seven flights, conducted over a mountain in Wyoming (the Unites States), each with a no-seeding period followed by a seeding period. In order to assess this impact, geographically fixed flight tracks were flown over a target mountain, both upwind and downwind of the AgI generators. This paper examines data from the same flights for further evidence of the cloud seeding impact. Composite radar data show that the low-level reflectivity increase is best defined upwind of the mountain crest and downwind of the point where the cloud base intersects the terrain. The main argument that this increase can be attributed to AgI seeding is that it is confined to a shallow layer near the ground where the flow is turbulent. Yet during two flights when clouds were cumuliform and coherent updrafts to flight level were recorded by the radar, the seeding impact was evident in the flight-level updrafts (about 610 m above the mountain peak) as a significant increase in the ice crystal concentration in all size bins. The seeding effect appears short-lived as it is not apparent just downwind of the crest.     

基于CPLD的高精度可调脉冲信号发生器研制

为满足精密时间间隔测量设备的测试需要,研制了一种时间间隔可调的高精度脉冲信号发生器。利用计算机串口控制的方式,结合复杂可编程逻辑器件（CPLD）集成度高、可靠性好及工作速度快的优点,采用A1tera公司的设计软件QuartusII进行设计仿真及实现。仿真与实测实验表明,该脉冲信号发生器不仅可以产生单路可调脉冲信号,而且能产生多路可调脉冲信号,产生的单路秒脉冲信号的1s取样Allan方差为1．84×10^-11;产生的时间间隔为100ns的多路脉冲信号的1s取样Allan方差为2．36×10^-11,2路信号之间的时间间隔数据系列的峰一峰值为101ps,可以满足多通道时间间隔测量设备测试要求的稳定度与准确度。     

人工影响天气飞机播云作业有效催化范围的模拟评估

针对人工影响天气飞机播云作业效果评估需求,提出一种基于拉格朗日粒子扩散模式FLEXPART-WRF的催化剂催化范围模拟评估方法.以典型催化剂碘化银为例,开发催化剂物理化学特性参数清单模块,结合飞机播云特点和模式源项特点,将飞机不规则线性播撒方式离散化为连续移动点源播撒方式,实现模式对飞机播云的模拟能力.通过对一次飞机播云作业的模拟试验,证实了模拟评估方法的可行性和有效性.     

Extensive serendipitous X-ray coverage of a flare star with ROSAT

We report the serendipitous discovery of a flare star observed with the ROSAT X-ray observatory. From optical spectra, which show strong and variable emission lines of the hydrogen Balmer series and neutral helium, we classify this object as a M3.0Ve star, and estimate a distance of 52 pc from published photometry. Owing to the close proximity of the star (13.6 arcmin) to the calibration source and RS CVn binary AR Lacertae, long-term X-ray coverage is available in the ROSAT archive (∼50 h spanning 6.5 yr). Two large flare events occurred early in the mission (1990 June–July), and the end of a third flare was detected in 1996 June. One flare, observed with the Position Sensitive Proportional Counter (PSPC), had a peak luminosity L _X=1.1×10³⁰ erg s⁻¹, an e-folding rise time of 2.2 h and a decay time of 7 h. This decay time is one of the longest detected on a dMe star, providing evidence for the possibility of additional heating during the decay phase. A large High Resolution Imager (HRI) flare (peak L _X=2.9×10³⁰ erg s⁻¹) is also studied. The 'background' X-ray emission is also variable – evidence for low-level flaring or microflaring. We find that 59 per cent of the HRI counts and 68 per cent of the PSPC counts are caused by flares. At least 41 per cent of the HRI exposure time and 47 per cent of the PSPC are affected by detectable flare enhancement.     

Solar Energetic Particle Event of 2005 January 20： Release Times and Possible Sources

Based on cosmic ray data obtained by neutron monitors at the Earth's surface, and data on near-relativistic electrons measured by the WIND satellite, as well as on solar X-ray and radio burst data, the solar energetic particle (SEP) event of 2005 January 20 is studied. The results show that this event is a mixed event where the flare is dominant in the acceleration of the SEPs, the interplanetary shock accelerates mainly solar protons with energies below 130 MeV, while the relativistic protons are only accelerated by the solar flare. The interplanetary shock had an obvious acceleration effect on relativistic electrons with energies greater than 2 MeV. It was found that the solar release time for the relativistic protons was about 06:41 UT, while that for the near-relativistic electrons was about 06:39 UT. The latter turned out to be about 2 min later than the onset time of the interplanetary type III burst.