Coronal Heating by Magnetic Explosions

From magnetic fields and coronal heating observed in flares, active regions, quiet regions, and coronal holes, we propose that exploding sheared core magnetic fields are the drivers of most of the dynamics and heating of the solar atmosphere, ranging from the largest and most powerful coronal mass ejections and flares, to the vigorous microflaring and coronal heating in active regions, to a multitude of fine-scale explosive events in the magnetic network, driving microflares, spicules, global coronal heating, and, consequently, the solar wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

Strong geomagnetic activity forecast by neural networks under dominant southern orientation of the interplanetary magnetic field

The paper deals with the relation of the southern orientation of the north–south component _Bz$B_z$ of the interplanetary magnetic field to geomagnetic activity (GA) and subsequently a method is suggested of using the found facts to forecast potentially dangerous high GA. We have found that on a day with very high GA hourly averages of _Bz$B_z$ with a negative sign occur at least 16 times in typical cases. Since it is very difficult to estimate the orientation of _Bz$B_z$ in the immediate vicinity of the Earth one day or even a few days in advance, we have suggested using a neural-network model, which assumes the worse of the possibilities to forecast the danger of high GA – the dominant southern orientation of the interplanetary magnetic field. The input quantities of the proposed model were information about X-ray flares, type II and IV radio bursts as well as information about coronal mass ejections (CME). In comparing the GA forecasts with observations, we obtain values of the Hanssen–Kuiper skill score ranging from 0.463 to 0.727, which are usual values for similar forecasts of space weather. The proposed model provides forecasts of potentially dangerous high geomagnetic activity should the interplanetary CME (ICME), the originator of geomagnetic storms, hit the Earth under the most unfavorable configuration of cosmic magnetic fields. We cannot know in advance whether the unfavorable configuration is going to occur or not; we just know that it will occur with the probability of 31%.     

地磁Ap指数滞后太阳周循环分析

把1932-2006年地磁Ap指数12个月流动均值分解成为(Ap)R和(Ap)I.其中(Ap)R为太阳黑子数R的线性函数,与太阳黑子数R相位相同,可能对应于日冕物质抛射(CME)等地磁控制因素. (Ap)I分量与太阳黑子数R相位相差约180°,该分量可能对应于极冕洞变化(从太阳峰年开始,由日面极区逐渐向赤道延伸).以地磁Ap指数与太阳黑子数R滞后非常严重的第20太阳周为例,证实了(Ap)I分量与极冕洞向赤道延伸循环变化相对应.因此极冕洞循环变化可能是导致地磁扰动指数与太阳周循环相位不一致,出现滞后现象的一个十分重要原因.      

肋角度和出流孔位置对流动特性的影响

针对带肋和双排出流孔通道,研究了肋角度和出流孔位置对流量系数分布和总压系数分布的影响.研究的肋角度为60°,90°和120°.出流孔分别位于相邻两肋之间距前肋1/4肋距、两肋中间、距后肋1/4肋距.研究表明:不同的肋角度和出流孔位置不改变流量系数和总压系数沿流向的分布规律;流量系数随肋角度增大而增大;60°和120°肋通道中总压系数绝对值接近且小于90°肋通道中的绝对值;两肋之间,出流孔位置靠近下游,将使流量系数增大,总压系数绝对值增大.      

基于流动控制的水下航行体流体动力特性分析

利用CFX对水下航行体流体动力特性进行了数值模拟研究.求解了混合介质的剪切压力输运湍流模型控制方程、雷诺-平均奈维尔-斯托克斯方程以及各相间的质量输运方程,采用三维数值模拟方法对比分析了不同流动控制方案的水下航行体空泡形态特征、表面压力分布和阻力系数变化特性,讨论了不同参数对减阻效果的影响.结果表明,对于有横流作用的水下垂直发射航行体,多相流动控制不仅可以降低通气空泡的不对称性和航行体阻力,同时可以均匀迎流面和背流面压力,从而实现航行体多相流空泡形态及表面压力特性等的控制.此外,通气口的位置对减阻效果具有显著影响.      

扩展型面排孔气膜冷却的实验研究

本文设计了三种型面的气膜孔扩展结构,研究了气膜冷却效率、壁面换热系数及流量系数随吹风比的变化规律。研究结果表明,与典型的圆柱形气膜孔相比,有后向扩展型面的气膜孔具有相对较高的冷却效率和换热系数,流量系数略有降低。扩展型面的流向扩展角α对冷却效率和换热系数的影响大于侧向扩展角 的影响。侧向扩展角 只在特定吹风比下才对提高气膜的侧向覆盖率、进而提高气膜冷却效率起作用,它使得位于二次流出流下游的低压区域范围增大,流量系数减小。     

Geoeffectivity of Coronal Mass Ejections

Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour high-latitude activity.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

高温下DD6单晶气冷叶片模拟试样拉伸性能试验

通过选晶法制备DD6单晶薄壁圆管模拟试样,对850℃和980℃两种温度下[001]晶体取向含与不含气膜孔的薄壁试管进行拉伸性能试验研究.结果表明:在850℃条件下,[001]取向含气膜孔的拉伸性能比[001]取向不含气膜孔的拉伸性能降低10.5%;在980℃条件下,[001]取向含气膜孔的拉伸性能与[001]取向不含气膜孔的拉伸性能水平相当,这表明温度越高,气膜孔对薄壁件拉伸性能的影响越不显著;但在980℃ 条件下,[001]取向通气状态的拉伸强度比不通气状态下的拉伸强度提高16%.同时,发现圆管表面状态及通气状态是影响单晶薄壁试样高温性能的重要因素,特别是通气状态的存在显著提高了其高温力学性能.      

喷嘴匹配方案及火焰筒开孔对燃烧室性能影响的试验研究

基于航空发动机主燃烧室扇形试验,针对点火喷嘴特性以及火焰筒大孔射流的改变对主燃烧室性能的改善情况进行了研究。试验中进行了点火用喷嘴匹配方案对燃烧室熄火性能,以及火焰筒大孔面积变化对燃烧室贫油熄火、燃烧效率和出口温度场性能影响的研究。研究结果表明：在供油系统设计中采用放大型点火喷嘴可改善主燃烧室贫油熄火性能;增大火焰筒主燃孔的面积可提高燃烧室的燃烧效率,改善出口温度场分布,而贫油熄火特性将变差;增大掺混孔的面积可提高燃烧室的燃烧效率,改善出口温度场分布,拓宽燃烧室的熄火动界．