Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

一种考虑结构瞬态互辐射的有限元法

研究结构元件之间瞬态辐射过程及特点 ,对于元件温度未知时的瞬态辐射提出了一种有限元计算模型。通过广义边界条件简化了元件互辐射的数学描述 ,最后得到了广义互辐射元。所建模型具有简单、方便、实用和精度高等特点 ,使复杂的互辐射计算化为统一模式 ,并通过试验与实例计算证明其有效性。     

四并联推力室外向辐射传热对壁温分布的影响

提出了四台对角布置全辐射冷却推力室外向辐射传热的物理模型和数学方程 ,分析此布置形式推力室的热特点。计算表明 ,因推力室之间辐射传热而引起的周向温度畸变 ,主要取决于推力室间的相对间距L/D和单机壁温水平T0 ;周向温度峰值出现位置从喉部的Ψ =0°附近渐变到喷口的Ψ =± 45°处 ,周向壁温分布亦相应地从单峰形态渐变成双峰形态。对仅有两对角推力室工作、另一对推力室不工作时的温度分布特点也作了分析。地面模拟实验证明数值分析结果是正确的     

小突片对热射流红外辐射的影响研究

实验研究了收敛喷管在高温（约913K）、高速（超临界）流动状态下，加装小突片后对热排气的红外辐射抑制特性，并探讨了小突片安装片数、后倾角度、堵塞比等因素对红外辐射抑制特性的影响。结果表明，小突片对热排气的红外辐射具有明显的抑制作用，与不装小突片的相比，不仅使热排气的核心区长度大为缩短，而且使热排气的总体红外辐射信号大幅度下降（在实验范围内，最大可下降约73％）。     

收扩喷管加小突片对尾喷流红外辐射的影响

针对收扩喷管,在高温(约640℃)、高速(超音速)流动状态下,实验研究了加装小突片后对飞机发动机尾喷流红外辐射的抑制效果,并探讨了小突片堵塞比、小突片后倾角度等因素对红外辐射抑制特性的影响。结果表明,小突片对热射流的红外辐射具有明显的抑制作用,不仅使热射流的核心区长度大为缩短,而且使热射流的总体红外辐射信号大幅度下降(在本文实验范围内,最大可下降约57%)。      

带有双层壁扩压器的波瓣喷管混合流场的数值计算

采用三维贴体曲线坐标网格,边界网格加密且正交,在整个计算区域进行全场计算。为避免因波瓣造成的网格强烈的非正交引起解的发散,采用了Chen和Kim修正的k-ε湍流模型及同位网格SIMPLC计算方法,对带有双层壁扩压器的波瓣喷管混合流动进行了数值计算和分析。对波瓣及双层壁,采用大粘性的方法解决流固耦合。计算结果表明:在双层壁间有外界冷气流被引射进入,形成了壁面的冷却气流;自波瓣出口截面沿流向产生的环流速度场,强化了主次流的掺混,速度分布渐趋均匀。计算结果与实验数据符合良好,二者在离开波瓣52 mm的混合管内相对主流速度的最大误差为21.65 %。     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

再入体实验模型热化学非平衡绕流流场的数值分析

利用数值求解一个和多个振动温度热化学非平衡Navier-Stokes方程的CFD计算程序,对爆轰风洞球锥试验模型的热化学非平衡绕流流场进行了数值模拟,分析了分子组分振动温度在全流场(头身部流场和底部流场)中的分布规律.研究结果表明:(1)计算的压力、电子数密度以及流场的光辐射数据与试验数据符合较好;(2)在再入体身部,大多数分子的振动温度峰值大大高于平动温度的峰值;在再入体近尾出现振动温度冻结并大大高于平动温度的现象;CO2的两个振动态的振动温度分布非常接近平动温度分布.     

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.     

涡扇发动机轴对称引射收敛喷管红外辐射特性

数值研究了涡扇发动机轴对称引射收敛喷管的红外辐射特性.排气系统的流场计算采用商用数值模拟软件,红外辐射特性计算采用自主开发的软件NUAA-IR,计算分析了轴对称收敛喷管和引射收敛喷管在3~5μm波段红外辐射特性以及喷管内不同固体壁面在探测方向上的红外辐射贡献.结果表明:引射收敛喷管的红外抑制作用主要在于引射加强了尾喷流与环境大气的掺混,减小了尾喷流的长度,降低了燃气流的红外辐射;引射收敛喷管对喷管内固体壁面的遮挡以及降温作用很小,只在方位角为20°方向上对内涵壁面、外涵内壁等中低温壁面有效;引射收敛喷管的总积分辐射强度在方位角为0°~15°范围内与收敛喷管几乎相等,在其他方位角范围内均小于收敛喷管,且在方位角为40°方向上降低幅度达到最大,约为34%.