Spartan 201 white light coronagraph experiment

A white light coronagraph was launched into orbit aboard the space shuttle OV 103 (Discovery) on 7 April 1993. This device was one of two instruments included in the SPARTAN 201-1 payload, a completely autonomous sub-satellite deployed from the shuttle for a period of about 47 hours. The WLC system is an externally occulted coronagraph system which incorporates a rotating half-wave plate polarimeter, and the image data is used to infer the brightness, the polarized brightness and the degree of polarization of the white light emission from the solar corona. These data are in turn used to infer estimates of the K- and F-coronal brightnesses and density distributions. We shall present preliminary results of the electron density estimate in the coronal streamer and hole region and describe the methods employed.affiliated to USRA     

Radial profile measurements of the solar wind speed using radio sounding techniques

Velocity measurements of the solar wind in the region of its acceleration were carried out in 1984 with Venera Orbiters using the following specific radio sounding techniques: (i) phase and frequency correlations from two or three widely-spaced ground stations; (ii) phase and frequency correlations from two spacecraft and two widely-spaced ground stations; (iii) two station two-way coherent Doppler measurements; (iv) determination of the break frequency in power spectra of intensity fluctuations. Our results are substantially lower than those derived from direct Doppler shift measurements of transition region and lower coronal resonance lines and those from measurements applying the Doppler dimming technique.     

Probing solar and stellar interior dynamics and dynamo

Solar and stellar activity is a result of complex interaction between magnetic field, turbulent convection and differential rotation in a star’s interior. Magnetic field is believed to be generated by a dynamo process in the convection zone. It emerges on the surface forming sunspots and starspots. Localization of the magnetic spots and their evolution with the activity cycle is determined by large-scale interior flows. Thus, the internal dynamics of the Sun and other stars hold the key to understanding the dynamo mechanism and activity cycles. Recently, significant progress has been made for modeling magnetohydrodynamics of the stellar interiors and probing the internal rotation and large-scale dynamics of the Sun by helioseismology. Also, asteroseismology is beginning to probe interiors of distant stars. I review key achievements and challenges in our quest to understand the basic mechanisms of solar and stellar activity.     

高分影像辅助下的航空高光谱严密几何检校方法

 惯性测量单元(IMU)与传感器视准轴的偏心角和偏心矢量是造成航空线阵列高光谱数据几何校正误差的主要原因之一。在分析偏心角与偏心矢量误差来源之后提出该误差由IMU主轴与传感器主轴的角度偏差、测区固定偏差、GPS中心与传感器投影中心相对偏差组成,在此基础上建立了较为严密的检校模型。针对模型解算时需要大量高精度控制点的问题,提出了一种高分影像辅助下的亚像元精度控制点自动提取方法。通过多地区、多传感器高光谱航测实验表明,亚像元精度控制点能有效提高模型解算精度。新检校模型可获得亚像元校正精度,推扫式传感器——应用型机载成像光谱仪(AISA)建模中误差约为0.39个像元,摆扫式传感器——实用型模块化成像光谱仪(OMIS)建模中误差约为0.23个像元,校正后的影像可直接进行拼接。     

基于等效理论的蜂窝夹层板强度等效分析

通过采用三明治夹芯板等效方法计算,得到了等效物理参数,建立了三明治夹芯蜂窝板的有限元模型,完成了蜂窝夹层板模型的静力分析和随机振动分析,并对试验样机进行了静力与随机振动分析和试验验证。结果表明:基于三明治夹芯板等效理论建立的有限元模型能够准确反映蜂窝夹层板的静强度特性和结构动特性,静力应变值结果误差小于4%,振动固有频率结果误差小于5%,偏差较小,表明所建模型合理、准确。     

基于连续同伦算法的天基仅测角初定轨方法

要进一步提高天基短弧初定轨的精度,在观测资料精度较高的情况下,仅考虑二体问题是不够的,还应考虑轨道摄动的影响。因此,基于无摄初轨的单位矢量法原理和矢量斜分解方法,给出了考虑摄动的天基仅测角初定轨单位矢量法。针对天基仅测角观测条件方程组求解过程中易出现迭代不收敛或收敛到平凡解的问题,引入连续同伦算法求解观测条件方程组,提出了单星观测方式下的空间目标天基仅测角初定轨方法,并通过数值仿真算例验证了该算法在较大范围的收敛性和数值稳定性。     

The Seed Population for Energetic Particles Accelerated by CME-Driven Shocks

Understanding properties of solar energetic particle (SEP) events associated with coronal mass ejections has been identified as a key problem in solar-terrestrial physics. Although recent CME shock acceleration models are highly promising, detailed agreement between theoretical predictions and observations has remained elusive. Recent observations from ACE have shown substantial enrichments in the abundances of ³He and He⁺ ions which are extremely rare in the thermal solar wind plasma. Consequently, these ions act as tracers of their source material, i.e., ³He ions are flare suprathermals and He⁺ ions are interstellar pickup ions. The average heavy ion composition also exhibits unsystematic differences when compared with the solar wind values, but correlates significantly with the ambient suprathermal material abundances. Taken together these results provide compelling evidence that CME-driven shocks draw their source material from the ubiquitous but largely unexplored suprathermal tail rather than from the more abundant solar wind peak. However, the suprathermal energy regime has many more contributors and exhibits much larger variability than the solar wind, and as such needs to be investigated more thoroughly. Answers to fundamental new questions regarding the preferred injection of the suprathermal ions, the spatial and temporal dependence of the various sources, and the causes of their variability and their effects on the SEP properties are needed to improve agreement between the simulations and observations.     

时域有限体积法的格式稳定性分析

以模型方程为例,采用MUSCL插值的S-W通量分裂格式,分别结合二步、四步龙格一库塔时间推进格式建立数值求解方法.用Von Neumann傅里叶级数分析方法,通过对不同格式的放大因子及色散因子的计算,分析了时域有限体积法(FVTD)格式的稳定性.     

Jets and brightenings generated by energy deposition in the middle and upper solar chromosphere

Numerical simulations of energy depositions in the middle and upper solar chromosphere result in ejection of chromospheric material into the corona and heating of the chromospheric gas. These simulations may be capable of describing some of the features seen by the soft X-ray telescope on board theYohkoh satellite.     

TVC/PSM飞机的过失速动态边界及敏捷性分析

以飞机为质点，考虑在最少输入数据情况下，曲于转弯速率图并从能量的角度计算和分析了TVC/PSM飞机的过失速动态边界，选取敏捷性尺度空战周期时间和指向裕度，对比分析了TVC/PSM飞机和传统飞机的敏捷性，得出了一些有益的结论，并提出了一些建议。