A first step towards proton flux forecasting

We present a preliminary version of a potential tool for real time proton flux prediction which provides proton flux profiles and cumulative fluence profiles at 0.5 and 2 MeV of solar energetic particle events, from their onset up to the arrival of the interplanetary shock at the spacecraft position (located at 1 or 0.4 AU). Based on the proton transportation model by Lario et al. [Lario, D., Sanahuja, B., Heras, A.M. Energetic particle events: efficiency of interplanetary shocks as 50 keV E < 100 MeV proton accelerators. Astrophys. J. 509, 415–434, 1998] and the magnetohydrodynamic shock propagation model of Wu et al. [Wu, S.T., Dryer, M., Han, S.M. Non-planar MHD model for solar flare-generated disturbances in the Heliospheric equatorial plane. Sol. Phys. 84, 395–418, 1983], we have generated a database containing “synthetic” profiles of the proton fluxes and cumulative fluences of 384 solar energetic particle events. We are currently validating the applicability of this code for space weather forecasting by comparing the resulting “synthetic” flux profiles with those of several real events.     

太阳风质子束流的演化

太阳神飞船观测表明，太阳风高速流中质子束分量相对于核分量的密度随日心距离增加而增加．提出解释这一观测现象的机理并给出二维数值模拟结果．由于阿尔芬波速随日心距离增加而减少，第二支左旋波将与更多的质子共振，把部分原来属于核分布的质子拉到束分布中来．用数值模拟方程方法求解回旋波共振导致的准线性扩散方程，数值结果与观测结果相符合．     

地磁急始年发生数周期特征的小波分析

采用小波分析方法分析了急始年发生数的时间序列的周期特征，并对急始发生数的特征与太阳黑子相对数的特征进行了简要的对照分析，分析结果表明，急始发生数的周期规律与太阳黑子相对数的周期规律是有差异的．还进行了太阳黑子相对数与急始数的相关性，太阳黑子相对数与急始磁暴的相关性研究，分析结果表明它们之间显著相关．还对急始数与急始磁暴致以及其他的一些参数之间的相关性进行了分析，最后对分析结果进行了讨论．     

1989年3月太阳活动引起的强烈磁暴群

本文分析了1989年3月上旬一个太阳超级活动区中多次特大耀斑引起的强磁暴群.联系源耀斑的等级、位置等讨论了磁暴形态特征.随着耀斑活动区位置由东向西旋转,磁暴的形态呈现有规律的变化,充分显示了磁暴形态特征有依赖于耀斑位置的中心子午线效应和东西不对称性.     

Transition region line-shifts in the rebound shock spicule model

Spectral emission lines created in the solar chromosphere — corona transition region show net red-shifts. It has been proposed that this may be the result of the return of spicular material. We simulate a spicule numerically using the rebound shock model and find that the resulting hydrodynamic evolution leads to a perceived up-flow in transition region spectral lines even though the average velocity in the line forming region is directed downward. The explanation for this apparent paradox is found in the correlation between density and velocity in the waves generated by the rebound shock spicule.     

Phase Space Density Analysis of Energy Transport in the Earth’s Magnetotail

Two energetic events in the Earth’s magnetotail detected by Geotail are examined with detailed analysis of three-dimensional velocity phase space density. It is found that the occurrence of multiple ion components is high during these dynamic episodes. Different populations evolve independently of each other, suggesting particles from multiple activity sites contributing to the observed phase space density. The transport properties with consideration of multiple components are evaluated, with the result showing significant differences from those based on a single fluid approach. This comparison indicates that precise evaluation of the energy and magnetic flux transport of energetic events in the magnetotail requires resolving individual populations in the phase space density.     

利用非交错对称矩阵构造Cartesian认证码

利用特征为2的有限域上非交错对称矩阵构造了一个Cartesian认证码，并计算出其参数。进而，假定编码规则按照均匀的概率分布所选取，计算出了该码被模仿攻击成功的最大概率只和被替换攻击成功的最大概率Ps。     

300M钢纯洁度磁粉检验磁痕现象的分析

采用交、直流磁粉检验并结合金相试验、电子探针试验及微量元素含量分析的方法，对３００Ｍ钢磁痕现象的本质进行了分析。结果表明，采用磁粉检验方法对航空优质钢进行纯洁度检验是可信的。     

超音速斜板进气道侧向溢流估算

 本文采用超音速线化理论,算出斜板侧缘附近干扰区内的流场,并根据流量积分方法,导出了关于流量系数的侧向溢流公式。本文还根据Busemann锥型流理论,应用Carafoli方法,得出了估算侧后掠端板影响的方法和图线。理论计算结果与现有的实验数据作了比较,符合程度很好。     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.