等参化FVDAM在复合材料湿热应力分析中的应用

在等参化有限元体积直接平均法（FVDAM）中引入等效湿胀系数,建立了复合材料湿热耦合的细观应力场分析模型。计算了湿热环境中不同纤维体积含量和湿含量复合材料的细观应力场。结果表明：湿热环境中复合材料界面径向应力最大值发生于纤维密集区的相邻纤维间的界面处,最小值出现在基体富区;初始吸湿对热残余应力有释放作用,最终吸湿的影响将超过热残余应力,界面应力状态也随之改变。计算所得细观应力场与有限元（FEM）法有较好的一致性。     

Monopolar structure of the Sun in between polar reversals and in Maunder Minimum

After a polar reversal in one hemisphere the Sun has two polar caps of the same sign, leaving it in a kind of monopolar state. It may take months before a polar reversal occurs in the other hemisphere. The situation may have been extreme in the Maunder Minimum where the northern hemisphere most probably did not have polar reversals during several cycles, while the southern hemisphere may have had some. This may affect the interplanetary field and thus the cosmic rays reaching the Earth. Using the relation between the Wolf number and the speed of the global magnetic field regions the yearly mean Wolf number has to exceed 40 in order to have polar reversals, hence per hemisphere we expect that it must exceed 20. This may be used to give a definition of a deep minimum.     

Variation of energetic particle precipitation with local magnetic time

The detailed study of the precipitation of magnetospheric particles into the atmosphere is complicated by the rather complex spatial configuration of the precipitation region and its variability with geomagnetic activity. In this paper we will introduce polar oval coordinates and apply them to POES observations of 30 keV to 2.5 MeV electrons and comparable protons to illustrate the dependence of particle precipitation on local time and geomagnetic activity. These coordinates also allow an easy separation of the spatial precipitation patterns of solar and magnetospheric particles. The results indicate that (a) the spatial precipitation pattern of energetic magnetospheric electrons basically follows the pattern of the field parallel Birkeland currents up to MeV energies and (b) at least in the mesosphere the influence of magnetospheric electrons is comparable to the one of solar electrons. Implications for modeling of atmospheric chemistry will be sketched.     

New index of long-term variations of galactic cosmic ray intensity

We find that the soft rigidity spectrum of the Galactic Cosmic Ray (GCR) intensity variations for the maximum epoch and the hard rigidity spectrum for the minimum epoch calculated based on the neutron monitors experimental data (1960–2002) are related with the various dependence of the diffusion coefficient on the GCR particle’s rigidity for different epoch of solar activity. This dependence is stronger in the maximum epoch than in the minimum epoch of solar activity, and is provided by the essential temporal rearrangements of the structure of the Interplanetary Magnetic Field (IMF) turbulence from the maxima to minima epoch of solar activity. We also show that the rigidity spectrum of GCR intensity variations is harder for the effective rigidities ∼(10–15) GV (by neutron monitors data), than for the effective rigidities ∼(25–30) GV (by neutron monitors and muon telescopes data). A general scenario of GCR modulation versus solar activity is settled on the essential temporal rearrangements of the structure of the IMF turbulence. Therefore, the temporal changes of the power law rigidity spectrum exponent can be considered as a vital (new) index to explain the 11-year variations of the GCR intensity. We assume that ∼(70–80)% of the changes of the amplitudes of the 11-year variations of GCR intensity is related with the changes of the IMF turbulence versus solar activity.     

Whistler waves in plasmas with time-varying magnetic field: Laboratory investigation

Modulation of whistler waves in a plasma with time-dependant magnetic field perturbations was investigated experimentally. The experiments were performed on large “Krot” device, which was specially designed to study space plasma physics phenomena. It is shown that magnetic field variations on the wave propagation path can lead to splitting of initially continuous whistler wave into the sequence of bursts, whose repetition rate corresponds to magnetic field perturbation period. The frequency inside each burst is changing from its front edge to the back edge. Relative shift of the wave frequency can be as large as the relative magnetic disturbance. Distortion of whistler wave frequency spectrum after its passing through magnetically disturbed areas can be used as a diagnostics for low-frequency magnetic field variations. The applicability of our laboratory results to space plasma is discussed.     

A question raised from the observation of dynamic cusp formation: When and where does particle acceleration occur?

We present observations of a C9.4 flare on 2002 June 2 in EUV (TRACE) and X-rays (RHESSI). The multiwavelength data reveal: (1) the involvement of a quadrupole magnetic configuration; (2) loop expansion and ribbon motion in the pre-impulsive phase; (3) gradual formation of a new compact loop with a long cusp at the top during the impulsive phase of the flare; (4) appearance of a large, twisted loop above the cusp expanding outward immediately after the hard X-ray peak; and (5) X-ray emission observed only from the new compact loop and the cusp. In particular, the gradual formation of an EUV cusp feature is very clear. The observations also reveal the timing of the cusp formation and particle acceleration: most of the impulsive hard X-rays (>25 keV) were emitted before the cusp was seen. This suggests that fast reconnection occurred during the restructuring of the magnetic configuration, resulting in more efficient particle acceleration, while the reconnection slowed after the cusp was completely formed and the magnetic geometry was stabilized. This observation is consistent with the observations obtained with Yohkoh/Soft X-ray Telescope (SXT) that soft X-ray cusp structures only appear after the major impulsive energy release in solar flares. These observations have important implications for the modeling of magnetic reconnection and particle acceleration.     

磁空间群PC 63/mmc的C-G系数计算

在晶体拉曼散射的张量计算中，晶体磁空间群的C-G系数具有重要的作用。利用本征函数法计算了Pc63／mmc磁空间群第一布里渊区中的对称点A之间的C-G系数。     

高新航空武器装备的发展对含氟材料的需求

介绍了氟橡胶，氟涂料，氟塑料金属自润滑材料，新型膨化聚四氟乙烯的性能特点及在国内外飞机上的应用概况。由于高分子材料经氟化改性后会有更好的稳定性和更长的使用寿命，因此，设计员在设计某些有特殊功能要求的结构时，可以重点考虑上述材料。     

可渗透各向同性多孔材料动静压轴承性能研究

利用Ｒｅｙｎｏｌｄｓ和Ｌａｐｌａｃｅ方程以及Ｄａｒｃｙ定律，导出了可渗透各向同性材料动静压窄轴承的计算方程．计算结果显示出这种轴承具有承载力高和姿态角小的特点，并指出设计参数之间存在优化组合．     

核辐射对透波材料介电性能影响

用加速老化试验的方法,在有氧存在的条件下,研究了TDE-85环氧树脂/E玻璃纤维体系、4501A双马来酰亚胺树脂/D3W玻璃纤维体系2种透波材料介电性能受核辐射影响的规律.用60Co辐射源在辐射量为50~800kGy范围内对样件进行辐射,用波导法测试样件的介电常数和介电损耗,测试频率为10GHz.结果发现2种体系透波材料介电性能受核辐射的影响较小,且后者比前者具有更好的抗辐射稳定性.同时利用IR,TGA等手段研究了材料介电性能变化的原因.