22太阳周极大期Imp≥M1.0X射线耀斑的分布特征

本文对第22太阳周极大时期Imp≥M1.0X射线耀斑的空间分布进行了统计分析.结果表明,该事件存在南北半球分布的不对称性,且不对称性在极大年或其后一年改变符号.文中还对不对称性与太阳活动的相关关系也进行了探讨.      

下一代地铁车辆TQ250永磁同步牵引电机研制

介绍了下一代地铁车辆用TQ250永磁同步牵引电机的研制情况。主要从总体技术要求、设计难点、关键技术、样机试验等方面进行了论述。根据下一代地铁车辆永磁同步牵引电机的技术特点及主要技术参数指标要求,通过对等效定额设计、电磁设计、轻量化设计及冷却结构设计等关键技术攻关,研制了1台永磁同步牵引电机,并进行了试验。样机试验结果分析表明,该电机满足下一代地铁车辆指标要求,验证了所设计的可行性。     

嫦娥四号着陆器月面工作遮挡应对方案研究

嫦娥四号着陆于月球背面南极 艾特肯盆地内,着陆区周围复杂地形导致测控和通信遮挡风险。针对这一问题,开展了着陆区的测控、光照遮挡分析,提出利用轨道控制策略的精细化设计来提高着陆点精度、优化月面工作程序和增加自主控制功能的设计方法,全方面降低嫦娥四号着陆器在月球背面着陆区的生存风险。该方法已通过嫦娥四号着陆器在轨验证,可以为其他深空探测任务提供参考和借鉴。     

星敏感器杂光抑制分析

介绍了用蒙特卡洛法进行星敏感器杂光分析的基本思想、数学模型以及表面热辐射概率模型 ,对典型卫星星敏感器的杂光传递进行了模拟。在复杂的杂光环境下 ,建立杂光传递模型 ,获得了星敏感器杂光环境的定量杂光贡献 ,并对大衰减比遮光罩及光学系统内的杂光传递进行了跟踪 ,给出了遮光罩的消杂光能力     

Transient Effects and Disturbed Conditions

In the present phase of the solar cycle no big transients leading to strong modulation had been observed after 1991. Apart from a few minor disturbances cosmic rays were still recovering to a new intensity maximum. It was suggested, therefore, that existing literature from previous cycles should be critically reviewed. The scene was set by the introductory papers on— phenomenology of cosmic ray modulation in successive solar cycles throughout the heliosphere— the present state of models for long term modulation and their shortcomings— the relation between cosmic ray variations and the magnitude of the interplanetary magnetic field (the CR-B-relation)— charge dependent effects.In the discussions, the study of propagating diffusive disturbances and the CR-B-relation played a central role. The difference was stressed between isolated transient disturbances in the inner solar system (Forbush decreases), and the long lasting, step-like decreases caused by merged interaction regions in the outer heliosphere. The recovery rates following the step-like decreases vary with the phase in the 22-year solar cycle. In some cases this requires a modification of existing drift models. In the outer heliosphere, the CR-B-relation leads to the result 1/ between the diffusion coefficient and the field magnitude . This simple result is a challenge for theoreticians to derive the perpendicular diffusion coefficient fromfirst principles. The three articles in this report essentially follow the list of open points and arguments just presented.The article "Observations and Simple Models" is organised around the model of a propagating diffusive barrier, its application to Forbush effects in the inner heliosphere and to decreases caused by merged interaction regions in the outer heliosphere. Acomparison of observed Forbush decreases with model predictions requires a careful separation of the two steps related to the turbulent region behind the shock front and the closed magnetic field regions of the ejecta (the interplanetary counterparts of coronal mass ejections). It is shown that models for propagating disturbances can be used to derive values of the diffusion coefficients phenomenologically, not only during the disturbance, but also in the ambient medium.The "Modeling of Merged Interaction Regions" summarizes the dynamic and time-dependent process of cosmic ray modulation in the heliosphere. Numerical models with only a time-dependent neutral sheet prove to be successful when moderate to low solar activity occurs but fail to describe large and discrete steps in modulated cosmic rays when solar activity is high. To explain this feature of heliospheric modulation, the concept of global merged interaction regions is required. The com-bination of gradient, curvature and neutral sheet drifts with these global merged interaction regions has so far been the most successful approach in explaining the 11-year and 22-year cycles in the long-term modulation of cosmic rays.The "Remarks on the Diffusion Tensor in the Heliosphere" describe available theories of perpen-dicular diffusion and drift, and discuss their relevance to cosmic rays in the heliosphere. In addition, the information about diffusion coefficients and spatial gradients obtained from the analysis of steady state anisotropies at neutron monitor energies is summarized. These topics are intimately related to the other two articles. They are also part of the general discussion about the "Diffusion Tensor throughout the Heliosphere" which played an important role in all working groups.     

The Solar Wind - Inner Heliosphere

The solar wind in the inner heliosphere, inside ~ 5 AU, has been almost fully characterized by the addition of the high heliographic latitude Ulysses mission to the many low latitude inner heliosphere missions that preceded it. The two major omissions are the high latitude solar wind at solar maximum, which will be measured during the second Ulysses polar passages, and the solar wind near the Sun, which could be analyzed by a Solar Probe mission. Here, existing knowledge of the global solar wind in the inner heliosphere is summarized in the context of the new results from Ulysses.     

Fractionation of SI, NE, and MG Isotopes in the Solar Wind as Measured by Soho/Celias/MTOF

Using the high-resolution mass spectrometer CELIAS/MTOF on board SOHO we have measured the solar wind isotope abundance ratios of Si, Ne, and Mg and their variations in different solar wind regimes with bulk velocities ranging from 330 km/s to 650 km/s. Data indicate a small systematic depletion of the heavier isotopes in the slow solar wind on the order of (1.4±1.3)% per amu (2σ-error) compared to their abundances in the fast solar wind from coronal holes. These variations in the solar wind isotopic composition represent a pure mass-dependent effect because the different isotopes of an element pass the inner corona with the same charge state distribution. The influence of particle mass on the acceleration of minor solar wind ions is discussed in the context of theoretical models and recent optical observations with other SOHO instruments. This revised version was published online in June 2006 with corrections to the Cover Date.     

Coronal plumes and fine scale structure in high speed solar wind streams

We present a solar wind model which takes into account the possible origin of fast solar wind streams in coronal plumes. We treat coronal holes as being made up of essentially 2 plasma species, denser, warmer coronal plumes embedded in a surrounding less dense and cooler medium. Pressure balance at the coronal base implies a smaller magnetic field within coronal plumes than without. Considering the total coronal hole areal expansion as given, we calculate the relative expansion of plumes and the ambient medium subject to transverse pressure balance as the wind accelerates. The magnetic flux is assumed to be conserved independently both within plumes and the surrounding coronal hole. Magnetic field curvature terms are neglected so the model is essentially one dimensional along the coronal plumes, which are treated as thin flux-tubes. We compare the results from this model with white-light photographs of the solar corona and in-situ measurements of the spaghetti-like fine-structure of high-speed winds.     

LED 光质对紫背天葵挥发油和酚类成分积累的影响

为了探索促进紫背天葵在受控环境中更好地积累生物活性成分的有效光质条件,采用3种LED光源（ R60B30G10/60％红光＋30％蓝光＋10％绿光,R70B20G10/70％红光＋20％蓝光＋10％绿光,R60B20G20/60％红光＋20％蓝光＋20％绿光）研究了光质条件对紫背天葵次级代谢物（挥发油和酚类）的影响。结果表明：与R70B20G10光质相比,R60B20G20光质显著增加了萜烯类物质（α,β-石竹烯）的积累,降低了醛类成分（绿叶挥发物）在香气物质中的比例,而R60B30G10与此结果相反;与其它光质相比,R60B30G10光质增加了总花色苷和总黄酮的含量,而在R70B20G10和R60B2OG20光质条件下这些物质的含量没有显著差异;与其它光质相比,R70B20G10光质增加了β-胡萝卜素积累和植物叶片提取物的抗氧化活性（DPPH）,而R60B20G20光质则显著降低了β-胡萝卜素的含量。因此,R70B20G10为适合于紫背天葵积累更多有用次级代谢产物及提高其营养和药用价值的光质条件。     

太阳质子事件与微波爆发的某些特征

选用NOAA提供的太阳质子事件表以及SGD发表的与其相关的射电多波段的观测资料进行了统计分析,试图从厘米波,毫米波爆发与质子事件的关系上寻找规律,从而获得一些有意义的结果.