The detection of “magnetic element” – Why we need a one-meter Space Solar Telescope

The nature of a magnetic element, the elemental structure of the solar magnetic field, is one of the most important mysteries in solar physics. In this paper, we will discuss the requirements of magnetic element detection, such as spatial resolution and magnetic sensitivity. By these discussions, we conclude that it is almost impossible to detect magnetic element with currently used ground-based telescopes and techniques. The proposed Space Solar Telescope, a one-meter Chinese space project, can match these requirements.     

7T磁共振seipin鼠活体无损显型

因遗传突变作用引起皮下脂肪组织缺失可导致脂肪萎缩。本文利用7T小动物磁共振仪对seipin鼠进行了活体无损显型的研究。通过伪彩及加权图像融合技术对采集的seipin鼠和野生鼠图像的处理，可清楚观察到seipin组老鼠的脂肪组织明显少于野生组。同时利用自行开发的7T小动物三维可视化系统中的stroke—based分类方法可方便提取感兴趣组织。为了对两组老鼠的脂肪组织进行定量比较，利用t检验对两组老鼠总的脂肪组织、皮下脂肪及内脏脂肪占总体积的比例进行统计。统计结果表明，seipin组老鼠的脂肪组织及皮下脂肪明显少于野生组，但在本次实验中没有发现两组鼠在内脏组织中脂肪含量存在明显差异。7T小动物磁共振仪为活体研究seipin鼠的显型提供了可靠的手段。     

A MHD-turbulence model for solar corona

The disposition of energy in the solar corona has always been a problem of great interest. It remains an open question how the low temperature photosphere supports the occurence of solar extreme phenomena. In this work, a turbulent heating mechanism for the solar corona through the framework of reduced magnetohydrodynamics (RMHD) is proposed. Two-dimensional incompressible long time simulations of the average energy disposition have been carried out with the aim to reveal the characteristics of the long time statistical behavior of a two-dimensional cross-section of a coronal loop and the importance of the photospheric time scales in the understanding of the underlying mechanisms. It was found that for a slow, shear type photospheric driving the magnetic field in the loop self-organizes at large scales via an inverse MHD cascade. The system undergoes three distinct evolutionary phases. The initial forcing conditions are quickly “forgotten” giving way to an inverse cascade accompanied with and ending up to electric current dissipation. Scaling laws are being proposed in order to quantify the nonlinearity of the system response which seems to become more impulsive for decreasing resistivity. It is also shown that few, if any, qualitative changes in the above results occur by increasing spatial resolution.     

Geosynchronous magnetic field response to the large and fast solar wind dynamic pressure change

We present a comparison of large and sharp solar wind dynamic pressure changes, observed by several spacecraft, with fast disturbances in the magnetospheric magnetic field measured by the GOES-8, 9 and 10 geosynchronous satellites. Almost 400 solar wind pressure changes in the period 1996–2003 were selected for this study. Using the large statistics we confirmed that increases (decreases) in the dynamic pressure always results in increases (decreases) in the magnitude of geosynchronous B_z component. The amplitude of the geosynchronous B_z response strongly depends on the location of observer relative to the noon meridian, from the value of solar wind pressure before the disturbance arriving and firstly – from the amplitude of the pressure change.     

On the application of the boundary element method in coronal magnetic field reconstruction

Solar magnetic field is believed to play a central role in solar activities and flares, filament eruptions as well as CMEs are due to the magnetic field re-organization and the interaction between the plasma and the field. At present the reliable magnetic field measurements are still confined to a few lower levels like in photosphere and chromosphere. Although IR technique may be applied to observe the coronal field but the technique is not well-established yet. Radio techniques may be applied to diagnose the coronal field but assumptions on radiation mechanisms and propagations are needed. Therefore extrapolation from photospheric data upwards is still the primary method to reconstruction coronal field. Potential field has minimum energy content and a force-free field can provide the required excess energy for energy release like flares, etc. Linear models have undesirable properties and it is expected to consider non-constant-alpha force-free field model. As the recent result indicates that the plasma beta is sandwich-ed distributed above the solar surface (Gary, 2001), care must be taken in modeling the coronal field correctly. As the reconstruction of solar coronal magnetic fields is an open boundary problem, it is desired to apply some technique that can incorporate this property. The boundary element method is a well-established numerical techniques that has been applied to many fields including open-space problems. It has also been applied to solar magnetic field problems for potential, linear force-free field and non-constant-alpha force-free field problems. It may also be extended to consider the non-force-free field problem. Here we introduce the procedure of the boundary element method and show its applications in reconstruction of solar magnetic field problems. This revised version was published online in August 2006 with corrections to the Cover Date.     

轴向磁悬浮轴承位置检测方法的研究

本文研究了采用非接触差动电感位移传感器器检测轴向磁悬浮轴承的方法及特点，并对该方法的可行性进行了分析。     

圆盘类钛合金零件的精密加工

文章介绍了以钛合金为材料的某型号圆盘类结构件的结构和加工特点、主要表面加工措施等，通过采用合理的装夹方法和加工方法，选择合理的切削工艺参数和刀具参数，安排合适的热处理，解决了高精度薄壁圆盘类结构件的加工难题，为圆盘类钛合金结构件的加工积累了经验。     

根据线性迭加理论实现微小卫星姿态磁控制

根据地磁力矩定向阻尼特性和线性迭加理论,提出仅用磁力矩器实现对地指向微小卫星三轴姿态稳定的控制律。推导了采用迭加补偿,并考虑附加磁矩影响时改进的卫星姿态动力学方程。理论分析和仿真结果表明,该控制律简单、姿态控制精度高。     

日冕膨胀和太阳角动量向行星际空间的转移

本文讨论了日冕膨胀中的角动量问题。利用大量I型彗尾资料的计算,证实了日冕膨胀中方位分量的存在;它不仅是随机量,而是具有大小为9.8km/s的定常量。太阳演化到主序星阶段以来,由于日冕膨胀丢失了80％的角动量,太阳自转角速度正以指数律下降。因此,这将对太阳动力演化起到很大的影响。