Relativistic proton production at the Sun in the 20 January 2005 solar event

Based on the concept of multiple acceleration of solar energetic particles (SEP) we analyzed the super-event of 20 January 2005 by the data of ground level, balloon and spacecraft observations. The main characteristics of relativistic solar protons (energy spectra, anisotropy directions and pitch-angle distributions) are derived and their dynamics during the event is studied. It is shown that the flux of relativistic solar protons may consist of two distinct components, the so-called prompt and delayed ones. Within a two-source model of particle generation, one of which is associated with an expanding magnetic loop, we solved the transport equation in energy phase space, including adiabatic losses simultaneously with the stochastic acceleration process, and calculate the expected spectra of the delayed component at the source. The confrontation of experimental spectra with theoretical ones shows that the delayed component may be correctly described by stochastic acceleration, but not the prompt component. The required acceleration efficiencies turned out to be rather high, so that, for this particular event, adiabatic cooling is practically negligible. Our results provide a new support to the existence of two populations of relativistic solar protons in some SEP events.     

Magneto-gravity Waves Trapped in the Lower Solar Corona

The possibility of trapped magneto-gravity waves in the lower solar corona with an open magnetic field is discussed. Intensity variations and/or Doppler shifts of relevant UV, EUV and x-ray spectral lines in the chromosphere, transition region and lower corona may reveal the existence of such low-frequency modes (with periods longer than ∼ 1.5 hour). The spectrum may be either discrete or continuous depending on the reflection property of the narrow transition region. These modes can be utilized to probe the dynamics of the upper chromosphere, transition region and lower corona; they may also play an important role in coronal heating. This revised version was published online in June 2006 with corrections to the Cover Date.     

精密小直径盲孔珩磨

在论述了珩磨、盲孔珩磨现状的基础上,重点介绍了精密小直径盲孔珩磨的原理、珩磨条座、珩磨杆的结构,可达到的加工精度,推广此项工艺应解决的问题及其展望。     

一种适用于曲面结构的机器人制孔误差在线补偿技术

针对工业机器人应用于飞机零部件自动钻孔时各项误差累积造成制孔精度差的问题，提出一种利用单应关系计算机器人驱动坐标三维偏差，以在线补偿机器人制孔精度的方法。首先利用外部测量设备建立机器人制孔系统中各坐标系关系；在标定阶段，通过以一定倾斜角度固联于机器人末端的相机拍摄一幅安装于制孔工作平面上与刀轴正对的平面标定板图像，并据此完成基于单应变换的手-眼关系标定；在实际制孔过程中，机器人在测距传感器及相机的辅助下，从基准孔理论坐标对应的姿态，不断调整至基准孔正上方理想位置，通过手-眼关系计算基准孔实际位置对应的机器人驱动坐标，然后根据一组基准孔的机器人三维驱动误差，计算三维驱动误差变换矩阵，据此获得这组基准孔邻域范围内各待钻孔的机器人驱动坐标补偿量，从而实现待钻孔定位误差补偿。以飞机结构实验件为对象进行了模拟制孔验证，实验结果表明，补偿前待钻孔三维综合定位误差和法向误差测量值范围分别为2.28~2.85 mm和2.09°~3.93°，平均为2.55 mm和3.30°，补偿后制孔最大误差分别不超过0.30 mm和0.21°，满足自动制孔位置精度要求。     

CME productivity associated with Solar Flare peak X-ray emission flux

It is often noticed that the occurrence rate of Coronal Mass Ejections (CMEs) increases with increase in flare duration where peak flux too increase. However, there is no complete association between the duration and peak flux. Distinct characteristics have been reported for active regions (ARs) where flares and CMEs occur in contrast to ARs where flares alone occur. It is observed that peak flux of flares is higher when associated with CMEs compared to peak flux of flares with which CMEs are not associated. In other words, it is likely that flare duration and peak flux are independently affected by distinct active region dynamics. Hence, we examine the relative ability of flare duration and peak flux in enhancing the CME productivity. We report that CME productivity is distinctly higher in association with the enhancement of flare peak flux in comparison to corresponding enhancement of flare duration.     

带肋和出流孔通道换热研究

采用热色液晶瞬态测试技术测量了带肋和出流孔通道各壁面的换热系数分布,分析了雷诺数和出流比对换热系数的影响,其中雷诺数的变化范围是20000~80000,出流比的变化范围是0.3~0.6。结果表明:出流比的变化对各壁面均有较大影响,无出流孔带肋壁面的换热沿通道减弱,带肋和出流孔壁面的换热在通道入口处先增大之后沿通道减小;各壁面平均换热增强系数随雷诺数增大而减小。无出流孔的带肋壁面和侧壁的平均换热增强系数随出流比增大而减小,带肋和出流孔壁面的平均换热增强系数不随出流比变化而变化。     

A balloon-borne very long baseline interferometry experiment in the stratosphere: Systems design and developments

The balloon-borne very long baseline interferometry (VLBI) experiment is a technical feasibility study for performing radio interferometry in the stratosphere. The flight model has been developed. A balloon-borne VLBI station will be launched to establish interferometric fringes with ground-based VLBI stations distributed over the Japanese islands at an observing frequency of approximately 20?GHz as the first step. This paper describes the system design and development of a series of observing instruments and bus systems. In addition to the advantages of avoiding the atmospheric effects of absorption and fluctuation in high frequency radio observation, the mobility of a station can improve the sampling coverage (“uv-coverage”) by increasing the number of baselines by the number of ground-based counterparts for each observation day. This benefit cannot be obtained with conventional arrays that solely comprise ground-based stations. The balloon-borne VLBI can contribute to a future progress of research fields such as black holes by direct imaging.     

Kelvin–Helmholtz instability in a twisting solar polar coronal hole jet observed by SDO/AIA

We investigate the conditions under which the fluting ($m=2$), $m=3$, and $m=12$ magnetohydrodynamic (MHD) modes in a uniformly twisted flux tube moving along its axis become unstable in order to model the Kelvin–Helmholtz (KH) instability in a twisting solar coronal hole jet near the northern pole of the Sun. We employed the dispersion relations of MHD modes derived from the linearized MHD equations. We assumed real wavenumbers and complex angular wave frequencies, namely complex wave phse velocities. The dispersion relations were solved numerically at fixed input parameters (taken from observational data) and varying degrees of torsion of the internal magnetic field. It is shown that the stability of the modes depends upon five parameters: the density contrast between the flux tube and its environment, the ratio of the external and internal axial magnetic fields, the twist of the magnetic field lines inside the tube, the ratio of transverse and axial jet’s velocities, and the value of the Alfvén Mach number (the ratio of the tube axial velocity to Alfvén speed inside the flux tube). Using a twisting jet of 2010 August 21 by SDO/AIA and other observations of coronal jets we set the parameters of our theoretical model and have obtained that in a twisted magnetic flux tube of radius of $9.8$ Mm, at a density contrast of $0.474$ and fixed Alfvén Mach number of $?0.76$, for the three MHD modes there exist instability windows whose width crucially depends upon the internal magnetic field twist. It is found that for the considered modes an azimuthal magnetic field of $1.3$–$1.4$ G (computed at the tube boundary) makes the width of the instability windows equal to zero, that is, it suppress the KH instability onset. On the other hand, the times for developing KH instability of the $m=12$ MHD mode at instability wavelengths between 15 and 12 Mm turn out to be in the range of $1.9$–$4.7$ min that is in agreement with the growth rates estimated from the temporal evolution of the observed unstable jet’s blobs in their initial stage.     

Relativistic astrophysics explorer

The great success of the Rossi X-Ray Timing Explorer (RXTE) has shown that X-ray timing is an excellent tool for the study of strong gravitational fields and the measurement of fundamental physical properties of black holes and neutron stars. Here, we describe a next-generation X-ray timing mission, the Relativistic Astrophysics Explorer (RAE), designed to fit within the envelope of a medium-sized mission. The instruments will be a narrow-field X-ray detector array with an area of 6 m² equal to 10 times that of RXTE and a wide-field X-ray monitor. We describe the science made possible with this mission, the design of the instruments, and results on prototype large-area X-ray detectors.     

带抑涡支孔结构新型气膜孔的实验研究

采用稳态液晶测温法对基准孔和3个在计算中有较好冷却效率的带抑涡支孔结构新型气膜孔进行了实验研究。实验结果表明:新型气膜孔的抑涡支孔对主气膜孔起到了保护作用,使新型孔在不同吹风比下的冷却效率要高于普通基准孔,特别是在高吹风比的情况下,这种现象更加明显。在低吹风比情况下,三种不同结构新型孔的冷却效率差别不大;而在高吹风比时,支孔与主孔平行孔型和支孔在主孔下游孔型要高于支孔在主孔上游的孔型,该现象随着吹风比增加会愈加明显。