Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere

We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube.     

Recent advancements in the EST project

The European Solar Telescope (EST) is a project of a new-generation solar telescope. It has a large aperture of 4?m, which is necessary for achieving high spatial and temporal resolution. The high polarimetric sensitivity of the EST will allow to measure the magnetic field in the solar atmosphere with unprecedented precision. Here, we summarise the recent advancements in the realisation of the EST project regarding the hardware development and the refinement of the science requirements.     

Interpretation of the SOHO/UVCS observations of two CME-driven shocks

We report on the analysis of two fast CME-driven shocks observed with the UltraViolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO). The first event, detected on 2002 March 22 at 4.1 R_⊙ with the UVCS slit placed in correspondence with the flank of the expanding CME surface, represents the highest UV detection of a shock obtained so far with the UVCS instrument in the corona. The second one, detected on 2002 July 23 at 1.6 R_⊙ with the UVCS slit placed in correspondence with the front of the expanding CME surface, shows an anomalous deficiency of ion heating with respect to what observed in previous CME/shocks observed by UVCS, possibly reflecting the effect of different coronal plasma conditions over the solar cycle. From the two different sets of observations we derived an estimate for the shock compression ratio X, which turns out to be X = 2.4 ± 0.2 and X = 2.2 ± 0.1, respectively, for the first and second event. Comparison between the two events provides complementary perspectives on the dynamical evolution of CME-driven shocks.     

EXPERIMENTAL INVESTIGATION ON R134A AIRBORNE VAPOR-COMPRESSION REFRIGERATION SYSTEM

The airborne high power electrical equipments have been widely used in modern aircrafts, which conse- quently causes the dramatic increase of heating load up to dozens of kilowatts. Accordingly, vapor-compression re- frigeration system （VCRS） with lower engine bleed air and larger refrigeration capacity has been paid much atten- tion in recent years. Therefore, based on the analysis of the characteristics of VCRS, an experiment system of VCRS using R134a is set up to simulate operation performances. The influences of different parameters including evaporation pressure, condensing pressure, refrigerant mass flow rate and compressor rotation speed are also in- vestigated. The impacts of different parameters on the system performance are various. This work can help to es- tablish the specific control law under different work conditions.     

Solar neutron events as a tool to study particle acceleration at the Sun

The Sun provides unique opportunities to study particle acceleration mechanisms using data from detectors placed on the Earth’s surface and on board spacecrafts. Particles may gain high energies by several physical mechanisms. Differentiating between these possibilities is a fundamental problem of cosmic ray physics. Energetic neutrons provide us with information that keeps the signatures of the acceleration site. A summary of some representative solar neutron events observed on the Earth’s surface, including associated X and γ-ray observations from spacecrafts is presented. We discuss evidence of acceleration of particles by the Sun to energies up to several tens of GeV. In addition, a recent solar neutron event that occurred on September 7th 2005 and detected by several observatories at Earth is analyzed in detail.     

基于Zernike矩的高精度太阳图像质心提取算法

在基于太阳观测的月球车天文导航系统中,针对太阳传感器中图像噪声以及典型图像退化的不良影响,提出了一种基于Zernike矩的高精度太阳质心提取算法。采用Sobel算子进行边缘检测,Zernike矩重定位亚像素边缘,用最小二乘法拟合圆心。而当图像存在退化时,进行有效圆边缘点检测后,再用该法提取质心。从理论上分析了Zernike矩亚像素边缘检测对圆拟合法的改进作用。利用仿真图像和地表实验图像,将本文方法与传统的重心法、带阈值的重心法和圆拟合法进行了比较。结果表明,本文方法精度更高,具有更好的稳定性,可以对月球车天文导航精度的提高起良好作用。     

孙中山与邓小平的社会主义本质论的相通性

孙中山的社会主义思想和邓小平的社会主义本质论,在发展生产力、变革生产关系和实现共同富裕等方面存在着相同性或相通性。这些相通性启迪我们必须坚持走社会主义道路,坚持马克思主义基本原理和中国的具体国情相结合,在实践中不断丰富和发展马克思主义。     

基于CFD方法的机翼阵风响应研究

通过引入＂网格速度＂方法模拟阵风条件,求解非定常欧拉方程实现了不同展弦比0012平直机翼阵风响应的数值模拟。首先采用该方法对NACA0006翼型迎角阶跃型阵风的气动力响应进行了计算,计算结果与文献结果、理论值吻合良好。进一步对展弦比分别为5、10的0012平直机翼在迎角阶跃型、One-Minus-Cosine型阵风作用下的气动力响应过程进行了模拟分析。研究结果表明,当展弦比增大时,阵风作用下机翼的升力系数响应会增加,机翼翼根部位气动响应幅值大于翼尖部位响应特性。     

改进谢别德插值方法在地磁图构建中的应用

构建地磁图是地磁/惯性组合导航研究的一项重要内容,为了提高地磁导航中地磁基准图的精度,本文分析研究了改进谢别德插值算法,简要概述了数字地磁图的构建原则,并将改进谢别德插值算法应用到地磁图构建中.通过实验验证,发现该方法与距离加权反比插值算法、克里格插值算法相比,具有较好的插值效果.由此,初步判定改进谢别德插值算法在地磁...     

Spin parameters of nanosatellite BLITS determined from Graz 2 kHz SLR data

The nanosatellite BLITS (Ball Lens In The Space) is the first object designed as a passive, spherical retroreflector of the Luneburg type, dedicated for Satellite Laser Ranging (SLR). The 2 kHz SLR station Graz measures spin parameters of this satellite, providing information about the rotational dynamics of the body. The measurements obtained during the period from September 26, 2009 to November 24, 2010 show a significant change of the spin configuration. The spin axis was dynamically precessing since the launch and currently is sinus-like behaving between coordinates RA 120°…150°, Dec 30°…60° (J2000 inertial reference frame). The angle between the symmetry axis and the spin axis of BLITS is not constant, but is decreasing since the launch, while its spin period is rather stable with a mean value of 5.613 s (clockwise rotation). The satellite was dynamically changing its attitude during the first three months after deployment; after this time the spin parameters are relatively stable.