利用光纤电容液滴分析仪测量液体折射率的研究

光纤电容液滴分析仪(FCDA:Fiber-capacitive Drop Analyzer)是一种用于液体特性研究的新型仪器,该仪器利用光纤液滴分析技术和电容液滴分析技术制成特殊的液滴传感器,获取经过液滴的光强信号随液滴生长变化的规律,得到反映液体综合特性的“液滴指纹图”。该仪器具有测量液体的物理特性参数的能力。本文就利用光纤电容液滴分析仪在液体折射率的测量方面进行了研究,利用线性关系来测量不同浓度的酒精的折射率,并给出了结果的误差分析。     

Global characteristics of ionospheric electric fields and disturbances during the first hours of magnetic storms

The ionospheric plasma density can be significantly disturbed during magnetic storms. In the conventional scenario of ionospheric storms, the negative storm phases with plasma density decreases are caused by neutral composition changes, and the positive storm phases with plasma density increases are often related to atmospheric gravity waves. However, recent studies show that the global redistribution of the ionospheric plasma is dominated primarily by electric fields during the first hours of magnetic storms. In this paper, we present the measurements of ionospheric disturbances by the DMSP satellites and GPS network during the magnetic storm on 6 April 2000. The DMSP measurements include the F region ion velocity and density at the altitude of ∼840 km, and the GPS receiver network provides total electron content (TEC) measurements. The storm-time ionospheric disturbances show the following characteristics. The plasma density is deeply depleted in a latitudinal range of ∼20° over the equatorial region in the evening sector, and the depletions represent plasma bubbles. The ionospheric plasma density at middle latitudes (20°–40° magnetic latitudes) is significantly increased. The dayside TEC is increased simultaneously over a large latitudinal range. An enhanced TEC band forms in the afternoon sector, goes through the cusp region, and enters the polar cap. All the observed ionospheric disturbances occur within 1–5 h from the storm sudden commencement. The observations suggest that penetration electric fields play a major role in the rapid generation of equatorial plasma bubbles and the simultaneous increases of the dayside TEC within the first 2 h during the storm main phase. The ionospheric disturbances at later times may be caused by the combination of penetration electric fields and neutral wind dynamo process.     

Stochastic particle acceleration by the forced interaction of relativistic current sheets

We address the problem of interacting relativistic current sheets in self-consistent kinetic plasma simulations within the framework of the Particle-In-Cell model. The interaction is enforced in head-on collisions of up to 10 current sheets at relativistic bulk speeds. The simulations are motivated by the general problem of Poynting flux dissipation in ‘striped wind’ configurations presumably governing the relativistic outflows pervasive in pulsar winds and gamma-ray bursts. We identify the generation of non-thermal particles and formation of a stable power-law shape in the particle energy distributions f(γ) dγ ∝ γ^−s dγ. In 1D, a spectral index s ∼ 2 is observed and attributed to a stochastic Fermi-type acceleration mechanism. In 2D, the generic index of s ∼ 3–4 is retained as in previous simulations of individual current sheets. Whereas in 2D the high energy cut-off is constrained by the limited dissipation of magnetic energy, in 1D the process converts the bulk motion of current sheets towards directed particle momentum of an exclusive class of non-thermal particles.     

利用奇异辛几何构作新的带仲裁的认证码

利用有限域上奇异辛几何构造了一个新的带仲裁的认证码，并计算了这个码的参数。当收方和发方的编码规则按等概率分布选取时，计算出了各种攻击成功的概率。     

可变桨距冲压空气涡轮混合型流场数值研究

冲压空气涡轮流场数值研究主要目的是模拟在实际高空加油工作状态下涡轮变桨距气动特性.数值风洞实验采用代数Baldwin-Lomax湍流模型,雷诺平均Navier-Stokes方程,模拟可变桨距冲压空气涡轮全三维混合型流场,并分析其流场主要气动特性,探讨桨叶载荷分布原因,然后将数值模拟结果与风洞实验数据进行了比较.改进桨叶近轮毂区域气动性能可进一步提高冲压涡轮载荷.      

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.     

利用有限域上向量空间构作具有仲裁的认证码

利用有限域上向量空间的子空间构作了一个具有仲裁的认证码，计算了这个码的参数。当收方和发方的编码规则按等概率分布选取时，各种攻击成功的概率也被算出。     

Improved orbital parameters of accreting millisecond pulsar SAX J1808.4-3658

We analyze the three outbursts of the X-ray millisecond pulsar SAX J1808.4-3658 that occurred in 1998, 2000, and 2002 observed with RXTE. With a technique based on epoch folding search we find an unique orbital solution valid over the five years of high temporal resolution data available. We revise the estimate of the orbital period, P_orb = 7249.1569(1) s and of its error, which we decrease by one order of magnitude. We also give the first constraint on the orbital period derivative, . We find that in 2002 the pulse profile shape is clearly asymmetric, showing a secondary peak at about 145° from the main pulse, which is different from the sinusoidal shape reported at the beginning of the 1998 outburst.     

三维钝体结构风压分布与绕流特性的大涡模拟研究

针对风场作用下三维钝体结构的绕流特性与空间风压分布特性,采用大涡模型对其进行了数值模拟研究,以平均风速和脉动风速作为入口边界条件,在稳态分析的基础上对9种不同来流方向的工况进行了瞬态动力分析,再现了钝体绕流的冲撞、分离、重附着等现象,揭示了钝体绕流主、次涡循环区的形成、发展机理,提出了空间风压场分布的一般规律。研究表明:钝体绕流对流场风速剖面影响的强弱程度依次为尾流区、屋顶区、来流区,且对中心区域流场风速剖面的影响要大于两侧流场,并由中心区域向两侧逐渐减小;来流区钝体绕流特性与空间风压分布特性较屋顶区和尾流区稳定,尾流区涡旋的非对称生成、脱落对钝体左右两侧流场的冲撞、分离、重附着等具有重要的影响;来流方向与钝体呈45°或135°夹角时,对尾流风场的影响范围最小,但随着来流方向逐渐垂直于钝体,尾流影响区域也逐渐增大。     

Plasmasphere Response: Tutorial and Review of Recent Imaging Results

The plasmasphere is the cold, dense innermost region of the magnetosphere that is populated by upflow of ionospheric plasma along geomagnetic field lines. Driven directly by dayside magnetopause reconnection, enhanced sunward convection erodes the outer layers of the plasmasphere. Erosion causes the plasmasphere outer boundary, the plasmapause, to move inward on the nightside and outward on the dayside to form plumes of dense plasma extending sunward into the outer magnetosphere. Coupling between the inner magnetosphere and ionosphere can significantly modify the convection field, either enhancing sunward flows near dusk or shielding them on the night side. The plasmaspheric configuration plays a crucial role in the inner magnetosphere; wave-particle interactions inside the plasmasphere can cause scattering and loss of warmer space plasmas such as the ring current and radiation belts.