CSRH-Ⅰ观测数据接收子系统的设计与实现

中国新一代厘米-分米波射电日像仪(Chinese Spectral Radio Heliograph,CSRH)项目已经完成了硬件建设。为了实现从数字接收机中读取观测数据,并将最新的可用数据状态通知其他子系统如监控系统和实时展现系统等,迫切需要一个稳定可靠的数据接收子系统。针对CSRH-I的特点及要求,在分析数字接收机原始数据格式的基础上,设计并实现了CSRH-I观测数据接收子系统。系统基于Linux环境,采用Boost软件包作为底层开发库,实现了基于TCP协议的网络套接服务器,能够异步接收、过滤数字接收机发送来的数据,经过相应的分析处理后最终以文件方式存储数据,进而采用UDP报文方式通知其它子系统观测数据的更新状态。本系统充分考虑了通信过程中可能的异常情况并采取了相应的对策。测试表明,CSRH-I观测数据接收子系统工作稳定可靠,容错能力强,可以满足CSRH-I的应用需求。     

CSRH-I观测数据接收子系统的设计与实现

中国新一代厘米-分米波射电日像仪(Chinese Spectral Radio Heliograph,CSRH)项目已经完成了硬件建设.为了实现从数字接收机中读取观测数据,并将最新的可用数据状态通知其他子系统如监控系统和实时展现系统等,迫切需要一个稳定可靠的数据接收子系统.针对CSRH-I的特点及要求,在分析数字接收机原始数据格式的基础上,设计并实现了CSRH-I观测数据接收子系统.系统基于Linux环境,采用Boost软件包作为底层开发库,实现了基于TCP协议的网络套接服务器,能够异步接收、过滤数字接收机发送来的数据,经过相应的分析处理后最终以文件方式存储数据,进而采用UDP报文方式通知其它子系统观测数据的更新状态.本系统充分考虑了通信过程中可能的异常情况并采取了相应的对策.测试表明,CSRH-I观测数据接收子系统工作稳定可靠,容错能力强,可以满足CSRH-I的应用需求.     

法国高层大气所空间综合孔径项目研究进展

概述了法国高层大气所空间综合孔径项目背景、科学目标以及有效载荷,介绍了该项目演示系统的基本工作原理,探讨了该演示系统的望远子系统、指向子系统、共相子系统和成像子系统,并分别给出了该演示系统在非共相控制和共相控制情况下对半导体激光器和白光点光源的成像结果,实验结果表明演示系统不同独立望远镜之间已经基本实现了共相成像。最后对该演示系统进行了总结,并指出该系统可以进一步优化之处。该演示系统对我国综合孔径成像实验研究具有一定的借鉴意义。     

同幅双速跟踪成像CCD相机模拟电路系统设计

讨论了同幅双速跟踪成像技术对CCD相机系统的特殊要求,详细地介绍了该相机前端模拟系统的设计思想、系统结构和主要的电路模块。对系统中一些关键电路模块进行了仿真和测试,并对仿真和测试结果进行比较分析,以检验电路系统设计的合理性。     

FX型相关处理机长期累加器子系统的研究

介绍了中国VLBI网FX型相关处理机的结构和功能,并着重阐述了相关处理机的长期累加器子系统(LTA),它是相关处理机的条纹数据压缩部件。通过对长期累加器子系统的研究,提出了对该子系统的改进方案,以提高硬件线路的集成度和系统的可靠性,适应了对相关处理机更快速度、更高精度及多台站测量的要求,并说明了实现方法及其改进后的特点。     

FX型相关处理机长期累加器子系统的研究

介绍了中国VLBI网FX型相关处理机的结构和功能，并着重阐述了相关处理机的长期累加器子系统(LTA)，它是相关处理机的条纹数据压缩部件。通过对长期累加器子系统的研究，提出了对该子系统的改进方案，以提高硬件线路的集成度和系统的可靠性，适应了对相关处理机更快速度、更高精度及多台站测量的要求，并说明了实现方法及其改进后的特点。     

LAMOST总控系统程序设计

国家重大科学工程项目LAMOST总控系统的程序设计是一个庞大的软件工程．其总控系统下共包括8个既相互独立又互有关联的子系统．如何通过良好的软件设计方法来处理好这8个子系统之间的关系使其协调运转，以及如何确保软件开发的可维护性、可持续性是研究重点．     

被动型氢钟波谱信号观测装置的设计

简单介绍了被动型氢钟的量子系统,阐述了波谱信号观测装置的设计。该装置采用标准10MHz晶振产生被动型氢钟的微波激射信号(1.420406GHz),然后将该信号输入氢钟的脉泽振荡器中。脉泽振荡器输出的信号经过低噪声放大、两次混频及滤波后所得的谱线包含了量子系统的信息,通过分析最终的谱线即可得知量子系统的优劣。该装置已用于对两台被动型氢钟的测试,并根据测试结果对量子系统进行了改进。     

上海天文台硬件相关处理机Mark5数据回放功能实现

m2hc程序是上海天文台硬件相关处理机的一个子系统，实现从Mark5系统自动回放甚长基线干涉测量（VLBI）原始观测数据给相关处理机的功能。目前已工作在绕月探测工程VLBI测轨任务中。该文详细介绍了m2hc的设计和实现以及应用结果。     

基于USB2.0总线数据侦听的实时幸运成像系统

为进一步提高现有实时幸运成像系统的实时性,针对第二代通用串行总线(Universal Serial Bus 2.0, USB2.0)接口的电子倍增电荷耦合(Electron Multiplying Charge-Coupled Devices, EMCCD)相机进行幸运成像观测的情况,提出了一个基于USB2.0总线数据侦听的实时幸运成像技术方案,进行了侦听电路的硬件设计和数字逻辑设计,搭建了一个具有实时侦听、传输、处理、动态更新和显示的幸运成像系统。当相机拍摄天文图像并与个人计算机(Personal Computer, PC)进行数据交互时,系统的USB2.0总线数据侦听子系统就会对交互的USB2.0总线实现无侵入式侦听,并且加以分析处理后,只将有效的天文图像数据发送给底层现场可编程门阵列(Field Programmable Gate Array, FPGA)开发板中的幸运成像子系统,然后幸运成像子系统对接收的数据进行预处理、动态选图、实时配准和叠加处理,最后采用9个实时分割阈值水平切割高分辨率图像并对二值图像进行动态更新和显示。实验结果表明,所实现的系统能够对在USB2.0总线上连续传输的10 000帧512×512像素的图像进行实时侦听、幸运成像和动态更新显示,实现了幸运成像技术的实时化。     

On the theory of the oblateness of the Sun

In this paper we first emphasize why it is important to know the successive zonal harmonics of the Sun's figure with high accuracy: mainly fundamental astrometry, helioseismology, planetary motions and relativistic effects. Then we briefly comment why the Sun appears oblate, going back to primitive definitions in order to underline some discrepancies in theories and to emphasize again the relevant hypotheses. We propose a new theoretical approach entirely based on an expansion in terms of Legendre's functions, including the differential rotation of the Sun at the surface. This permits linking the two first spherical harmonic coefficients (J ₂ and J ₄) with the geometric parameters that can be measured on the Sun (equatorial and polar radii). We emphasize the difficulties in inferring gravitational oblateness from visual measurements of the geometric oblateness, and more generally a dynamical flattening. Results are given for different observed rotational laws. It is shown that the surface oblateness is surely upper bounded by 11 milliarcsecond. As a consequence of the observed surface and sub-surface differential rotation laws, we deduce a measure of the two first gravitational harmonics, the quadrupole and the octopole moment of the Sun: J ₂=−(6.13±2.52)×10⁻⁷ if all observed data are taken into account, and respectively, J ₂=−(6.84±3.75)×10⁻⁷ if only sunspot data are considered, and J ₂=−(3.49±1.86)×10⁻⁷ in the case of helioseismic data alone. The value deduced from all available data for the octopole is: J ₄=(2.8±2.1)×10⁻¹². These values are compared to some others found in the literature. Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1005238718479     

Accounting for the viscosity of the fluid core in the problem of the physical libration of the moon

A two-component theoretical model of the physical libration of the Moon in longitude is constructed with account taken of the viscosity of the core. In the new version, a hydrodynamic problem of motion of a fluid filling a solid rotating shell is solved. It is found that surfaces of equal angular velocity are spherical, and a velocity field of the fluid core of the Moon is described by elementary functions. A distribution of the internal pressure in the core is found. An angular momentum exchange between the fluid core and solid mantle is described by a third-order differential equation with a right-hand side. The roots of a characteristic equation are studied and the stability of rotation is proved. A libration angle as a function of time is found using the derived solution of the differential equation. Limiting cases of infinitely large and infinitely small viscosity are considered and an effect of lag of a libration phase from a phase of action of an external moment of forces is ascertained. This makes it possible to estimate the viscosity and sizes of the lunar fluid core from data of observations.     

Rotation of the elastic Earth: the role of the angular-velocity-dependence of the elasticity-caused perturbation

We calculate the so-called convective term, which shows up in the expression for the angular velocity of the elastic Earth, within the Andoyer formalism. The term emerges due to the fact that the elasticity-caused perturbation depends not only on the instantaneous orientation of the Earth but also on its instantaneous angular velocity. We demonstrate that this term makes a considerable contribution into the overall angular velocity. At the same time the convective term turns out to be automatically included into the correction to the nutation series due to the elasticity, if the series is defined by the perturbation of the figure axis (and not of the rotational axis) in accordance with the current IAU resolution. Hence it is not necessary to take the effect of the convective term into consideration in the perturbation of the elastic Earth as far as the nutation is related to the motion of the figure axis.     

Impact of the Quadrupole Moment of the Sun on the Dynamics of the Earth-Moon System

Range of values of the Sun's mass quadrupole moment of coefficient J₂ arising both from experimental and theoretical determinations enlarge across literature on two orders of magnitude, from around 10^-7 until to 10^-5. The accurate knowledge of the Moon's physical librations, for which the Lunar Laser Ranging data reach an outstanding precision level, prove to be appropriate to reduce the interval of J₂ values by giving an upper bound of J₂. A solar quadrupole moment as high as 1.1 10^-5 given either from the upper bounds of the error bars of the observations, or from the Roche's theory, is not compatible with the knowledge of the lunar librations accurately modeled and observed with the LLR experiment. The suitable values of J₂ have to be smaller than 3.0 10^-6. As a consequence, this upper bound of 3.0 10^-6 is accepted to study the impact of the Sun's quadrupole moment of mass on the dynamics of the Earth-Moon system. Such as effect (with J₂ = 5.5±1.3 × 10^-6) has been already tested in 1983 by Campbell & Moffat using analytical approximate equations, and thus for the orbits of Mercury, Venus, the Earth and Icarus. The approximate equations are no longer sufficient compared with present observational data and exact equations are required. As if to compute the effect on the lunar librations, we have used our BJV relativistic model of solar system integration including the spin-orbit coupled motion of the Moon. The model is solved by numerical integration. The BJV model stems from general relativity by using the DSX formalism for purposes of celestial mechanics when it is about to deal with a system of n extended, weakly self-gravitating, rotating and deformable bodies in mutual interactions. The resulting effects on the orbital elements of the Earth have been computed and plotted over 160 and 1600 years. The impact of the quadrupole moment of the Sun on the Earth's orbital motion is mainly characterized by variations of , , and . As a consequence, the Sun's quadrupole moment of mass could play a sensible role over long time periods of integration of solar system models. This revised version was published online in July 2006 with corrections to the Cover Date.     

On the role of the motion of the photospheric footpoints of the magnetic field lines

By means of a simple relation between the velocity v of the fluid particle and the velocity v_f of the photospheric footpoint of the magnetic field line v_z and B_z being respectively the components of v and the magnetic field B normal to the photospheric surface, it is shown formally that through the phtospheric surface the transport of all the quantities attributed to the magnetic field, such as the magnetic flux, the magnetic energy and the helicity, is independent of v_z, and v_f is the only kinematical quantity on which the transport depends. In addition, in the neighborhood of the neutral line the velocity v_l of the moving curve of constant B_z is found to be equal approximately to the component of v or v_f in the direction of v_l. Since v_l can be measured or extimated, so can the components of v and v_f near the neutral line.     

Determination of the temperature of the solar corona from the spectrum of the electron-scattering continuum

When the K-corona is formed by the scattering of photospheric radiation from free electrons, the Fraunhofer lines are greatly broadened by the thermal motions of the hot electrons. This paper discusses the possibility of measuring the coronal electron temperature from the residual depressions in the K-coronal spectrum. If the ratio of the intensities at 4100 Å and 3900 Å can be measured to an accuracy of ±1%, the coronal temperature can be inferred to an accuracy of ±0.2 MK. The temperature of a coronal inhomogeneity may also be measured by this method, provided the position angle is known.Now at Fraunhofer Institute, Freiburg, Germany.     

Calculation of the global system of the field-aligned currents on the dayside of the magnetosphere

Using the well-known equation for the normal component of the current which exist near the tangential discontinuity in the plasma in the case of the frozen-in magnetic field, and supposing that the current closes in the ionosphere in the auroral oval in the region 1, one calculates and compares with the data of observations the dependence of the density of the field-aligned current at the level of the ionosphere on the local time.     

On the systematic errors of the determinations of the absolute orientation of the meridian marks

The classical method of determination of the absolute azimuth (or Bessel's parameter n) can secure sufficiently precision for RA from observations of stars at high geographical latitudes during polar night only.