FASTL波段多波束馈源设计的初步分析

把抛物面天线的偏焦理论应用于FASTL波段多波束馈源系统的设计,分析了馈源喇叭横向偏焦距离与相应波束偏离角之间的关系,结合多波束射电望远镜扫描方式的要求,给出了FASTL波段多波束馈源的工作带宽、多波束馈源中相邻喇叭的间距以及喇叭口径大小的限制,并对正六边形阵列中处于不同位置的喇叭对应的波束的主瓣情况作了详细计算和分析。由此说明了FASTL波段多波束馈源采用19波束的可行性。另一方面,根据得到的工作频率带宽和喇叭口径大小的情况,对OMT和喇叭类型的选择进行了探讨。本文给出了FASTL波段多波束系统的大概轮廓,为进一步精确设计指明了方向。     

超宽带四脊张角喇叭设计与研究

对下一代候选超宽带馈源进行了分析对比,并设计了一种圆形四脊张角喇叭,该喇叭在7:1的频带范围内在波瓣图相位角0°和45°所对应的E面和D面取得了近乎常数的波束带宽,并且其在2-14 GHz频段范围内回波损耗均在10 dB以上。最后对圆形四脊张角喇叭的增益性能和波束带宽特性进行了探索和研究。该喇叭的研究对中国VLBI2010的超宽带接收系统的设计有重大意义。     

天马望远镜P波段轴向偏焦研究

天马望远镜是65 m口径全实面地平式射电望远镜,信号经赋型抛物面主反射镜和赋型双曲面副反射镜汇集后在卡塞格伦焦点处馈入低温低噪声接收系统。开展天马射电望远镜轴向偏焦研究,旨在拓展天马望远镜在低频段的接收,创新之处在于利用P波段低频振子天线作为接收机馈源,放置在距离副反射面顶点下方约1/4波长处,研究天马望远镜在P波段开展天文观测的可行性。研究内容包括P波段振子天线设计、馈源轴向偏焦位置优化以及观测性能分析。P波段振子天线作为馈源,天线最大增益45 d B,天线效率64.25%。     

FAST30m模型L-波段馈源的设计、制作和性能测试

叙述了FAST（500m口径球面射电望远镜）30m模型L-波段馈源的设计、制作和性能测试过程。馈源的设计仿真使用了HFSS软件，并选用纸板或塑料板和铝箔胶带，通过手工操作完成馈源制作。馈源的性能通过测试表明满足FAST30m模型天文观测的需要。文中采用的HFSS软件仿真及手工制作馈源的方式不失为形式简单的馈源的模型制作的一种快速、经济和有效的方法。这种方法对相近的工作有一定的参考价值。     

射电天文中焦面阵或多波束馈源的应用

焦面阵技术或者多波束馈源系统已经日益广泛地应用于现代射电望远镜，因为它可以充分地利用同一射电望远镜反射面所能提供的信息，在观测比射电望远镜方向瓣大得多的展源时数倍乃至数十倍地提高观测的速度；当存在大气层或电离层的起伏或不均匀影响观测成像质量时，可消除这种影响，提高观测质量；利用焦面阵各单个馈源接收到的信息的互相关，则可以实时监控射电望远镜的反射面、二次反射面、指向精度，从而降低地面上大射电望远镜或空间射电望远镜的精度要求和造价。目前焦面阵已经愈来愈广泛地配置在毫米波射电望远镜和大型射电望远镜的主要波段。对此作了一个较新和全面的评述，对焦面阵应用中的限制，包括相位误差的限制和性能价格比的考虑和可能的前景作了简要的介绍。还分析了在计划中的大型主动球反射面射电望远镜（即FAST）上，配置焦面阵的相应限制、问题和难点，提出了初步的建议，并给出经中英双方讨论后初步拟定的FAST频段、波束及低噪声放大器的配置。     

结构因素对圆锥喇叭电性能影响的仿真分析

馈源是射电望远镜天线系统的一个重要组成部分,其性能将直接影响整个天线系统的电性能。针对射电望远镜天线系统中典型的圆锥喇叭馈源,通过三维电磁仿真软件（CST STUDIO SUITE12．0）进行建模,分析了不同圆锥度、椭圆度及不圆度对圆锥喇叭馈源远场方向性的影响。结果表明：口径面的椭圆度在一定范围内变化时,对圆锥喇叭馈源方向性的影响较小。且其回波损耗小于-15dB;圆柱波导段的圆锥度大于1：20时,圆锥喇叭的效率会受到一定的影响：不圆度的影响则较大。文中得到的结构因素对圆锥喇叭馈源电性能影响的研究结果．对射电望远镜天线系统中圆锥喇叭馈源的设计和制造具有一定的参考作用。     

一种扩大FAST视场的方法

所有的大口径射电望远镜都存在这样一个问题：在其分辨率和灵敏度提高的同时，视场变小．而且口径越大，视场越小．这成为大口径望远镜不可回避的矛盾．要解决这个矛盾，可以在望远镜的焦平面上放置Ⅳ个分立馈源．让它们同时工作，这样可以看作把视场扩大了Ⅳ倍．望远镜的工作效率提高Ⅳ倍．但是这样做的缺点是——视场不连续．且馈源数目Ⅳ受到望远镜焦比(F／D)的限制．采用致密焦面阵(dense focal plane array)就可以很好地解决这个问题．致密焦面阵的单元不是喇叭口天线，而是无方向性的Vivaldi天线(Vivaldi antenna)．要把Vivaldi阵列应用到望远镜上，需要对单个Vivaldi天线和Vivaldi阵列的电性能有清楚的认识，并能根据需要来设计照明方向图．还要知道大望远镜的焦面上电磁场的分布情况，借此判断能否应用Vivaldi阵列，以及给出Vivaldi单元的分路赋权网络．主要给出了FAST的焦面场的分布情况．并说明应用Vivaldi阵列的可能性．     

FAST馈源舱倾覆的理论分析及试验研究

FAST望远镜馈源舱通过6根钢索悬浮于空中,在运行过程中其倾角连续变化,存在发生倾覆的风险。通过舱索系统的静力学理论分析和模型试验对FAST馈源舱的最大倾覆角进行了研究。基于舱倾角最大的优化原则和舱-索系统静力平衡,对索力和姿态角的限定等约束条件,建立了求解舱最大倾角(倾覆角)的目标优化函数,利用牛顿迭代法解得了舱在其运行轨迹面(焦面)的倾覆角,同时研究了重心改变对倾覆角的影响。通过舱索系统3 m缩尺模型对理论分析结果进行了验证,得到了模型舱在给定位置的倾覆角,试验结果与理论计算结果比较吻合。最后分析了馈源舱原型在整个焦面上的倾覆角,结果表明馈源舱在实际工作过程中是安全的,不会发生倾覆。     

新疆奇台110米射电望远镜主焦点馈源换馈方案研究

随着射电天文研究的不断深入,科学家对望远镜分辨率和灵敏度的要求也不断提高,同时要求望远镜具有更宽的观测波段。单口径望远镜低频波段用主焦点接收,馈源尺寸可以更紧凑。为了不影响双反射面天线次焦点的馈电功能,主焦点馈源的放置及换馈方案必须高效合理。以建于新疆奇台的110 m口径全可动射电望远镜为研究对象,以意大利SRT 64 m和德国Effelsberg 100 m射电望远镜为参考,对两种方案应用于奇台110 m射电望远镜的可行性进行分析,并提出一种利用线性模组进行主焦馈源快速切换的新型方案。进行了直线模组机构的建模和仿真,并对口径面信号遮挡进行了分析,结果表明,此方案能有效满足望远镜的工作需求。     

FAST 19波束脉冲星漂移扫描巡天模拟

脉冲星搜索是500 m口径球面射电望远镜(Five-hundred-meter Aperture Spherical Radio Telescope,FAST)的主要科学目标之一。针对FAST设备性能,模拟FAST脉冲星巡天,优化巡天方案,对即将开展的FAST脉冲星巡天项目具有重要的实用价值。基于Parkes多波束巡天、Parkes中纬度巡天和Parkes高纬度巡天的结果,利用脉冲星分布模拟软件包PsrPopPy,模拟得到了银河系中正常脉冲星和毫秒脉冲星的空间分布样本,并根据FAST设备参数进行了虚拟观测。结果表明,使用FAST 19波束接收机漂移扫描观测模式,在中心频率为1250MHz,带宽为400 MHz,每波束扫描时间为13.5 s,有效积分时间为6.0 s的情况下,在赤纬为-14~?12′～65~?48′天区内,可发现1600颗正常脉冲星和238颗毫秒脉冲星。为获得银河系中脉冲星自旋演化的样本,使用evolve代码进行了再次模拟。设置相同的观测参数的情况下,在全天范围内模拟探测到孤立正常脉冲星1749颗,并得到其在P-P图上的分布。     

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.