自行与银河系研究的前沿

简述了精确测定相对自行的方法,特别介绍了在用2～3个历元的底片和CCD观测结果推导恒星自行的过程中如何消除光学视场畸变、星等差和色差的具体办法;并介绍了用星系把相对自行推算绝对自行的方法。还介绍了用自行资料研究银河系结构和演化的一些前沿课题,其中包括星团研究、与银河系兼并的矮星系的发现、暗物质的检测、外星行星的探测和银河系中心黑洞的质量估算等。最后评价了自行在研究银河系中的重要性,论述了我国研制4m光学/近红外望远镜的重要意义。     

一种基于傅里叶变换和图像二值化阈值遍历的干涉条纹角度计算方法

消除综合孔径望远镜子孔径之间的相对光程差是实现高分辨率干涉成像的前提条件,条纹检测法是一种检测相对光程差的有效办法。因子孔径的空间位置排布使干涉条纹具有一定的方向性,若不能精确获知干涉条纹的角度,则无法沿条纹的法线方向行采样,进而无法根据对比度变化曲线的最大值获得子孔径之间的最小光程差位置。提出了一种基于傅里叶变换和图像二值化阈值遍历的获得干涉条纹角度的方法,首先介绍了算法的基本原理,其次通过对条纹角度为43°的仿真数据进行算法验证得到的角度为43.007 8°,与理论值的误差为0.018%,证实了方法的可行性。最后对比了未旋转相机和旋转相机两种情况下的条纹对比度变化曲线,可知通过旋转相机使条纹转至相机靶面纵轴方向再进行采样的办法,更有利于精确得到相对光程差的最小位置。     

并置VLBI站的相对形变及其与全球解结果的比较

基于ITRF2000地球参考架的三维VLBI站速度矢量和NNR-NUVEL-1A地球板块运动模型，采用观测的VLBI基线长变化率作为约束，估计和讨论了全球6个并置VLBI站的局部或区域性地壳的相对形变，并与国际地球参考架ITRFs解和VLBI全球解glb2003以及VTRF2003的结果进行了比较．结果表明日本Kashima与Kashim34VLBI站之间，美国GREENBANK的NRAO20与NRAO85-3站之间可能存在每年约近4毫米的相对垂直形变；WESTFORD与HAYSTACK二站间每年近2毫米的垂直形变率差基本可得到肯定，KOKEE和KAUAI二站的垂直形变率约有每年1至3毫米的差．利用如下方法能较可靠地检测出并置VLBI站间的局部或区域性的地壳垂直形变，改进ITRF解的可能不足．     

关于脉冲星的磁层结构

本文讨论有力场的脉冲星磁层结构。用极角展开的方法。可以得到轴对称脉冲星方程组的局部解。本文特别讨论了极轴附近和赤道面附近的区域。在脉冲星表面附近磁能密度比其他能量密度大,远离脉冲星表面处,引力势能和转动动能相对较大,这些因素会影响脉冲星磁层中的物质分布。分析表明,等离子体的转动可能是非刚性的,因而可能不存在一个闭场的共转区域。     

1988年至1995年IERS天球参考架的指向维持

本文分析了１９９２年至１９９５年期间国际地球自转服务（ＩＥＲＳ）天球参考架的指向维持情况，结合１９８８年至１９９２年的指向维持情况指出，该参考架在１９８８年至１９９５年期间历年的指向均存在显著变化，赤经零点和天极的最大年度漂移约为０．４ｍａｓ。至１９９５年，ＩＥＲＳ天球参考架的赤经零点和天极与各自预期位置的偏差不于０．４ｍａｓ。１９９４年和１９９５年的ＩＥＲＳ天球参考架基本上维持了１９９３年的ＩＥＲＳ天球参考指向，但是其实际维持精度约为０．０５ｍａｓ，并非０．００５ｍａｓ。０．００５ｍａｓ的维持精度只是数学上的平均效果，相当一部分基本源在相邻年度的ＩＥＲＳ天球参考架中的坐标差大于０．５ｍａｓ，这说明只有采用恰当的消除局部相对形变的方法，才能将天球参考架的指向真正维持在较高水平。     

附加相对约束关系的月表全景相机平差算法研究

我国近期发射的月球探测器携带了全景相机的科学载荷,负责获取巡视器着陆区的月球表面影像。全景相机共有两台,采用双目立体成像,实际工作时保持相对位置和姿态关系不变。参考地球测绘、计算机视觉等领域的多个相似案例,使用一种改进的平差模型,经过实验验证,证明该模型能够消除不同立体像对间相对位置和姿态的偏差,使平差结果更加可靠,为我国探月任务中月表全景相机影像数据的摄影测量处理提供帮助和支持。     

用日全食光谱探测太阳中低层大气对局部热动平衡的偏离

在太阳大气不同层次连续光谱中叠加有丰富的发射线或吸收线,对这些谱线轮廓进行反演分析可以探测太阳大气的化学成分和物理状态.太阳大气的色球及过渡区由于其密度低难以建立热动平衡,建立相应的大气模型需要采用非局部热动平衡(Non-Local Thermodynamic Equilibrium,N-LTE)理论.根据相对偏离因子计算来研究太阳中低层大气偏离局部热动平衡(Local Thermodynamic Equilibrium,LTE)分布的情况.首先对日全食观测过程中得到色球和过渡区不同高度形成的两条光谱数据进行反演,得到确定观测谱线的参数信息,如连续谱源函数、谱线源函数、多普勒宽度和由此推出的等效动力学温度;根据这些反演出的谱线参量计算出二维视场内每个空间采样点偏离LTE状态的定量结果;其次,根据用于观测的积分视场单元光纤排布阵列重构出辐射强度、等效动力学温度和相对偏离因子二维分布.结果显示:在局部小区域,温度分布和相对偏离因子的分布存在较强相关性,而与辐射强度分布无明显相关.从两条谱线导出的等效温度和相对偏离因子分布存在明显的差异.这两种二维分布揭示出太阳大气某些小尺度区域具有较强的结构性和复杂性,为进一步理解太阳中低层大气物理提供了一种新的视角.     

基于多项式模型的射电天文中的移动干扰消除

射电天文观测数据受无线电的影响日益严重。因此,射频干扰(Radio Frequency Interference,RFI)消除已经成为信号处理流程中不可或缺的一步。考虑了自适应阵列信号处理中的移动干扰源的消除问题,对于阵列天线望远镜而言,射频干扰消除可以通过采样协方差矩阵在空域实施处理。在很多应用场景中,可得到的零点深度受限于协方差矩阵的估计误差,进而影响干扰子空间的估计精度。方法应用了一种多项式模型以跟踪阵列协方差矩阵随时间的变化,消除干扰子空间的估计误差,提高干扰消除性能。最后通过仿真对比了传统的子空间投影(Subspace Projection,SP)算法和基于多项式模型的子空间投影(Polynomialaugmented Subspace Projection,PSP)算法,仿真结果证明了所提方法的有效性。     

基于先验信息的空间碎片探测方法

提出了一种基于先验信息的空间碎片图像探测方法.该方法通过先验信息,在图像中碎片星像的邻域设置波门,计算波门内的局部背景阈值,辅以相关的判据识别目标.随后使用矩方法计算碎片质心相对波门中心的偏离值,通过线性平移计算碎片质心在整幅图像中的位置.实验表明:该方法复杂度低、便于实现、实时性好,可以高效、准确地探测空间碎片,比较精确地确定碎片的质心位置.     

消除CCD图像中宇宙射线的算法的比较

CCD天文图像在采集过程中会受到各种噪声的影响,其中宇宙射线噪声有时会严重影响到图像中的有用信息。研究如何有效识别和剔除宇宙射线噪声对于天文图像的信息提取是非常重要的。针对目前国际上较新的三种消除宇宙射线的算法:Laplacian边缘检测算法(A Laplacian Edge Detection Algorithm),基于直方图的快速算法(A Fast Algorithm BasedOn Histogram)以及万能噪声消除算法(A Universal Noise Removal Algorithm),采用由云南天文台1m望远镜拍摄的CCD图像进行了模拟实验和实际宇宙射线的处理。实验表明Laplacian边缘检测算法能相对准确地探测到恒星和星系图像上的宇宙射线。并对算法的效果和复杂度进行比较和分析。最后探讨了如何准确替代宇宙射线像素点的灰度值。     

Some results of geodetic referring of the radio telescope and SLR stations to GPS markers in the Crimean geodynamical test area Simeiz-Katsyveli

Positions of space-geodetic instruments are calculated in the International Terrestrial Reference Frame (ITRF2000) by referring the instrument reference points to the local geodetic network and GPS markers. The eccentricities of the SLR stations CrAO and CLO and the permanent GPS station CrAO with respect to the reference point of the radio telescope RT-22 are determined. The local relative deformations of the Earth’s surface are presented as shifts of the instrument reference points with respect to the nearest points of the local geodetic network and with respect to each other.     

1979-1999全球天测与测地VLBI观测资料处理结果与讨论

采用国际地民服务（ＩＥＲＳ）１９９６年规范和上海天文台甚长基线干涉测量（ＶＬＢＩ）资料分析软件,对自１９７９年８月以来全球约２９００次天测与测地ＶＩＢＬ实验进行了综合归算,得到６０１颗河外射电源在Ｊ２０００．０的坐标、１０１台站在Ｊ１９９７．０的坐标和运动速度、以及约２０年地地球定向参数序列。与国际相关结果的比较表明,归算结果不存在显著系统差。通过对归算结果的分析,指出目前国际上评估天球参考架局部     

低纬子午环的总体设计要求

根据地面光学天体测量发展的需要和低纬子午环课题目标的要求，叙述了该仪器的总体设计要求和提出这些要求的理由，强调指出了如何高精度地测定仪器的制造误差、安装误差和重力变形、热变形的影响，以及如何消除测量仪器误差的各设备的零点偏差及其漂移的影响，以便保持仪器观测系统的长期稳定性。     

The results of the third geodetic campaign in the local geodynamic test area of the MAO NAS of Ukraine

The high-precision coordinates of reference (reduction) points of stations located in the geodynamic area of the MAO NAS of Ukraine were determined in the local topocentric coordinate system. The local geodetic ties (eccentricities) between the reference points of the GPS station “Kiev/Goloseev” and satellite laser location station “Goloseev-Kiev” that are equal to 100.2358 m, ?11.0398 m, ?85.8256 m on the X, Y, Z axes, respectively, were obtained in the ITRF97 system as of the epoch 1997.0. The coordinates of the reference point of the station “Goloseev-Kiev” were determined in the ITRF97 system as of the epoch 1997.0 by adding local geodetic ties to the coordinates of the reference point of the GPS station “Kiev/Goloseev.” They were compared with the estimates of the coordinates of these stations obtained by the methods of cosmic geodesy and geodynamics. The local deformations of the geodynamic area that took place in the 1997–2006 period were estimated and the conclusion was made about the existence of certain trends with respect to the local displacements of the points of the geodynamic area of the MAO NAS of Ukraine.     

Comparisons of CME Morphological Characteristics Derived from Five 3D Reconstruction Methods

We compare different methods to reconstruct three-dimensional (3D) coronal mass ejection (CME) morphology. The explored methods include geometric localisation, mask fitting, forward modelling, polarisation ratio, and local correlation tracking plus triangulation. These five methods are applied to the same CME event that occurred on 7 August 2010. Their corresponding results are presented and compared, especially in their propagation direction and spatial extent in 3D. We find that the mask fitting and geometric localisation methods produce consistent results. Reconstructions including three-view observations are more precise than reconstructions done with only two views. Compared to the forward modelling method, in which an a priori shape of the CME geometry is assumed, the mask fitting has more flexibility. The polarisation ratio method makes use of the Thomson scattering geometry. We find that spatially the 3D CME derived from the mask fitting lies mostly in the overlap region obtained with the polarisation method using data from STEREO. In addition, the mask fitting can help resolve the front/back ambiguity inherent in the polarisation ratio method. However, the local correlation tracking plus triangulation did not show consistent results with the other four methods. This method performed poorly, primarily because the two STEREO spacecraft had a large angular separation. Under these circumstances, it is difficult to identify points taken from independent images that correspond to the same physical feature. Excluding the local correlation tracking method, the latitude of the CME??s centre of gravity derived from the other methods deviates within 1^°, and the longitude differs within 19^°.     

The effect of the internal structure of Mars on its seasonal loading deformations

Mars is continuously subjected to surface loading induced by seasonal mass changes in the atmosphere and ice caps due to the CO₂ sublimation and condensation process. It results in surface deformations and in time variations of gravity. Large wavelength annual and semi-annual variations of gravity (particularly zonal coefficients ΔJn) have been determined using present day geodetic satellite measurements. However loading deformations have been poorly studied for a planet like Mars. In this paper, we compute these deformations and their effect on spacecraft orbiting around Mars. Loading deformations of terrestrial planet are typically investigated assuming a spherical planet, radially symmetric. The mean radial structure of Mars is not well known. In particular the radius of the liquid or solid core remains not precisely determined. One may then wonder what is the effect of these uncertainties on loading deformations. Moreover, Mars presents a strong topography and probably large lateral variations of crustal thickness (relative to the Earth). The paper answer the questions of what is the effect of such lateral heterogeneities on surface deformations, and is the classical way to calculate loading deformation well adapted for a planet like Mars. In order to answer these questions we have investigated theoretically loading deformations of Mars-like planets. We first investigated classical load Love numbers. We show that for degrees inferior to 10, the load Love numbers mainly depend on the radius of the core and on its state, and that for degree greater than 10, they depend on the mean radius of mantle-crust interface. Using a General Circulation Model (GCM) of atmosphere and ice caps dynamics we show that loading vertical displacements have a 4-5 cm magnitude and present a North-South pattern with periodic transitions. Finally we investigated the effect of lateral variations of the crustal thickness on these loading deformations. We show that thickness heterogeneities perturb the deformations and the time variation of gravity at about 0.5%. However this perturbation on ΔJn is only about 1‰ due to main direct attraction of surface fluid layers. We conclude that lateral variations of crustal thickness are today negligible. However, observation of load Love numbers would bring information on the radial internal structure of the planet, particularly on the core radius. ΔJn study would permit to infer the load Love number , particularly for degree 2 and 3, knowing surface fluid layer dynamics. However load Love numbers are quite small (about 0.05), and despite the present good agreement between GCM and ΔJn observations, will only be estimated in the near future when a slightly better precision in observation and modeling will make it possible to infer these numbers. The investigation of load Love number , which are larger than numbers, would be particularly interesting. It would permit to study degree 1 contribution of atmosphere and ice caps dynamics, which is the most important component of surface fluid dynamics on Mars. Surface displacement measurements would be necessary on a few places near the pole regions, which may be possible in the future, with a project involving precise positioning of a lander on the surface of Mars.     

Measuring and analyzing thermal deformations of the primary reflector of the Tianma radio telescope

The primary reflector of the Tianma Radio Telescope (TMRT) distorts due to the varying thermal conditions, which dramatically reduces the aperture efficiency of Q-band observations. To evaluate and overcome the thermal effects, a thermal deformations measurement system has been established based on the extended Out-of-Focus holography (e-OOF). The thermal deformations can be measured in approximately 20 min with an illumination-weighted surface root mean square (RMS) accuracy of approximately 50 μm. We have measured the thermal deformations when the backup and front structure were heated by the sun respectively, and used the active surface system to correct the thermal deformations immediately to confirm the measurements. The thermal deformations when the backup structure is heated are larger than those when the front structure is heated. The values of half power beam width (HPBW) are related to the illumination-weighted surface RMS, and can be used to check the thermal deformations. When the backup structure is heated, the aperture efficiencies can remain above 90% of the maximum efficiency at 40 GHz for approximately two hours after one adjustment. While the front structure is heated, the aperture efficiencies can remain above 90% of the maximum efficiency at 40 GHz, and above 95% after one adjustment in approximately three hours.     

以基线长度变化率为约束估算VLBI站的垂直形变率

基于NNR-NUVEL-1A地球板块运动模型和ITRF2000地球参考架的三维VLBI站速度矢量,采用实测的VLBI基线长度变化率作为约束,重新估计了部分国际VLBI站的局部或区域性地壳的垂直形变,并与国际地球参考架ITRFs解和VLBI全球解GLB2003,VTRF2003和VTRF2005的结果进行了比较。结果表明,欧亚板块的URUMQI站和太平洋板块的KWAJAL26站,南极OHIGGINS站的垂直形变率、ITRFs解和VLBI全球解存在6-15mm/a的差异,北美YUMA站可能有15-31mm/a 的垂直形变率,而美国西部太平洋板块的San Francisco(PRESIDIO)站的垂直形变率还有待进一步的研究。此外,SC-VLBA,CRIMEA和EFLSBERG站的垂直形变率、ITRFs解和VLBI全球解的差约为1-6mm/a。用不同方法得到的VLBI站的水平形变率解有较好的一致性。