VLBI观测双线极化条纹拟合方法

提出了一种可用于下一代VLBI观测系统(VGOS)的双线极化条纹拟合方法。现有的VLBI观测模式采用的是右圆极化(RCP),而VGOS系统采用的是双线极化。本文方法包括校正和组合条纹拟合两部分。校正部分选择一颗强源作为参考源,分别得到不同极化方式下的通道时延及相位校正数据,用于目标源的校正。组合条纹拟合部分将4种极化分量的可见度数据组合成伪Stokes分量,通过搜索差分星位角使伪Stokes分量的幅值达到最大,从而获得最终的时延观测量。与单极化条纹拟合相比,组合极化获得的条纹具有更高的信噪比(SNR)及更小的条纹相位弥散度。     

组合电离层残差与改进的码相伪距探测与修复周跳研究

传统码相组合算法能探测7～8周以上大周跳,而传统的电离层残差法仅对于±4周以内的周跳可实现唯一分离,这限制了两者组合的应用.针对这一问题,对码相组合探测与修复周跳方法进行改进,使得改进的码相组合与电离层残差法能够完全探测周跳.经理论与实验分析,组合改进的码相组合法与电离层残差法两者结合能够完全探测采样间隔小于10 s观测数据中的周跳,对动态非差观测值数据的周跳自动探测与修复有极佳的效果.     

Radio properties of the Shapley Concentration — II. J1324–3138: a remnant of a radio galaxy in the Abell cluster A3556?

In this paper we present a detailed study of the radio galaxy J1324–3138, located at a projected distance of 2 arcmin from the centre of the Abell cluster of galaxies A3556, belonging to the core of the Shapley Concentration, at an average redshift of z  = 0.05. We have observed J1324–3138 over a wide range of frequencies: at 327 MHz (VLA), 843 MHz (MOST), and at 1376, 2382, 4790 and 8640 MHz (ATCA).   Our analysis suggests that J1324–3138 is a remnant of a tailed radio galaxy, in which the nuclear engine has switched off and the radio source is now at a late stage of its evolution, confined by the intracluster gas. The radio galaxy is not in pressure equilibrium with the external medium, as is often found for extended radio sources in clusters of galaxies. We favour the hypothesis that the lack of observed polarized radio emission in the source is a result of Faraday rotation by a foreground screen, i.e. the source is seen through a dense cluster gas, characterized by a random magnetic field.   An implication of the head–tail nature of the source is that J1324–3138 is moving away from the core of A3556 and that, possibly, a major merging event between the core of A3556 and the subgroup hosting J1324–3138 has already taken place.     

射阳港区双导堤建设前后冲淤变化及成因研究

基于近年来射阳港区水下地形数据和定点全潮水文观测资料,分析了双导堤建设前后冲淤变化特征,并对其成因进行了初步探讨。研究结果表明,研究区近6年来总体上以淤积为主,净淤积量约为65.23×106m3,年均净淤积速率约为7.9 cm/a;淤积区域主要分布于导堤两侧浅水区,侵蚀区域主要分布于导堤口附近。2008-2013年间研究区冲刷、淤积和相对稳定区域面积分别占15%、55%和30%。堤口东侧的SSW02站实测最大流速为1.54 m/s,北堤北部的SSW01站为1.4 m/s,无论是涨潮还是落潮,堤口均大于导堤北侧;导堤产生了沿堤水流和口门回流,改变了导堤两侧附近海域潮流方向并增大了口门处的沉积动力。研究区泥沙运动方式主要表现为波浪掀沙、潮流输沙;区域海流泥沙的沿程落淤和导堤挡流效应导致导堤两侧出现淤积,导堤产生的回流促使堤口冲刷和堤内泥沙回淤。导堤引起的局部流场变化是海底冲淤格局重新分布的主因。     

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关于数字化记录中前兆信号的分析

介绍了如何用MATLAB工具软件—小波分析的基本理论对数字信号进行数字滤波,着重分析和研究了呼和浩特地震台形变观测资料出现各种信号,提出了小波分析理论对台站实际工作的重要性。     

内蒙古高温酷暑天气的气候学特征和环流类型

利用1971—2008年内蒙古117个观测站日最高气温资料,结合同期的NCEP再分析资料,分析了内蒙古高温酷暑天气的气候学特征。结果表明:内蒙古高温酷暑天气地域差异大,高温中心在阿拉善盟沙漠地区的拐子湖,年平均35℃高温日数达32天,也是全国的高温区之一;内蒙古的高温天气年日数有增长趋势,高温酷暑的影响在增强;内蒙古高温酷暑集中出现在盛夏季节6—8月,7月发生最多,占一半以上;最高气温出现在每日的14—17时,气温日较差大,多为干热天气。通过对内蒙古较大范围的64次高温天气过程分析总结,将内蒙古高温酷暑天气分为蒙古暖脊型、贝加尔湖高压坝型、副高西进型、乌拉尔山高脊型4个类型。大陆暖高压脊的强烈发展和维持与内蒙古高温酷暑天气密切相关。     

自动与人工观测的气压差异分析

利用陕西省97个气象站2004—2007年间自动与人工平行观测期间的资料,分析了陕西和陕西不同地域人工与自动观测气压的差异并对气压月、年平均值进行了显著性检验。结果表明:人工观测比自动观测日平均气压平均偏高0.21 hPa,标准差为0.30 hPa;气压差值有明显的地域特征;气压对比差值的日、月变化规律明显;DYYZ和CAWS系列测压仪的性能没有明显差异;自动与人工观测时间不同步对定时值有一定影响,但对气候分析没有影响;校准值随时间漂移是气压传感器的主要误差源之一;自动站所测气压可与人工站气压连续使用。     

CCD astrometric observations of 2017 VR12, Camillo and Midas

We have observed three near-Earth objects(NEOs), 2017 VR12, Camillo and Midas, during 2018.The observations were made with the 1-m telescope, operated by Yunnan Observatories, over two nights.Their precise astrometric positions are derived from 989 CCD observations. The theoretical positions of asteroids are retrieved from the Jet Propulsion Laboratory(JPL) Horizons System and Institut de M′ecanique C′eleste et de Calcul des ′Eph′em′erides(IMCCE). The positions of three asteroids are measured with respect to stars in the Gaia DR2 star catalog. For 2017 VR12, the means(O-C) of right ascension and declination are -0.090′′and-0.623′′respectively based on the published JPL ephemeris, but the corresponding means(O-C) are 3.122′′and-0.636′′based on the published IMCCE ephemeris. The great difference in declination could be explained by several factors.(1) The degraded CCD images caused by the fast apparent motion of the objects lead to a reduction in positioning accuracy.(2) The poor timing system may introduce systematic errors, especially in the high speed direction.(3) The asteroid may be perturbed by Earth when it approaches the Earth too closely. These astrometric results demonstrate that the centroid centering method can reduce the dispersion of non-Gaussian images as compared with the PSF modeling method.For Camillo and Midas, the astrometric results are consistent based on the two ephemerides. Implementing a high-precision timing system, and analyzing some astronomical effects and geometric distortions in CCD images should be carefully considered in future works.