低纬子午环电水准的成功和不足之处

本文叙述了电水准的采用能适应低纬子午环的高精度要求,分析了水平差的个别测量值产生跳变的原因：既有其本身的结构问题,也有仪器其它部件的不良影响。文中还介绍了对电水准作局部改善的情况。     

电水准的参数测定

介绍了低纬子午环的水平差分两部分测定的要求和电水准的实际配置情况，分析了在这种配置中系统参数增多的原因，叙述了测定这些参数的方法，并提出在参数测定后如何保持系统状态的要求。     

电容式气泡水准器及其在中星仪上的应用

本文介绍了利用电容传感原理研制的电容式气泡水准器。其传感器是由粘于水准管玻璃表面上的四块铝箔组成。它们构成两个差动电容,测定两电容之差,即可得到气泡的位置。本装置测量范围为12角秒,精度为±0.1角秒.测量结果实现数字化及自动打印记录,并与目视兼容。应用于中星仪观测时,大大压缩了人差,提高了测时精度。     

光电中星仪的人差

本文通过光电中星仪现有观测资料的分析,证实了光电中星仪存在着以水准读数误差为主要因素造成的人差,并提出一种利用光学读水准装置来测定水平差,使人差得到明显的缩减.     

甚长基线干涉仪测量佘山财区的地壳垂直运动

本简述了VLBI测量地壳垂直运动的原理，并给出了利用上海天台VLBI站自1988年以年的VLBI国际联测资料及VLBI站与邻近基岩水准点的水准联测资料所得到上海佘山地区地壳垂直运动的初步结果为－1mm/yr。最后还提出进一步提高VLBI垂直运动的测量精度及全面了解整个上海地区地壳垂直运动的现状的意见。     

测定子午仪水平轴水平差的轴准直方法

本文就转轴观测的子午仪,提出了以水银面为基准、用轴准直方式测定水平轴的真实水平差的方法,以代替常用的受多种因素影响的水准管测定法。文中还对这种方法可能达到的精度作了估计。     

紫金山天文台纬度的测定

所用仪器为蔡司厂100毫米口径物镜、100厘米焦距的子午仪.该仪器附有二具泰尔科特水准.便用泰尔科特法测纬,用下式     

简讯

简讯青岛观象台“六一”免费向少年儿童开放为庆祝“六一”儿童节，已有近百年历史的中国科学院紫金山天文台青岛观象台于“六一”期间免费向广大少年儿童开放。５００余名少年儿童通过３２厘米折射天文望远镜，饶有兴趣地观看了太阳黑子。参观了“中华人民共和国水准原点...     

中日卫星双向法时间传递与全球TWSTT合作

双向法卫星时间传递(TWSTT)是比 GPS 共视法精度更高的洲际时间频率比对方法,比对精度可达亚毫微秒。国际权度局(BIPM)向世界各国时频实验室推荐使用TWSTT 方法,支持组建亚、欧、美三大洲以及全球的高精度比对网,提高国际原子时的水准。同时,国际秒定义咨询委员会(CCDS)专门成立了 TWSTT 工作组,进行推动     

低纬子午环的电水准器与水平差测定

本文介绍了低纬子午环上电水准器的工作原理；讨论了电水准器在测定定位盘上盘的水平差时，其Ｄｅｔｉｃｏｎ的比例尺的测定方法及其测量精度；讨论了电水准器中狭缝倾斜量的测量方法；最后给出了水平差的测量范围以及可达到的精度，证明低纬子午环对轴系的要求是比较低的，而水平差的测量精度是相当高的。     

Interannual sea level variability in the South China Sea and its response to ENSO

Sea level observed by altimeter during the 1993–2004 period, thermosteric sea level from 1945 through 2004, and tide gauge records are analyzed to investigate the interannual variability of sea level in the South China Sea (SCS) and its relationship with ENSO (El Niño and Southern Oscillation). Both the interannual variations of the observed sea level and the thermosteric sea level are closely related to ENSO. An ‘enigma’ that the SST and sea level in the SCS have inverse response to ENSO is revealed. It is found that the thermosteric sea level has an excellent correspondence to seawater temperature at 100 m depth, and their variations are unsynchronized to SST. Detailed analysis denotes that the warming of seawater occurs only in the upper 75 m during and after the mature phase of El Niño, while the cooling appears in the layers deeper than 75 m during El Niño years. The volume transports between the SCS and the adjacent oceans and the anomalous Ekman pumping contribute a lot for the sea level fall in the developing stage of El Niño, while the mass exchange, which is dominated by precipitation, plays a more significant role in the following continuous negative sea level anomalies.     

Acoustic-gravity waves in the thermosphere of Venus

Properties of acoustic-gravity waves in the upper atmosphere of Venus are studied using a two-fluid model which includes the effects of wave-induced diffusion in a diffusively separated atmosphere. In conjunction with neutral mass spectrometer data from the Pioneer Venus orbiter, the theory should provide information on the distribution of wave sources in the Venus upper atmosphere. Observed wave structure in species density measurements should generally have periods ?30–35 min, small N₂, CO, and O amplitudes, and highly variable phase shifts relative to CO₂. A near resonance may exist between downward phase-propagating internal gravity and diffusion waves near the 165-km level at periods near 29 min. As a result, if very large He wave amplitudes are observed near this level, it will indicate that the wave source is below the 150- to 175-km level and that the exospheric temperature is close to 350°K. Wave energy dissipation may be an important mechanism for heating of the nightside Venus thermosphere. Large-density oscillations in stratospheric cloud layer constituents are also possible and may be detectable by the Pioneer Venus large probe neutral mass spectrometer.     

Sea level forcing in the Mediterranean Sea between 1960 and 2000

Sea level trends and inter-annual variability in the Mediterranean Sea for the period 1960–2000 is explored by comparing observations from tide gauges with sea level hindcasts from a barotropic 2D circulation model, and two full primitive equation 3D ocean circulation models, a regional one and the Mediterranean component of a global one,. In the 2D model, 50% of the sea level variance was found to result from the wind and atmospheric pressure forcing. In the 3D models, 20% of the sea level variance was explained by the steric effects. The sea level residuals at the tide gauges locations, calculated by subtraction of the 2D model output from the sea level observations are significantly correlated (r = 0.4) with the steric signals from the 3D models. After the removal of the atmospheric and the steric contributions the tide-gauge sea level records indicate a period where sea level was stable (1960–1975) and a period where sea level was rising (1975–2000) with rates in the range 1.1–1.8 mm/yr. A part of the residual trend can be explained by the contribution of local land movements (0.3 mm/yr) while its major part indicates a global signal, probably mass addition, appearing after 1975.     

Flare variability in the close binary FL Vir

The results of U -filter flare monitoring of the binary flare star FL Vir = Wolf 424 is presented. 57 flares with energies between  2 × 10²⁸  and  2 × 10³¹ erg  were recorded in 20 h of observation. The properties of flare occurrence and flare time-scales are analysed, and the flare activity level in 1980 April is determined to be   L _f( U ) = 8.0 × 10²⁶ erg s⁻¹  . This is larger than previously published results and may indicate a variation in the flare activity level on a time-scale of years. An analysis of existing data indicates that the flare activity level correlates with the relative orbital positions of the stars.     

On the ionisation of hydrogen in optical flares

Non-steady state and non-LTE effects on the ionisation equilibrium of hydrogen in optical flares are considered in terms of a two-level hydrogen atom. It is shown that, just as in the quiet low chromosphere, the ionisation equation is controlled by spontaneous recombination to the second level and by photoionisation from this level by photospheric radiation, and is independent of the nature of the flare energy input mechanism.Adjustment of the ionisation then occurs on the recombination time scale which is short compared to the flare heating time scale. Consequently the ionisation is given by a simple LTE-modification of Saha's equation at the instantaneous electron temperature obtained from the energy equation. These conclusions are contrasted with those of previous authors who, by using one-level atoms only, have omitted the optically thin Balmer continuum which dominates the optically thick Lyman transitions.     

Temporal and spatial variability of annual extreme water level in the Pearl River Delta region, China

This paper is concerned with identifying the spatial and temporal patterns in the annual maximum and minimum water level in the Pearl River Delta (PRD) region. The Mann–Kendall test and Pettitt test are used to detect trends and abrupt change points, and the Trend Free Pre-Whitening (TFPW) approach then eliminates the effect of serial correlation in data series with significant autocorrelation. Approximately fifty years of the annual hydrological variables from 18 stations in the three major rivers (the West River, the North River, and the East River) are examined. The changing trends of the extremes in water level show different features in different parts of the PRD region. Generally speaking, in the upper part of the delta, the water levels show a decreasing trend while in the middle and lower part there is an increasing trend. This spatial pattern of the extreme water level variation is unlikely to be due to a long-term change in stream flow in the PRD region because the water level changes do not always coincide with the extreme stream flow variations. Sand excavation initiated in the 1980s and continuing for more than 20 years in almost all tributaries around the PRD region is one of the most serious intensive human activities affecting water levels. The result of the Pettitt test indicates that most abrupt change points occurred in 1980s–1990s, which reveals that sand excavation and channel regulation are likely to have been the most significant factors contributing to the change over this period. These anthropogenic activities modify the annual extreme water level dramatically in a way that affects the morphology of river channels and estuaries of the PRD and also the redistribution of discharge. However, there are differences in the geographic locations of significant trends for the water level investigated, which implies that these impacts are not spatially uniform.     

我国天文台及潜在台址所在地区Fried参数γ0的计算与统计分析

用1986-1995年的10年探空气象资料，在塔塔尔斯基模式下，计算了我国天语言台及候选台址所在的10个地区的Fried参数r0。给出了地面、900米、1500米、3000米、5000米各度上的r0年平均值。在3000米高度上冬季丽江视宁度最好，夏季酒泉最好，均达到相应季节定日4301米高度上视宁度水平。     

On Determining the Vertical Structure of the Aerosol Component in the Atmosphere of Saturn

Relying upon the values of the geometric albedo of Saturn obtained in the methane absorption bands at λ = 887, 864, 842, 727, and 619 nm in 1993, how the aerosol and gaseous scattering components of the effective optical depth change with depth in the atmosphere of the planet are analyzed. The model of homogeneous spherical aerosol particles is used. For the altitude levels in the pressure range from 0.18 to 1.5 bar, that the parameters of aerosol particles used in the analysis are close to their actual values is confirmed. Above the level of 0.054 bar, the presence of stratospheric aerosol was detected. At least seven peculiarities were found in the vertical structure of the cloud cover of the upper atmosphere of Saturn. The altitude position of the maximum relative concentration of aerosol was estimated at approximately a level of 0.3 or 0.12 bar given the relative concentration of methane as 0.0021 or 0.0533, respectively. In the atmospheric layers of Saturn, where the pressure is larger than 0.44 bar, the cloud extended in altitude and containing no distinguishable aerosol layers was found. In the layers deeper than 1.5 bar, indications of probable changes in the parameters of aerosol particles were detected.     

Determining the motion of the Solar system relative to the cosmic microwave background using Type Ia supernovae

We estimate the Solar system motion relative to the cosmic microwave background using Type Ia supernovae (SNe) measurements. We take into account the correlations in the error bars of the SNe measurements arising from correlated peculiar velocities. Without accounting for correlations in the peculiar velocities, the SNe data we use appear to detect the peculiar velocity of the Solar system at about the 3.5σ level. However, when the correlations are correctly accounted for, the SNe data only detect the Solar system peculiar velocity at about the 2.5σ level. We forecast that the Solar system peculiar velocity will be detected at the 9σ level by GAIA and the 11σ level by the Large Synoptic Survey Telescope. For these surveys, we find the correlations are much less important as most of the signal comes from higher redshifts where the number density of SNe is insufficient for the correlations to be important.