厄尔尼诺与太阳黑子和大气环流的关系及其预报

通过对1956-1996年11次厄尔尼诺现象与太阳黑子、大气环流的关系分析,发现有一定规律,用概率统计方法建立起厄尔尼诺的预报模式。     

地球自转速度的年变化

本文利用宋贯一等（2006）发表的“极移的成因及其移动特征”一文中的自转轴受迫摆动资料,从理论上推断出地球自转速度年变化的特征.结果证明,理论计算出的地球自转速度年变化曲线形态特征与观测曲线形态特征十分吻合.从而得出,太阳辐射光压在南、北半球的不平衡分布是引起地球自转速度年变化的主要原因.     

A note on strong mass loss from early sun and warm and wet Mars

Recently, the possibility of strong mass loss from an early sun has been proposed in connection with the lithium depletion problem along with early solar system problems. However, the time scale for this enhanced mass loss is uncertain. Using an empirical relation for the dependence of the Martian surface temperature on solar luminosity and surface pressure, we find that the mass loss time scale for a 1.1 M sun should be about 1 × 10⁹ years or longer if Mars had liquid water on its surface 3.8 billion years ago. The minimum surface pressure on early Mars should be about 5 bars of CO₂.     

Probability Distribution of Surface Wave Slope Derived Using Sun Glitter Images from Geostationary Meteorological Satellite and Surface Vector Winds from Scatterometers

The probability distribution of the sea surface slope has been estimated using sun glitter images derived from the visible wavelength radiometer on the Geostationary Meteorological Satellite (GMS) and surface vector winds observed by spaceborne scatterometers. The brightness of the visible images is converted to the probability of wave surfaces which reflect the sunlight toward GMS in grids of 0.25° × 0.25° (latitude × longitude). The slope and azimuth angle required for the reflection of the sun's rays toward GMS are calculated for each grid from the geometry of GMS observation and location of the sun. The GMS images are then collocated with surface wind data observed by three scatterometers. Using the collocated data set of about 30 million points obtained in a period of 4 years from 1995 to 1999, the probability distribution function of the surface slope is estimated as a function of wind speed and azimuth angle relative to the wind direction. The results are compared with those of Cox and Munk (1954a). The surface slope estimated by the present method shows a narrower distribution and much less directivity relative to the wind direction than that reported by Cox and Munk. It is expected that their data were obtained under conditions of growing wind waves. In general, wind waves are not always developing, and the slope distribution might differ from the results of Cox and Munk. Most of our data are obtained in the subtropical seas under clear-sky conditions. This difference in the conditions may be the reason for the difference of slope distribution. This revised version was published online in July 2006 with corrections to the Cover Date.     

光谱仪测量离水辐射亮度的方法

概述了利用光谱仪在水面上方进行水表光学特性测量和基本原理与测量方法，以及处理和计算离水辐射亮度、归一化离水辐射亮度及遥感反射比等水表光学特性参数的主要方法。对1998年东海3个站点的测量数据进行了处理和分析，并与剖面法计算结果进行了比较。     

SOLAR-TERRESTRIAL AND CLIMATIC PHENOMENA IN RELATION TO SOLAR INERTIAL MOTION

The time series of solar and volcanic activities have been processed to show, mostly by means of statistical characteristics, the exceptional and recurring pattern of these phenomena in the intervals of the exceptional and recurring pattern of solar motion, i.e. in the intervals of the Sun's motion along the trefoils which reoccur in steps of 178.7 years. Nearly the same sets of five sunspot cycles have been found in the latest trefoil intervals (1730–1780 and 1910–1960), their length being constant and equal to 10 years (cycles No. 15–19). The steadily attenuated volcanic activity have been pointed out in the three latest trefoil intervals. The long-term maxima of surface air temperature occured in the central decades of the trefoil intervals. The results indicate a primary role of solar motion in a causal chain of ST-relations and a need of taking the Solar System as a whole into account to explain climatic changes. The solar motion can be computed in advance. Predictive assesments, so far in form of analogies, have been made: Because the solar motion in the next decades will be chaotic, lower and longer solar cycles (with irregular length), ocurrence of huge volcanic events and a decrease of global surface air temperature can be expected.     

手持式消光光度计的研制及用于掺杂牛奶的现场快速检测

自行设计新型消光池,研制了一种廉价的手持式消光光度计,并在此基础上建立了掺杂牛奶的现场检测方法。实验结果表明,所建立的方法无需对牛奶进行复杂处理,可对常见掺杂(如搀水、米汤、奶粉、豆浆、尿素等)牛奶和含重金属离子汞的牛奶,进行现场检测。由于采用新型消光池,有效地减小了蛋白质粒子因重力沉降所带来的误差,能够成功区分同密度劣质牛奶。该方法灵敏度高,对掺水牛奶的检出限低于2%,对重金属(如汞)的检出限为0.005μg/g。单个样品测定时间不到2 min,适合于牛奶品质的现场快速检测。     

Magnetic reconnection in solar flares

Abstract

The magnetic energy stored in the corona is the only plausible source for the energy released during large solar flares. During the last 20 years most theoretical work has concentrated on models which store magnetic energy in the corona in the form of electrical currents, and a major goal of present day research is to understand how these currents are created, and then later dissipated during a flare. Another important goal is to find a flare model which can eject magnetic flux into interplanetary space. Although many flares do not eject magnetic flux, those which do are of special importance for solar-terrestrial relations since the ejected flux can have dramatic effects if it hits the Earth's magnetosphere. Three flare models which have been extensively investigated are the emerging-flux model, the sheared-arcade model, and the magnetic-flux-rope model. All of these models can store and release magnetic energy efficiently provided that rapid magnetic reconnection occurs. However, only the magnetic-flux-rope model appears to provide a plausible mechanism for ejecting magnetic flux into interplanetary space.     

铀的紫外-可见分光光度分析专用试剂包的开发研究

利用新开发的铀试剂包和自行研制的手持式光度计,建立了环境水样中痕量铀的现场分析新方法。实验中分别考察了缓冲试剂、显色剂、掩蔽剂的选择及用量、显色时间稳定性、波长等主要因素对铀分析测定的影响。结果表明,与经典紫外-可见分光光度法相比,此方法具有操作简便、省时、满足现场测定要求等优点。     

甘肃金塔地区大气对太阳射电辐射吸收的测量研究

2008年8月1日,在我国西北的新疆、内蒙、甘肃等地区可以观测到一次日全食的天象,紫金山天文台太阳射电团组在甘肃省金塔用两架太阳射电望远镜对这次日全食进行了观测,并成功地取得了观测资料.为了科学分析观测资料,在日全食的前两天,实测了当地的大气吸收.着重分析这些观测数据,结合太阳射电方法,测得在λ=2.4 cm和λ=8....