GNSS掩星电离层观测的模拟试验

利用真实的电离层GNSS掩星轨道数据，采用全球3D射线追踪程序，从笛卡尔坐标系下的三维Haselgrove方程和Budden方程出发，利用“打靶”的方法来确定从指定的GNSS位置到指定的低轨卫星位置正确的射线路径，进而模拟出电离层对GNSS信号的时间延迟。然后，通过反演得到了电子密度剖面。分别 模拟了太阳活动对GNSS掩星信号电离层时延的影响，以及GNSS掩星信号电离层时延的年变化和日变化情况，结果发现太阳活动对电离层GNSS信号时延有较大影响，GNSS掩星信号电离层时延在一年和一天中都有较大起伏。     

地基火星反演技术中的掩星坐标系

我国开展的火星探测萤火计划(YH-1)的研究中,用地基掩星观测反演火星大气是其中一个重要的组成部分.由于各种观测资料处于日心和火星坐标系中,不易利用和处理.本文通过矩阵变换建立掩星坐标系,把原始的观测资料统一到同一个坐标系中,为掩星数据的分析处理提供了技术准备.     

GNSS无线电掩星数据的电离层校正和统计优化

为了消除电离层折射效应对全球卫星导航系统无线电掩星信号的影响,首先对掩星数据进行电离层订正,然后进行统计优化,最后与欧洲中期数值预报中心的数据比较,验证电离层校正和弯曲角统计优化对弯曲角廓线反演精度提高的效果。结果表明:无论是模拟仿真还是真实的掩星事件,电离层校正后,50km以上弯曲角廓线仍呈现高频振荡的形式;统计优化后,50km以上弯曲角廓线近似呈现与中性大气相同的分布规律,基本消除了电离层小扰动和接收机热噪声对高层弯曲角廓线的影响;弯曲角统计优化能有效提高弯曲角反演折射率廓线时的精度。     

火星探测研究结果分析

火星是地球的近邻,很多方面的特征与地球相似.有观点认为,火星是地球的未来,即地球经过长期演化,其内部机构、地表和空间环境可能会变成火星现在的状况.因而在与地球比较的基础上,开展火星探测和研究,不仅对于探索火星及其空间的奥秘,而且对于认识地球都有重要的意义.本文对空间飞行器所取得的有关火星的探测结果(包括火星内部结构和火星表面、火星大气、火星电离层和磁层,以及太阳风与火星的相互作用等)进行了分析和概述,内容涉及火星内部化学成分、火星岩石中的元素、火星表面地形和尘暴,火星大气的光化学过程、火星大气的季节变化和大气中的同位素,火星上过去全球尺度的磁场和现在的局域强磁场观测,火星全球尺度偶极磁场的可能反转,太阳风与火星电离层相互作用所形成的感应型磁层等科学问题.结合目前火星探测和研究的现状,对火星研究的主要科学问题和意义进行了简单描述.     

基于COSMIC数据开展全球电离层foF2建模及变化特征研究

电离层foF2是短波通信、天波超视距雷达系统所需的关键环境参数,使用2006—2014年COMSIC(constellation observing system for meteorology, ionosphere, and climate)掩星电离层数据和多项式方法,自主构建了高精度全球电离层foF2经验模型,并使用2015—2019年观测数据进行独立检验。本模型结果与建模及独立检验时段电离层foF2观测数据的相关系数分别为0.948和0.937,平均偏差分别为2.38%和3.08%,相对误差分别为11.72%和12.69%。利用该模型研究了电离层foF2时空变化特征,结果表明电离层foF2日夜变化幅度随纬度增加而变大,春秋分季期间南半球日夜变化幅度显著高于北半球,而夏季半球则远低于冬季半球。电离层foF2季节变化幅度随纬度增加而变大,夜间电离层foF2的季节变化以年特征为主,白天则包含了显著的年、半年特征,夜间季节变化幅度明显高于白天,南半球显著高于北半球。电离层foF2中纬槽现象主要出现在春秋分季夜间,经度方向四波结构主要出现在太阳活动低年和春秋分季期间。     

ROPP掩星数据反演软件及其精度分析

GPS掩星探测技术已成为地球大气和电离层探测的重要手段。介绍了无线电掩星数据反演地球大气参数的原理方法以及处理软件ROPP的功能和模块构成;并详细阐述了模块的算法原理。依据掩星探测几何关系,在球对称模式下利用ROPP软件进行参数配置,对COSMIC掩星数据进行预处理,由阿贝尔积分反演得到大气折射率廓线;并利用一维变分反演方法得到大气参数如温度、湿度和压强的廓线。反演结果图示说明,与CDAAC处理数据进行了比较和误差分析,分析表明折射率、温度、压强和湿度的吻合程度较好,30km以下折射率误差约在5%范围内;同时给出了误差的来源及分析。     

大气电离层对GPS测量影响的探讨

本文从GPS测量误差来源出发,详细的分析了大气电离层的结构、电离层的折射延迟数学表示方式以及延迟对GPS测量的具体影响。最后,本文深入探讨了格网模型修正电离层延迟的方法,提出了站际分区新型格网模型值的具体确定方法,并通过实际试验得到数据证明了该方法的优越性。     

低纬电离层闪烁对GPS观测值及其导航定位的影响

电离层闪烁对全球定位系统(GPS)的影响已经被认为是GPS现代化后面临的主要问题.利用低纬地区电离层闪烁监测接收机(18.34°N, 109.62°E)在2012-08-01～31的GPS闪烁数据和观测数据,开展了电离层闪烁对GPS观测值及单点定位的影响研究.研究结果表明,电离层闪烁可以导致GPS卫星信号发生衰减,最大衰减幅度达20 dB-Hz;相比于GPS L1观测值,电离层闪烁对GPS L2影响更大;电离层闪烁可导致周跳的发生,统计表明,每100个强电离层闪烁事件(S_40.5)可以导致21个周跳发生,而100个弱电离层闪烁事件(0.2S_4≤0.5)仅导致6个周跳发生;强电离层闪烁环境下,卫星信号会遭遇失锁现象,从而破坏卫星几何分布结构,导致GPS导航定位性能降低;相比正常的电离层环境,电离层闪烁活跃环境下的GPS单点定位精度降低了23%.     

电离层对耀斑响应的GPS观测研究

利用1997～1999年全球日地电离层观测卫星的耀斑观测资料以及全球定位系统(GPS)网的观测资料,对不同级别耀斑爆发期间的电离层总电子含量(TEC)随时间的变化特点、TEC增幅及其与X射线最大辐射通量之间的关系进行了研究.利用缓变型耀斑爆发期间的GPS观测数据,分析了电离层对此类耀斑的响应特点.     

单双频GPS混合观测高精度单频精密单点定位

精密单点定位不受局域观测和设施影响,有利于形变监测.为降低电离层延迟对单频精密单点定位结果的影响,提出了单双频混合观测的方法.但单频精密单点定位仍受相位非小数偏差影响,为此提出采用双差模糊度应用于单频精密单点定位.观测数据解算结果表明,电离层延迟精度优于1 cm,满足单频精密单点高精度定位的要求,对应的单频精密单点定位...     

电离层的朔望月周期变化

 电离层应该存在月球引力引起的朔望月周期变化,但一直没有观察到。2004年6月29日,法国发射了地震电磁监测卫星DEMETER,它是近极地太阳同步圆轨道卫星。本文将DEMETER卫星搭载的朗缪尔探针观测数据分为日侧半轨数据和夜侧半轨数据两组,对两组数据进行重采样和缺失数据填补,组织成日侧轨间信号和夜侧轨间信号,然后分别对这两种信号进行太阳日周期变化的滤除和不同长度周期信号信噪比的计算,进而绘制这两种信号的信噪比-周期变化曲线。在日侧半轨的电子密度、离子密度和电子温度中观察到了清晰的朔望月周期变化,而在夜侧半轨的电子密度、离子密度和电子温度中却没有观察到朔望月周期变化。解释是：月球引力会引起大气的朔望月周期涨落,在日侧半轨,光电离造成电子密度、离子密度、电子温度在高度方向上产生较大的变化梯度,在同一高度太阳同步轨道上运行的DEMETER卫星自然会观测到这种涨落变化,而在夜侧,光电离停止,电子密度、离子密度、电子温度在高度方向上的变化梯度很小,DEMETER卫星自然不会观测到这种涨落变化。     

The structure of Venus' middle atmosphere and ionosphere

The atmosphere and ionosphere of Venus have been studied in the past by spacecraft with remote sensing or in situ techniques. These early missions, however, have left us with questions about, for example, the atmospheric structure in the transition region from the upper troposphere to the lower mesosphere (50-90 km) and the remarkably variable structure of the ionosphere. Observations become increasingly difficult within and below the global cloud deck (<50 km altitude), where strong absorption greatly limits the available investigative spectrum to a few infrared windows and the radio range. Here we report radio-sounding results from the first Venus Express Radio Science (VeRa) occultation season. We determine the fine structure in temperatures at upper cloud-deck altitudes, detect a distinct day-night temperature difference in the southern middle atmosphere, and track day-to-day changes in Venus' ionosphere.     

Little or no solar wind enters Venus' atmosphere at solar minimum

Venus has no significant internal magnetic field, which allows the solar wind to interact directly with its atmosphere. A field is induced in this interaction, which partially shields the atmosphere, but we have no knowledge of how effective that shield is at solar minimum. (Our current knowledge of the solar wind interaction with Venus is derived from measurements at solar maximum.) The bow shock is close to the planet, meaning that it is possible that some solar wind could be absorbed by the atmosphere and contribute to the evolution of the atmosphere. Here we report magnetic field measurements from the Venus Express spacecraft in the plasma environment surrounding Venus. The bow shock under low solar activity conditions seems to be in the position that would be expected from a complete deflection by a magnetized ionosphere. Therefore little solar wind enters the Venus ionosphere even at solar minimum.     

Discovery of an aurora on Mars

In the high-latitude regions of Earth, aurorae are the often-spectacular visual manifestation of the interaction between electrically charged particles (electrons, protons or ions) with the neutral upper atmosphere, as they precipitate along magnetic field lines. More generally, auroral emissions in planetary atmospheres "are those that result from the impact of particles other than photoelectrons" (ref. 1). Auroral activity has been found on all four giant planets possessing a magnetic field (Jupiter, Saturn, Uranus and Neptune), as well as on Venus, which has no magnetic field. On the nightside of Venus, atomic O emissions at 130.4 nm and 135.6 nm appear in bright patches of varying sizes and intensities, which are believed to be produced by electrons with energy <300 eV (ref. 7). Here we report the discovery of an aurora in the martian atmosphere, using the ultraviolet spectrometer SPICAM on board Mars Express. It corresponds to a distinct type of aurora not seen before in the Solar System: it is unlike aurorae at Earth and the giant planets, which lie at the foot of the intrinsic magnetic field lines near the magnetic poles, and unlike venusian auroras, which are diffuse, sometimes spreading over the entire disk. Instead, the martian aurora is a highly concentrated and localized emission controlled by magnetic field anomalies in the martian crust.     

全火星模型中震波传播特征的数值模拟研究

采用基于交错网格的傅里叶伪谱与有限差分混合方法, 求解弹性波动方程, 根据地球化学分析得到的两个火星理论结构模型, 模拟二维全火星模型中P-SV波和SH波的传播过程。根据理论地震图和波场快照, 讨论全火星模型中震波的传播过程以及各种震相的产生和演变, 分析模型内部火星壳厚度以及火星核幔边界深度对震波传播的影响。结果表明, 在低速火星壳内部多重反射波及转换波的相干叠加会形成很强的波列, 其特征受火星壳厚度的影响较大, 在切向分量上可以更清晰地观测到核幔边界的反射震相。     

A map of the day-night contrast of the extrasolar planet HD 189733b

'Hot Jupiter' extrasolar planets are expected to be tidally locked because they are close (<0.05 astronomical units, where 1 au is the average Sun-Earth distance) to their parent stars, resulting in permanent daysides and nightsides. By observing systems where the planet and star periodically eclipse each other, several groups have been able to estimate the temperatures of the daysides of these planets. A key question is whether the atmosphere is able to transport the energy incident upon the dayside to the nightside, which will determine the temperature at different points on the planet's surface. Here we report observations of HD 189733, the closest of these eclipsing planetary systems, over half an orbital period, from which we can construct a 'map' of the distribution of temperatures. We detected the increase in brightness as the dayside of the planet rotated into view. We estimate a minimum brightness temperature of 973 +/- 33 K and a maximum brightness temperature of 1,212 +/- 11 K at a wavelength of 8 mum, indicating that energy from the irradiated dayside is efficiently redistributed throughout the atmosphere, in contrast to a recent claim for another hot Jupiter. Our data indicate that the peak hemisphere-integrated brightness occurs 16 +/- 6 degrees before opposition, corresponding to a hotspot shifted east of the substellar point. The secondary eclipse (when the planet moves behind the star) occurs 120 +/- 24 s later than predicted, which may indicate a slightly eccentric orbit.     

Ultraviolet-radiation-induced methane emissions from meteorites and the Martian atmosphere

Almost a decade after methane was first reported in the atmosphere of Mars there is an intensive discussion about both the reliability of the observations--particularly the suggested seasonal and latitudinal variations--and the sources of methane on Mars. Given that the lifetime of methane in the Martian atmosphere is limited, a process on or below the planet's surface would need to be continuously producing methane. A biological source would provide support for the potential existence of life on Mars, whereas a chemical origin would imply that there are unexpected geological processes. Methane release from carbonaceous meteorites associated with ablation during atmospheric entry is considered negligible. Here we show that methane is produced in much larger quantities from the Murchison meteorite (a type CM2 carbonaceous chondrite) when exposed to ultraviolet radiation under conditions similar to those expected at the Martian surface. Meteorites containing several per cent of intact organic matter reach the Martian surface at high rates, and our experiments suggest that a significant fraction of the organic matter accessible to ultraviolet radiation is converted to methane. Ultraviolet-radiation-induced methane formation from meteorites could explain a substantial fraction of the most recently estimated atmospheric methane mixing ratios. Stable hydrogen isotope analysis unambiguously confirms that the methane released from Murchison is of extraterrestrial origin. The stable carbon isotope composition, in contrast, is similar to that of terrestrial microbial origin; hence, measurements of this signature in future Mars missions may not enable an unambiguous identification of biogenic methane.     

Plasma transport between the ionosphere and plasmasphere in response to solar wind dynamic pressure pulsation

The plasma transport between the plasmasphere and the ionosphere in response to the interplanetary conditions is still not fully understood until now.Simultaneous observations of the plasmasphere and ionosphere from the newly developed Chinese Meridian Project provide a new opportunity for understanding the characteristic of the plasma transport and the coupling mechanism between these two regions.We investigate the response of the plasmasphere(L≈2)and ionosphere to the solar wind dynamic pressure pulse during geomagnetically quiet period of 21–27 March 2011.The response of the plasmasphere shows a significant depletion.The plasmaspheric density nearly decreases by half in response to the solar wind dynamic pressure pulse,and subsequently recovers to the original level in 1–2 d.Meanwhile,the maximum electron density of the ionospheric F2 layer(NmF2)and the total electron content(TEC)increase by 13%and 21%,respectively,and then gradually recover,which is opposite to the behavior during magnetic storms.Preliminary analysis shows that the plasmaspheric depletion may be mainly caused by the southward interplanetary magnetic field and changing dawn-dusk electric field.The plasmaspheric density variations seem to be controlled by both the IMF and ionospheric conditions.     

地球局部曲率中心修正特征的讨论

GPS掩星探测技术可以探测中性大气获得全球大气折射率、气压、密度、温度和湿度等气象参数,该技术基本原理是基于信号多普勒观测和球对称大气的几何光学近似下Abel积分反演,获得大气廓线.在归算过程中,需要考虑地球曲率、电离层传播时间延迟、大气大尺度水平梯度、多路径传播现象等物理因素对大气反演廓线的精度影响.研究了在标准大气模式下地球局部曲率中心相对于地球中心位置变化并拟合其最佳逼近函数,研究成果可以为相关领域的研究提供参考.