1987年9月23日在3.2cm波长上的日环食射电观测

本文介绍了1987年9月23日在3.2厘米波长上的日环食射电观测的资料处理、射电源的证认和结果分析,取得以下结果:(1)太阳射电半径为1.09±0.2;(2)日面亮度温度分布,在光学边缘13.4—15.9范围内有一明显的临边增亮,增亮的幅度为13.5±5％;(3)宁静太阳流量为264.8sfu;(4)射电源的角径、流量、平均亮温度和高度等.     

Radio emissions from the outer heliosphere

For nearly fifteen years the Voyager 1 and 2 spacecraft have been detecting an unusual radio emission in the outer heliosphere in the frequency range from about 2 to 3 kHz, Two major events have been observed, the first in 1983–84 and the second in 1992–93. In both cases the onset of the radio emission occurred about 400 days after a period of intense solar activity, the first in mid-July 1982, and the second in May–June 1991. These two periods of solar activity produced the two deepest cosmic ray Forbush decreases ever observed. Forbush decreases are indicative of a system of strong shocks and associated disturbances propagating outward through the heliosphere. The radio emission is believed to have been produced when this system of shocks and disturbances interacted with one of the outer boundaries of the heliosphere, most likely in the vicinity of the the heliopause. The emission is believed to be generated by the shock-driven Langmuir-wave mode conversion mechanism, which produces radiation at the plasma frequency (f _p ) and at twice the plasma frequency (2f _p ). From the 400-day travel time and the known speed of the shocks, the distance to the interaction region can be computed, and is estimated to be in the range from about 110 to 160 AU.Abbreviations PWS Plasma Wave Subsystem - AU Astronomical Unit - DSN Deep Space Network - NASA National Aeronautics and Space Administration - GMIR Global Merged Interaction Region - MHD Magnetohydrodynamic - CME coronal mass ejection - f _p plasma frequency - R radial distance - AGC automatic gain control     

Comparison of the CHAMP radio occultation data with the Canadian advanced digital ionosonde in the Polar Regions

In this paper we present the results of the comparison of the retrieved electron density profiles of the Ionospheric Radio Occultation (IRO) experiment on board CHAMP (CHAllenging Minisatellite Payload), with the ground ionosonde profiles for the Polar Regions. IRO retrieved electron density profiles from CHAMP are compared with Canadian Advanced Digital Ionosonde (CADI) measurements at two vertical sounding stations well within the Polar Cap, Eureka (geog. 80°13′ N; 86°11′ W) and Resolute Bay (geog. 74°41′ N; 94°54′ W). We compared the ionospheric parameters such as the peak electron density of the F-layer (NmF₂) and the peak height of the F-layer (h_mF₂) for a 3-year period, 2004–2006. CHAMP derived NmF₂ shows reasonable agreement with the ionosonde retrieved NmF₂ for both the stations (0.76 and 0.71 correlation coefficient, for Eureka and Resolute Bay, respectively) whereas the h_mF₂ agreement is not that acceptable (0.25 and 0.37 correlation coefficient, respectively). The h_mF₂ from vertical sounding showed less spread than the CHAMP h_mF₂.     

Comparison between ionospheric peak parameters retrieved from COSMIC measurement and ionosonde observation over Sanya

In this paper we compared the ionospheric peak parameters (peak electron density of the F region, NmF2, and peak height of the F region, hmF2) retrieved from the FORMASAT-3/COSMIC (COSMIC for short) satellite measurement with those from ionosonde observation at Sanya (18.3°N, 109.6°E) during the period of 2008–2013. Although COSMIC NmF2 (hmF2) tends to be lower (higher) than ionosonde NmF2 (hmF2), the results show that the ionospheric peak parameters retrieved from COSMIC measurement generally agree well with ionosonde observation. For NmF2 the correlation between the COSMIC measurement and the ionosonde observation is higher than 0.89, and for hmF2 the correlation is higher than 0.80. The correlation of the ionospheric peak parameters decreases when solar activity increases. The performance of COSMIC measurement is acceptable under geomagnetic disturbed condition. The correlation of NmF2 between COSMIC and ionosonde measurements is higher (lower) during the nighttime (daytime), while the correlation of hmF2 is lower (higher) during the nighttime (daytime).     

电波折射误差实时修正的公式拟合方法

在实际工程应用中,为了提高雷达测量精度,电波折射误差的修正主要采用实时修正方法。本文给出了电波折射误差实时修正的公式拟合方法,该方法在实际应用中能够快速得到折射误差,从而提高了雷达测量精度。     

多GNSS掩星大气探测卫星星座设计

为减少无线电掩星(RO)大气探测星座的卫星数量并增加探测数据量,将北斗（BD）和GPS、Galileo、GLONASS共同作为探测信源,提出一种多全球导航卫星系统（GNSS）掩星大气探测星座概念和优化设计方法。融合先验大气模型和二维射线追踪算法,建立兼容多GNSS信源的掩星事件前向模拟算法,实现掩星事件快速精确仿真;给出多GNSS掩星大气探测星座参数对探测性能的影响特性,降低了星座模型的复杂度;并利用改进的蚁群算法实现星座参数寻优。设计结果与COSMICII星座相比,卫星数量减少2颗,探测数据量增加了40%,探测均匀性提高了67%。     

基于空间信息的射频隐身数据链最优能量控制算法

为提高数据链的低被截获性能,提出了一种基于空间信息的射频隐身数据链最优能量控制算法。以数据链目标飞行区域的威胁因子为先验知识,基于数据链的实时空间信息,分析了影响数据链性能的各个参数,将辐射功率、开机时刻作为优化变量,以最小化辐射功率函数和最小化能量消耗函数作为目标,利用混合混沌粒子群优化算法对数据链通信模型进行优化,选取使两个目标函数最小的解作为最优解。仿真结果表明,算法与目前常见的数据链恒定功率辐射方法相比,在满足可靠通信的前提下,辐射功率较小,消耗能量较少,具有较好的射频隐身性能。     

Assessment of the occurrence of radio frequency interference with AMSR-E observations over India

The AMSR-E observed brightness temperatures over India have been analyzed to study the impact of manmade radio frequency interference (RFI) sources for the two dry months April and May from 2003 to 2010. It is observed that the brightness temperature values far exceed 300 K over different locations of India indicating the presence of RFI. It is pronounced over the urban areas. The regions over Punjab, Haryana and Delhi show a marked increase in spread of the RFI affected areas. The RFI affected areas have increased from 15% to 30% from 2003 to 2007 and decreased thereafter. A maximum brightness temperature of 353 K is observed in April 2007 indicating very high level of RFI.     

Solar and interplanetary parameters of CMEs with and without type II radio bursts

We have analyzed 101 CMEs, and their associated ICMEs and interplanetary (IP) shocks observed during the period 1997–2005. The main aim of the present work is to study the interplanetary characteristics of metric and DH type II associated CMEs such as, shock strength, IP shock speed, ICME speed, stand off distance and transit time. Among these 101 CMEs, 38 events show both metric and DH type II bursts characteristics. There are no metric and DH type II association for 52 events. While DH type II alone is found in 7 cases, metric type II alone is found in 4 events. It is found that the mean speeds of CMEs increase progressively from CMEs without type II events to CMEs associated with metric and DH type IIs as suggested by Gopalswamy et al. (2005). In addition, we found that the speeds of ICMEs and IP shocks progressively increase in the following order: events without metric and DH type IIs, events with metric alone, events with DH alone and events with both metric and DH type IIs. Similarly the Mach number is found to increase in the same order. While there is not much change in the stand-off distance among these cases, it is minimum (∼18 R_⊙) for CMEs with speed greater than 2200 km/s. The above results confirm that more energetic CMEs can produce both metric and DH type IIs for which the interplanetary parameters such as mean values of ICME speed and IP shock speed and Mach number are found to be higher.     

Towards validation of SCIAMACHY lunar occultation NO2 vertical profiles

Vertical profiles of stratospheric nitrogen dioxide (NO₂) have been retrieved from moderate resolution lunar occultation transmission spectra measured by Scanning Imaging Absorption spectroMeter for Atmospheric CHartographY (SCIAMACHY) on board the European Environmental Satellite (ENVISAT). These measurements were taken over the high southern latitude of 50°–90° during the period of 2003–2005. To assess the accuracy of the retrieved NO₂ profiles, the SCIAMACHY nighttime NO₂ profiles were compared with NO₂ profiles retrieved from sunrise solar occultation spectra measured by the Halogen Occultation Experiment (HALOE) and the Stratospheric Aerosol and Gas Experiments II (SAGE II) using a photochemical correction model. The validation results show good agreement of SCIAMACHY lunar occultation NO₂ with scaled HALOE and SAGE II profiles. The relative mean differences (rmd) with scaled HALOE profiles are within −13% to +5% and standard deviations (rms) of the relative differences are within 3–19% between 25 and 38 km. The rmd and rms with scaled SAGE II NO₂ profiles are in the range of −9 to +7 and 10–17% respectively between 22 and 39 km.