2004年3月13日TC-1和Cluster卫星联合观测的磁通量传输事件

分析了2004年3月13日12:15到12:25UT期间TC-1和Cluster卫星簇的磁通门磁力计(FGM)和电子/电流试验仪(PEACE)的联合观测数据.在此期间,TC-1卫星位于日下点以南的磁层顶附近的磁鞘中,并在12:19UT左右观测到了一个典型的先正后负的磁鞘磁通量传输事件(FTE);而Cluster卫星簇位于北半球日侧高纬磁层项附近,并于12:23UT左右穿出磁层顶进入磁鞘,且在12:21 UT左右也观测到了一个典型的先正后负的磁层FTE.比较分析发现此两个FTE具有类似的磁场结构和等离子体特征,可能是同一个北向运动的FTE先后被TC-1和Cluster卫星观测到.利用Cluster 4颗卫星的多点同时观测数据,采用最小方向微分法和时空微分方法,推断Cluster卫星观测的这个FTE是尺度大小约为1.21Re的准二维结构,其运动方向为东北方向,与Cooling模型预测方向基本一致.利用Cooling模型的预测,推算了TC-1卫星在12:19UT观测的FTE的运动速度和尺度,进而得出随着通量管的极向运动,其速度和尺度均有所增加.     

D-region IRI profiles in relation to radio observations

The D-region IRI profiles are compared with the direct rocket measurements as well as with ground-based radio observations by a variety of techniques. The characteristics of D-region IRI profiles and the dependence of electron density on solar zenith angle, sunspot number, latitude and season are discussed. The sensitivity of certain reflection coefficients on the height distribution of electron density below 70 km is illustrated with a typical example. For D-region modelling, the results show the importance of simultaneous measurement of reflection and conversion coefficients together with polarization phase over a wide frequency range.     

三基色测量法在S-GAP推进剂火焰温度分布中的应用(英文)

介绍了一种测量推进剂火焰温度的新方法,即三基色测量法(PCM)。采用三基色测量法测试了S-GAP推进剂(以HMX为氧化剂)的燃烧火焰温度。结果表明,随着的压强增加,S-GAP火焰区更接近燃烧表面;随着推进剂中HMX的增加,暗区变薄。S-GAP推进剂的火焰温度分布呈等温线形式,1 MPa下火焰温度范围为970～1 600℃,当压强增大为3MPa时,火焰温度范围为1 200～2 200℃。PCM法与热电偶方法测量的最高燃烧火焰温度值较为接近。     

Electron density reference profile in the lower ionosphere

The new IRI formula, as accepted at the 1983 Stara Zagora Workshop, prescribes the use of Epstein functions for reproducing logarithmic electron density profiles. In this paper we discuss solutions which might be applicable to the lower ionosphere. The experimental data base is briefly reviewed. It appears that the stratification near 80 km must be accepted as a regular feature of the daytime lower ionosphere. The C-layer problem is left open. In order to reproduce such profiles, one needs three LAY-functions. Examples show that the weighted sum of these does very well represent experimental profiles, the amplitudes being determined by a least square fit. For profile synthesis (as in IRI) a least square determination of the three amplitudes, admitting four linear conditions, is proposed.     

Highlights of the 1975 URSI/COSPAR workshop on the IRI

Some of the presentations made at the IRI Workshop held at Louvain in 1985 have not appeared in the Proceedings. Some discussions which took place during the workshop could be of interest in future work. This article tries to highlight the IRI modelling aspects in the four principal height regions of the ionosphere.