DORIS processing at the European Space Operations Centre

This paper gives an overview of the DORIS related activities at the Navigation Support Office of the European Space Operations Centre. The DORIS activities were started in 2002 because of the launch of the Envisat satellite where ESOC is responsible for the validation of the Envisat Precise Orbits and a brief overview of the key Envisat activities at ESOC is given. Typical orbit comparison RMS values between the CNES POE (GDR-C) and the ESOC POD solution is 6.5, 18.8 and 23.1 mm in radial-, along- and cross-track direction. In the framework of the generation of the ITRF2008 ESOC participated in the reprocessing of all three space geodetic techniques; DORIS, SLR, and GPS. Here the main results of our DORIS reprocessing, in the framework of the International DORIS Service (IDS), are given. The WRMS of the weekly ESOC solution (esawd03) for the 2004–2009 period compared to the IDS-1 combined solution is of the order of 12 mm. Based on the long time series of homogeneously processed data a closer look is taken at the estimated solar radiation pressure parameters of the different satellites used in this DORIS analysis. The main aim being the stabilization of the Z-component of the geocentre estimates. We conclude that the ESOC participation to the IDS ITRF2008 contribution has been beneficial for both ESOC and the IDS. ESOC has profited significantly from the very open and direct communications and comparisons that took place within the IDS during the reprocessing campaign.     

传输激光能量的光纤滑环结构设计与试验研究

本文设计了一种光纤滑环结构,可实现将激光能量从固定平台传输到旋转平台。该光纤滑环结构可精确控制对接光纤的端面间隙,有效保护传能光纤。实验表明,光纤耦合效率可达90%左右,可满足科研及工业应用需求。     

片光反射遮挡式超高速亚毫米粒子探测技术

为满足在超高速碰撞靶上开展航天器抗空间碎片防护性能试验，需要准确测量速度3～10km／s，以及更高速度的毫米级或亚毫米级粒子的飞行速度，在可以实现毫米级粒子探测的片光遮挡式粒子探测技术基础上发展了片光反射遮挡式粒子探测技术，通过采用提高粒子直径与激光光束宽度的比值，解决了探测粒子直径小于1mm时探测信号弱不能识别等关键技术，研制了试验装置并开展了验证试验，研究结果表明该技术在0．2～10km／s速度范围内可实现直径为0．1mm量级粒子的有效探测。     

小型电磁辐射敏感度自动测试系统的设计

介绍电磁辐射敏感度自动测试系统组成、工作原理和设计方法，叙述了硬件配置、系统控制、数据采集处理等软件设计。其中较详细地介绍了光纤式场强数据采集部分的设计。     

光学基片表面软质抛光胶体粒子的激光清洗

介绍了光学基片表面软质抛光胶体粒子激光清洗的基本方法、原理和实验装置,并通过对含有污染微粒的基片表面进行激光清洗,获得了高洁净表面的光学基片.     

激光加工气膜孔对定向凝固高温合金薄壁持久性能的影响

采用定向凝固无余量精铸工艺制造的接近于空心涡轮叶片形状和壁厚的管状薄壁（δ＝１．２ｍｍ）试样，研究了激光加工孔对定向凝固高温合金薄壁持久性能的影响。结果表明，在９００℃／３７０ＭＰａ下，与没有孔的薄壁试样相比，有一排孔的试样持久性能没有明显降低，有两排孔的试样持久寿命略有下降。显微分析表明，激光加工孔对组织没有明显的影响，只是稍微减小了承载面积，而且只有在出现两排激光孔时才有所表现。     

空间激光通信系统光斑小目标跟踪算法研究

在空间激光通信链路中，大气湍流、结构设计误差、平台扰动等因素为链路的精确对准和精密跟踪带来了困难。为提高激光链路的跟踪精度，首先对光斑跟踪过程中的影响因素进行研究分析，继而对跟踪算法做出改进。针对跟踪目标特性，设计了一种自适应模板目标相关跟踪算法，并搭建了基于粗精复合轴跟踪系统的实验平台，开展了实验验证。结果表明：与当前常用跟踪算法相比，该设计处理速度可达 1 kfps，目标跟踪位置与真实位置基本重合，目标跟踪准确率高于98%，在处理速度、跟踪准确率与算法鲁棒性上均有较大提升，具有一定的实用性。     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

Spectroscopic Constraints on Models of Ion-cyclotron Resonance Heating in the Polar Solar Corona

Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is rapid, even for minor ions like O⁵⁺, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona. This revised version was published online in June 2006 with corrections to the Cover Date.     

The relationship between plasma effects and cosmic radiation studied with TriTel-LMP measurements during the ESEO mission

The main point of the paper is to use the simultaneous measurements of the energetic particle flux by TriTel and those of electron density by a Langmuir probe to study the question of to what extent solar electromagnetic and corpuscular radiation (galactic cosmic rays, particle precipitation from the radiation belts) are responsible for the ionization of the atmosphere. The electron density measured by the Langmuir probe is the sum of the ionization produced by the solar electromagnetic radiation and that due to the corpuscular radiation. The ionization produced by the solar electromagnetic radiation may be computed. The flux of energetic particles in an energy range may be determined by taking the difference between the threshold energy of the TriTel telescopes and the energy corresponding to the local cut-off rigidity. As the ESEO satellite will have a quasi-polar and circular orbit, the cut-off rigidity will change from low to high latitudes, thus enabling the assignment of different energy bands for the telescopes. Thus, it will be possible to determine which energy bands of particle produce ionization at different latitudes.