近地磁尾准无碰撞磁重联事件

综合分析了ClusterⅡ－C1飞船在2001年9月15日飞越地球磁尾等离子体片区的热离子和磁场观测资料。结果表明，约在0340－0440UT时间期间，资料多次呈现出较强的尾向离子流（VXGSM＜0），明显的南向磁场分量（BZGSM＜0），以及明显的晨－昏向磁场分量BYGSM等特征。由此可以推断，在磁尾等离子体片中，在径向方向XGSE＞－18．6Re范围内，可能发生了多次磁重联事件，整个事件持续期约1h。磁重联事件的观测特征与准无（或半）碰撞磁重联理论的基本图像符合一致，因此这些事件应当是准无碰撞磁重联事件。     

Economic methods of improving efficient use of the orbit/spectrum resource by satellite systems

Satellite systems continue to play an important role in the booming market for communication and broadcasting services, driving up demand for use of the orbit/spectrum resource. Studies are required to address the problem of orbit capacity and find ways of making more efficient use of it, to avoid a situation in which there is not enough orbit/spectrum resource to cater for the development of future satellite networks. It is argued that, as far as satellite networks are concerned, the current international regulatory regime governing the use of the spectrum has significant shortcomings, which have a cost, in terms of resources and time, and make investment in satellite projects less attractive. An approach is proposed for improving efficiency of the use of the orbit/spectrum through the introduction of economic methods, to supplement the existing technical and regulatory regime. A spectrum pricing method is proposed for satellite communication systems.     

Magnetosphere response to the 2005 and 2006 extreme solar events as observed by the Cluster and Double Star spacecraft

The four identical Cluster spacecraft, launched in 2000, orbit the Earth in a tetrahedral configuration and on a highly eccentric polar orbit (4–19.6 R_E). This allows the crossing of critical layers that develop as a result of the interaction between the solar wind and the Earth’s magnetosphere. Since 2004 the Chinese Double Star TC-1 and TC-2 spacecraft, whose payload comprise also backup models of instruments developed by European scientists for Cluster, provided two additional points of measurement, on a larger scale: the Cluster and Double Star orbits are such that the spacecraft are almost in the same meridian, allowing conjugate studies. The Cluster and Double Star observations during the 2005 and 2006 extreme solar events are presented, showing uncommon plasma parameters values in the near-Earth solar wind and in the magnetosheath. These include solar wind velocities up to ∼900 km s⁻¹ during an ICME shock arrival, accompanied by a sudden increase in the density by a factor of ∼5 and followed by an enrichment in He⁺⁺ in the secondary front of the ICME. In the magnetosheath ion density values as high as 130 cm⁻³ were observed, and the plasma flow velocity there reached values even higher than the typical solar wind velocity. These resulted in unusual dayside magnetosphere compression, detection of penetrating high-energy particles in the magnetotail, and ring current development following several successive injections of energetic particles in the inner magnetosphere, which “washed out” the previously formed nose-like ion structures.     

A unified accretion–ejection paradigm for Black Hole X-ray binaries

We present a unified accretion–ejection picture that explains the different spectral state of Black Hole X-ray binaries (BHXrB) from radio to X/γ-rays. In this view, the central region of BHXrB has a multi-flow configuration which consists in (1) an outer standard accretion disc, (2) an inner magnetized accretion disc driving, (3) a self-collimated electron–proton MHD jet, surrounding and (4) a relativistic electron–positron beam when adequate conditions are met. This picture provides a simple and unified explanation to the various canonical spectral states of BH X-ray binaries, by varying the transition radius r_J between the inner disc driving jets and the outer standard disc. In this framework, large r_J correspond to Quiescent and Hard states while small r_J correspond to Thermal Dominant ones. In between these two extremes, r_J can reach values that switches on the pair cascade process giving birth to a relativistic electron–positron beam. This would correspond to the bright intermediate state.