## 2011年  第31卷  第2期

2011, 31(2): 125-149. doi: 10.11728/cjss2011.02.125

Both theory and simulation have played important roles in defining and illuminating the key mechanisms involved in substorms. Basic theories of magnetic reconnection and of interchange and ballooning instabilities were developed more than 50 years ago, and these plasma physical concepts have been central in discussions of substorm physics. A vast amount of research on reconnection, including both theoretical and computational studies, has helped provide a picture of how reconnection operates in the collisionless environment of the magnetosphere. Still, however, we do not fully understand how key microscale processes and large-scale dynamics work together to determine the location and rate of reconnection. While in the last twenty years, it has become clear that interchange processes are important for transporting plasma through the plasma sheet in the form of bursty bulk flows and substorm expansions, we still have not reached the point where simulations are able to realistically and defensibly represent all of the important aspects of the phenomenon. More than two decades ago it was suggested that the ballooning instability, the basic theory for which dates from the 1950s, may play an important role in substorms. Now the majority of experts agree that regions of the plasma sheet are often linearly unstable to ideal-MHD ballooning. However, it is also clear that kinetic effects introduce important modifications to the MHD stability criterion. It is still uncertain whether ballooning plays a leading role in substorms or has just a minor part. Among the different types of simulations that have been applied to the substorm problem, global MHD codes are unique in that, in a sense, they represent the entire global substorm phenomenon, including coupling to the solar wind and ionosphere, and the important mechanisms of reconnection, interchange, and ballooning. However, they have not yet progressed to the point where they can accurately represent the whole phenomenon, because grid-resolution problems limit the accuracy with which they can solve the equations of ideal MHD and the coupling to the ionosphere, and they cannot accurately represent small-scale processes that violate ideal MHD.
2011, 31(2): 150-153. doi: 10.11728/cjss2011.02.150

The magnetic field disturbances detected by the Phobos-2 spacecraft in 1989 have been suggested to be caused by a ring of dust and/or gas emitted from the Martian moon, Phobos. The physical nature of these Phobos events'' is examined using results from related investigations over the last twenty years. It is concluded that there is no clear evidence at present to support the association of magnetic field disturbances in the solar wind with Phobos. The situation will be further clarified taking advantage of the multi-spacecraft observations of the Yinghuo-1(YH-1), Mars Express and MAVEN missions beginning in 2012. It is expected that many novel features of solar wind interaction with Phobos (and possibly also Deimos) itself will also be revealed.

2011, 31(2): 154-164. doi: 10.11728/cjss2011.02.154

2011, 31(2): 165-169. doi: 10.11728/cjss2011.02.165

2011, 31(2): 170-175. doi: 10.11728/cjss2011.02.170

2011, 31(2): 176-181. doi: 10.11728/cjss2011.02.176

2011, 31(2): 182-186. doi: 10.11728/cjss2011.02.182

2011, 31(2): 187-193. doi: 10.11728/cjss2011.02.187

2011, 31(2): 194-200. doi: 10.11728/cjss2011.02.194

2011, 31(2): 201-207. doi: 10.11728/cjss2011.02.201

2011, 31(2): 208-213. doi: 10.11728/cjss2011.02.208

2011, 31(2): 214-222. doi: 10.11728/cjss2011.02.214

The configuration boundedness of the three-body model dynamics is studied for Sun-Earth formation flying missions. The three-body formation flying model is built up with considering the lunar gravitational acceleration and solar radiation pressure. Because traditional linearized dynamics based method has relatively lower accuracy, a modified nonlinear formation configuration analysis method is proposed in this paper. Comparative studies are carried out from three aspects, i.e., natural formation configuration with arbitrary departure time, initialization time and formation configuration boundedness, and specific initialization time for bounded formation configuration. Simulations demonstrate the differences between the two schemes, and indicate that the nonlinear dynamic method reduces the error caused by the model linearization and disturbance approximation, and thus provides higher accuracy for boundedness analysis, which is of value to initial parameters selection for natural three-body formation flying.

2011, 31(2): 223-228. doi: 10.11728/cjss2011.02.223

2011, 31(2): 229-235. doi: 10.11728/cjss2011.02.229

2011, 31(2): 236-245. doi: 10.11728/cjss2011.02.236

2011, 31(2): 246-253. doi: 10.11728/cjss2011.02.246

2011, 31(2): 254-259. doi: 10.11728/cjss2011.02.254

2011, 31(2): 260-268. doi: 10.11728/cjss2011.02.260