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| 1 | Kinetic features of bursty bulk flows and dipolarization fronts显示文摘Bursty bulk flows(BBFs)and dipolarization fronts(DFs)are two important phenomena responsible for the transport of energy,mass and magnetic flux from the Earth's magnetotail to the inner magnetosphere during magnetosphere substorms.The BBFs are defined as the high-speed flows of several hundred km/s in the central plasma sheet lasting about 10 minutes,while DFs are defined as,with much shorter time scale of several seconds,sharp increases in the northward magnetic field component in the plasma sheet.These two | LIU WenLong | 2016 | Science China(Information Sciences)2016，59，12： | 1 |
| 2 | Global frequency distributions of pulsations driven by sharp decrease of solar wind dynamic pressure显示文摘On 24 August 2005, an impulse of solar wind dynamic pressure(Psw) hit the magnetosphere. Using the high resolution geomagnetic field data from 15 ground stations and the data from Geotail and TC-1, we studied the geomagnetic pulsations at auroral latitudes driven by the sharp decrease of Psw at the trailing edge of the impulse. The results show that the sharp decrease of Psw can excite a global pulsation in the frequency range 4.3–11.6 m Hz. The pulsation has a reversal of polarization between two auroral latitude stations, a larger power spectral density(PSD) close to resonant latitude and increasing frequency with decreasing latitude. All these features indicate that the pulsations are associated with field line resonance(FLR). The fundamental resonant frequency(the peak frequency of PSD between 4.3 and 5.8 m Hz) is dependent on magnetic local time and is largest around magnetic local noon. This feature is due to the fact that the size of magnetospheric cavity is dependent on local time and smallest at noon. A second harmonic wave at about 10 m Hz is also observed, which is strongest in the daytime sector, and becomes heavily attenuated in the night sector. The comparison of the PSDs of the pulsations driven by sharp increase and sharp decrease of Psw shows that the frequency of pulsations is negatively proportional to the size of magnetopause. Since the FLR is excited by compressional cavity/waveguide waves, the above results indicate that the resonant frequency in the magnetospheric cavity/waveguide is controlled not only by solar wind parameters but also by magnetic local time of observation point. | WANG ZhiQiang | 2015 | Science China Earth Sciences2015，58，12： | 1 |
| 3 | Magnetospheric Physics in China:2014-2015显示文摘In the past two years,much progress is made in magnetospheric physics by using the data of Double Star Program,Cluster,THEMIS,RBSP,Swarm missions etc.,or by computer simulations.This paper briefly reviews these works based on papers selected from the 191 publications from January 2014 to December 2015.The subjects cover various sub-branches of magnetospheric physics,including geomagnetic storm,magnetospheric substorm,magnetic reconnection,solar windmagnetosphere-ionosphere interaction,radiation belt,outer magnetosphere,magnetotail,plasmasphere,geomagnetic field,auroras and currents. | CAO Jinbin YANG Junying | 2016 | 空间科学学报2016，36，5： | 0 |
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