排序方式: 共有22条查询结果,搜索用时 15 毫秒
21.
J. T. Gosling 《Space Science Reviews》2012,172(1-4):187-200
It is only within the last 5 years that we have learned how to recognize the unambiguous signature of magnetic reconnection in the solar wind in the form of roughly Alfvénic accelerated plasma flows embedded within bifurcated magnetic field reversal regions (current sheets). This paper provides a brief overview of what has since been learned about reconnection in the solar wind from both single and multi-spacecraft observations of these so-called reconnection exhausts. 相似文献
22.
By the time of the 34th ESLAB symposium, dedicated to the memory of John Simpson, Ulysses had nearly reached its peak southerly latitude in its second polar orbit. The global solar wind structure observed thus far
in Ulysses' second orbit is remarkably different from that observed over its first orbit. In particular, Ulysses observed highly irregular solar wind with less periodic stream interaction regions, much more frequent coronal mass ejections,
and only a single, short interval of fast solar wind. Ulysses also observed the slowest solar wind seen thus far in its ten-year
journey (∼270 km s−1). The complicated solar wind structure undoubtedly arises from the more complex coronal structure found around solar activity
maximum, when the large polar coronal holes have disappeared and coronal streamers, small-scale coronal holes, and frequent
CMEs are found at all heliolatitudes.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献