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31.
R. Schwenn 《Space Science Reviews》2006,124(1-4):51-76
In this paper I will briefly summarize the present status of our knowledge on the four different sorts of solar wind, their
sources and their short- and long-term variations. First: the fast solar wind in high-speed streams that emerges from coronal
hole regions. Second: the slow solar wind emerging from the non-active Sun near the global heliospheric current sheet above
helmet streamers and underlying active regions. Third: the slow solar wind filling most of the heliosphere during high solar
activity, emerging above active regions in a highly turbulent state, and fourth: the plasma expelled from the Sun during coronal
mass ejections. The coronal sources of these different flows vary dramatically with the solar activity cycle. 相似文献
32.
B. Inhester G. Stenborg R. Schwenn N. Srivastava B. Podlipnik 《Space Science Reviews》1999,87(1-2):211-214
We analyze data observed by the LASCO C1 coronagraph on board the SOHO spacecraft during the solar minimum activity from April
1996 to March 1997. Using the phase dispersion technique, we investigate the periodicity and recurrence of Fe XIV emission
structures with heliospheric latitude and distance above the Sun's surface with high spatial resolution. We find no significant
deviation from a rigidly rotating Fe XIV corona with latitude or with distance from the Sun even on these small scales. In
agreement with earlier work, the coronal rotation period at solar minimum is about 27.5 ± 1 days.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献