Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh13b1557m&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH13B-1557
Physics
2100 Interplanetary Physics, 6025 Interactions With Solar Wind Plasma And Fields, 7594 Instruments And Techniques
Scientific paper
The solar wind observations by STEREO A and B, together with the ACE spacecraft provide an unprecedented opportunity to examine three-dimensional structures of interplanetary magnetic clouds (MCs). The purpose of this study is to get a better insight into their spatial extent, differences in their detailed structures depending on the geometry of spacecraft encounter, and possible deformation due to interactions with other solar wind structures. For this purpose, we surveyed the STEREO and ACE data for the period from January 2007 through February 2008. As a result, we found that each of the three spacecraft encountered four or five well-defined MC during this period, in which the separation of STEREO A (B) from the Earth changed from 0 to 22 (-24) degrees. The observations from 21 to 23 May, 2007 provide a data set that is the most appropriate to our purpose. ACE detected two MCs (No. 1, May 21/2300 - May 22/1300; No.2, May 23/0300 - May 23/1200), and a less evident MC-like structure in between. Interestingly, the MC No. 1 was observed by STEREO B in a more beautiful form, with only a "remnant-like" structure observed by STEREO A, whereas the MC No.2 was observed by STEREO A in a more beautiful form than observed by ACE. It is supposed that these two MCs observed by ACE provide some evidence for deformation due to MC- MC interactions, although the analysis is not completed yet. On another topic, we need to admit that the probability for the same MCs to be observed by two spacecrafts is low despite the small separation between them. This observational fact can be explained by the direction of MC axis obtained from model fittings. This implies that we can obtain observational information about the spatial extent of MC only for those MCs with axes nearly parallel to the ecliptic plane.
Bong Suchan
Cho Kihyeon
Marubashi Katsuhide
Sung Sangkyung
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