Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989sxsr.rept.....k&link_type=abstract
In American Science and Engineering, Inc., Solar X-Ray Astronomy Sounding Rocket Program 12 p (SEE N90-10796 01-88)
Astronomy and Astrophysics
Astronomy
Coronal Holes, Magnetic Field Reconnection, Solar Magnetic Field, X Ray Astronomy, Image Analysis, Magnetic Flux, Solar Physics, Temporal Resolution, X Ray Sources
Scientific paper
Coronal holes are large scale regions of magnetically open fields which are easily observed in solar soft X-ray images. The boundaries of coronal holes are separatrices between large scale regions of open and closed magnetic fields where one might expect to observe evidence of solar magnetic reconnection. Previous studies by Nolte and colleagues using Skylab X-ray images established that large scale (greater than or equal to 9 x 10(4) km) changes in coronal hole boundaries were due to coronal processes, i.e., magnetic reconnection, rather than to photospheric motions. Those studies were limited to time scales of about one day, and no conclusion could be drawn about the size and time scales of the reconnection process at hole boundaries. Sequences of appropriate Skylab X-ray images were used with a time resolution of about 90 min during times of the central meridian passages of the coronal hole labelled Coronal Hole 1 to search for hole boundary changes which can yield the spatial and temporal scales of coronal magnetic reconnection. It was found that 29 of 32 observed boundary changes could be associated with bright points. The appearance of the bright point may be the signature of reconnection between small scale and large scale magnetic fields. The observed boundary changes contributed to the quasi-rigid rotation of Coronal Hole 1.
Kahler Stephen W.
Moses John Daniel
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