Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640507m&link_type=abstract
American Astronomical Society, AAS Meeting #216, #405.07; Bulletin of the American Astronomical Society, Vol. 41, p.890
Other
Scientific paper
When one active region emerges close to an older active region, coronal loops connecting the two regions are often observed in extreme ultraviolet (EUV). This signifies the occurrence of magnetic reconnection, an important mechanism in other contexts, such as solar flares and coronal mass ejections. We measure the rate of the magnetic reconnection by identifying each coronal loop observed in EUV that connects the existing and the emerging active regions. For each loop we estimate amount of magnetic flux it carries by measuring its apparent width in EUV and the magnetic field strength in the same location using (non)-linear force-free field reconstruction (Malanushenko et. al., 2009). We find that the amount of reconnected flux apparent on EUV is smaller than the flux through the separator surface in the point charge magnetic model (Longcope, 2005). This discrepancy provides a means to estimate the fraction of reconnecting loops that would appear in the EUV bandpass. We measure the delay time between the noticeable beginning of the emergence and the reconnection apparent in EUV. We apply this analysis to five emergence events. This work expands and improves the method described by Longcope et. al. (2005).
Longcope Dana Warfield
Malanushenko Anna
McKenzie David E.
Yusuf M. H.
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