Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1808k&link_type=abstract
American Astronomical Society, SPD meeting #42, #18.08; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The 3D structure of EUV bright points and its physical relation with the underlying magnetic flux concentrations are unveiled here observationally for the first time. The heights of EUV bright points have been measured within their lifetimes by 3D reconstruction method developed by Kwon, Chae, & Zhang (2010) using data sets taken from STEREO/SECCHI/EUVI. We found three distinct changes in the heights which were decreasing, increasing, and constant. In general, EUV bright points are multi-temperature loop system whose hot loops (T 106.2K) with an average height of 8.9Mm are overlying cooler loops (T < 106.0K) with an average height of 6.7Mm. This loop system has cool legs which have the peak temperature of T 104.9K and an average height of 5.2Mm. The heights were found to have remarkable correlations with lengths and distances of two opposite magnetic flux concentrations, indicating that the 3D structures of bright points were determined by the geometry of associated photospheric magnetic fluxes. Accordingly, the three types of bright points we found were associated with three distinct types of their underlying magnetic fragments: converging, diverging, and shearing. In all cases, both flux emergences and flux cancellations were observed during the lifetimes of the bright points. The flux emergences were dominant in the initial phase and the flux cancellations were significant after the intensities reached their maxima. Our results suggest that EUV bright points may be the flaring loop systems (Masuda et al. 1994) formed by coroanl magnetic reconnection and the flux emergence appears to be important to driving the coronal magnetic reconnection.
Davila Jose Manuel
Kwon Ryun Young
Ofman Leon
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