Other
Scientific paper
Mar 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jkas...35...59c&link_type=abstract
Journal of the Korean Astronomical Society, vol. 35, no. 1, pp. 59-65
Other
10
Scientific paper
Solar observations support that magnetic reconnection ubiquitously occurs in the chromosphere as well as in the corona. It is now widely accepted that coronal magnetic reconnection is fast reconnection of the Petschek type, and is the main driver of solar flares. On the other hand, it has been thought that the traditional Sweet-Parker model may describe chromospheric reconnection without difficulty, since the electric conductivity in the chromoshphere is much lower than that in the corona. However, recent observations of cancelling magnetic features have suggested that chromospheric reconnection might proceed at a faster rate than the Sweet-Parker model predicts. We have applied the Sweet-Parker model and Petschek model to a well-observed cancelling magnetic feature. As a result, we found that the inflow speed of the Sweet-Parker reconnection is too small to explain the observed converging speed of the feature. On the other hand, the inflow speeds and outflow speeds of the Petschek reconnection are well compatible with observations. Moreover, we found that the Sweet-Parker type current sheet is subject to the ion-acoustic instability in the chromosphere, implying the Petschek mechanism may operate there. Our results strongly suggest that chromospheric reconnection is of the Petschek type.
Chae Jongchul
Choi Byung-Kyu
Park J. M. M.
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