Physics
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991acasn..32..233z&link_type=abstract
Acta Astronomica Sinica (ISSN 0001-5245), vol. 32, no. 3, Sept. 1991, p. 233-238. In Chinese.
Physics
3
Coronal Loops, Electron Flux Density, Plasma Interactions, Solar Magnetic Field, H Alpha Line, Magnetic Field Reconnection, Solar Physics
Scientific paper
In this paper the occasional transient enhancement at the interaction regions of some loops as recorded in coronal images of FeXIV (5303A) and FeX (6374A), and the associated images in H alpha have been analyzed. The brightness of a green line enhancement gradually increases to a maximum and then fades with a typical lifetime of about 20-30 minutes. The maximum of the red line enhancement at the same location follows that of the green line on average by 8.6 minutes, and H alpha then reaches a maximum in extent on average 9.3 minutes after the red line maximum. This phenomenon is interpreted as a process of localized magnetic reconnection. Estimates of the electron density are derived from the cooling time, and the values of dissipated energy are obtained by two separate methods.
Smartt Raymond N.
Zhang Zhen-Da
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