| Autor: |
Xuan, J. Y., Gu, X. M., Lin, J., Jiang, Y. C., Zhong, S. H., Li, Y. S., Xuan, J. Y., Gu, X. M., Lin, J., Jiang, Y. C., Zhong, S. H., Li, Y. S. |
| Zdroj: |
Astronomy and Astrophysics. Supplement Series; May 1998, Vol. 129 Issue: 3 p553-561, 9p |
| Abstrakt: |
Some properties of the white light flare (WLF) that occurred on 18 January 1989 are presented. The flare consisted of 7 patched-shape kernels, with sizes $(1.5 \sim 4) \ 10^{17}$cm2. The lifetimes of the kernels were from several minutes to more than 40 minutes. The initial bright points of the WLF kernels originated between the umbra and penumbra, in penumbra fibrils, between penumbra fibrils and the photosphere, or on the photosphere and light bridge. These kernels appeared 2 to 3 minutes after Hαflares, and reached their maxima respectively before the first maximum and 1 to 2 minutes before the second maximum of the Hαflare, and disappeared slowly before the disappearance of the Hαflare. The direction and size of material motion in the kernels are different. The precursors of the WLF are similar to those of ordinary flares. The magnetic pattern of the photosphere in the active region is in δ- structure, and the kernels lie at or near the changing magnetic neutral lines. The small longitudinal field gradient may be constrained by the small transverse field on the photosphere. The flare exhibited both temporal and spatial properties in the center reversal and line-width of Hαprofiles, and has characteristics of both class I and II. Thus it may be a mixed-class white light flare. |
| Databáze: |
Supplemental Index |
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