Authors: You J.¹; Hiei E.²; Li H.¹

Source: Solar Physics, Volume 217, Number 2, November 2003 , pp. 235-245(11)

Publisher: Springer

Abstract:

After carefully comparing the white-light (5600±00 Å) and the slit-jaw H images (0.5 Å  passband) of the 2N/X20 white-light flare of 16 August 1989, we found that the H counterpart identification of the bright kernels in continuum by Hiei, Nakagomi, and Takuma (1992) was incorrect. Now we come to the conclusion that none of the two white-light kernels has a corresponding bright H area. Moreover, the loop shapes in white-light are also different from those in H. H loops rose more rapidly than white-light loops. However, their height–time variations on the whole are similar. This indicates that the continuum and chromospheric emissions of the flare presumably come from different plasmas, but may be modulated by some mutual factors, such as large-scale magnetic fields. Analysis of the He i 10 830 Å spectra taken simultaneously with the slit-jaw H images shows that the line-center intensity of He i 10 830 Å doesn't have a good correlation with the intensity of nearby continuum, which supports the above conclusions. In addition, the electron density at the white-light loop top estimated from the continuum around 5600 Å  and 10 830 Å  is as high as 10¹²–10¹³ cm^-3.

Document Type: Research article

Affiliations: 1: Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China 2: National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan

Publication date: 2003-11-01

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