Dynamics and turbulence of the chromospheric layers of a flaring
atmosphere
K. Brcekova(1),
A. Kucera(1),
A. Hanslmeier(2),
J. Rybak(1),
H. Wohl(3)
1 - Astronomical Institute, Slovak Academy of Sciences, SK-05960 Tatranská Lomnica, Slovakia
2 - Institut for Geophysics, Astrophysics and Meteorology, Universitätsplatz 5, A-8010 Graz, Austria
3 - Kiepenheuer-Institut fur Sonnenphysik, Schoneckstr. 6, 79104 Freiburg,
Germany
We investigated the time series of spectra of a subflare observed with high
spatial and spectral resolution in chromospheric Ca II K line 393.3 nm
(h~1500 km) and two
photospheric lines Fe I 522.5\,nm and Fe I 557.6 nm (h~370~km for
both).
The photospheric lines differ in magnetic sensitivity, g_eff=2.25
and g_eff=0 are valid for Fe I 522.5 nm and Fe I 557.6 nm,
respectively. The spectra were taken with the Vacuum Tower
Telescope on June 1st, 1993, simultaneously in all three spectral
regions.
During the time interval from 08:12:30 UT to
08:14:46 UT 12 sets of spectra were obtained. After applying
the reduction steps we determined the FWHM for both Fe I lines
and the asymmetry for Ca II K line (definition in Brcekova et
al. 2002). We plotted the trend of spectral characteristics along the slit
and compared the spectral characteristics from the photosphere and
chromosphere to investigate the influence of the flare on the underlying
layers of atmosphere.
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