Statistics – Methodology
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..27z&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Statistics
Methodology
Scientific paper
The He I 10830 Å triplet line gives an unique view of the chromosphere active regions. Several articles at early time had indicated the enhancement of the absorption at this line in sunspot umbra among other features. The line depths of the HeI 10830 triplet line are compare with plages and other AR features reliable registered in sunspot umbrae. It is good opportunity for examination of the chromosphere heating processes concerning with a quite difference magnetic structures. Up to date, systematically investigation of helium spectrum in sunspot umbrae had not conducted. This issue has provided the statistical results of the HeI 10830 triplet line observations in sunspot umbrae. The observations were made at the Large Nicolsky Coronagraph at Sayan mountain observatory. The setup for the multi-spectral observation was used. This setup consists of the CCD spectrograph and the two bandwidth (He/Hα) birefringent filter. The lens system of the coronagraph provides the possibility for synchronous registration of the spectral line and two monochromatic images in quite different spectral regions. Methodology to avoid of blurring effects on line profiles based on the point spread function (PSF) has been developed. PSF have been derived from pore continuum contrast profile registered immediately at the same time and place and set of empirical data. The PSF was used to restore monochromatic images to its original form. More than 35 sunspots umbra spectrum with area from 1 to 106 millionths have been recorded. The currently available data is not rich enough but some implications are available. We can state with assurance that HeI 10830 triplet really exist in sunspot umbrae and its line-depth, equivalent line-width, and half-width are increasing with sunspot area. For leader and individual unipolar sunspots triplet dependences between line parameters and area spot have been found which are quite differ from those obtained for f-spots. We have not possess clear conception of the nature of observed effects, but possible suggestion taken into account magnetic topology of active regions is discussed.
Chuprakov S. A.
Papushev Pavel G.
Zagaynova Yu. S.
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