Bereiche | Tage | Auswahl | Suche | Downloads | Hilfe
EP: Fachverband Extraterrestrische Physik
EP 8: Sonne
EP 8.7: Vortrag
Mittwoch, 28. März 2007, 15:30–15:45, H46
Magnetic structure of the solar transition region as observed in various ultraviolet lines emitted at different temperatures — •Eckart Marsch1 and Chuanyi Tu2 — 1Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau — 2Department of Geophysics, Peking University, Beijing, China
The structure of the solar transition region (TR) in a polar coronal hole of the Sun is studied. In particular, the detailed association of the coronal magnetic field with the radiance patterns of the TR, when seen in various far ultraviolet (FUV) emission lines, is investigated. A comparison is made of the coronal magnetic field, as obtained by extrapolation of the NSO/Kitt-Peak photospheric field to heights of several tens of megameters, with the radiances of many FUV lines, which are emitted by ions of various elements at different ionization stages, corresponding to different local coronal temperatures. By a correlation analysis of the emission pattern with the magnetic field (network and carpet of loops), the so-called correlation height of the emission can be determined. In particular, at mesoscopic scales of several megameters the regions with strong emission (originating from multiple small closed loops) are found to be located at low heights, whereas weak emissions (coming from locally open, i.e. far reaching fields) appear to originate at greater heights. These findings are consistent with results obtained at large scales for large-size loops and big coronal holes. Our correlation-height analysis of the emission lines confirms the notion that plasma at different temperature can coexist at the same height.