A Spectroscopic Model of euv Filaments |
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| Authors: | Heinzel P Anzer U Schmieder B |
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| Institution: | (1) Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching, Germany;(2) Observatoire de Paris, Section Meudon, LESIA, F-92195 Meudon Principal Cedex, France;(3) Institute of Theoretical Astrophysics, University of Oslo, Blindern, N-0315 Oslo, Norway |
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| Abstract: | We propose a new spectroscopic model for extended dark structures around Hα filaments observed in EUV lines. As in previous
papers, we call these structures EUV filaments. Our model uses at least three observed EUV lines (located shortward the hydrogen
Lyman-continuum limit) to compute iteratively the altitudes at which the EUV filament extensions are located. A transition-region line (O v in the present case) can be used to derive the opacity of the Lyman continuum and the other two coronal lines (e.g., Mg x and Si xii) then give two heights: the bottom and top of the EUV filament. The method takes into account self-consistently
the absorption of EUV-line radiation by the Lyman continuum, as well as the volume-blocking effect potentially important for
coronal lines. As an example we compute the heights of the EUV filament at one particular position, using CDS data for the
5 May 2000 filament. At this position, the EUV filament extension lies between altitudes 28 700 and 39 000 km, so that the
geometrical thickness of the structure is 10300 km (we discuss also the sensitivity of our models to variations of the line
intensities). These heights are consistent with the concept of twisted magnetic flux tubes, but there could be also some influence
on our results due to additional low lying cool structures from parasitic polarities. |
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