Volume 439, Number 1, August III 2005
|Page(s)||351 - 359|
|Published online||22 July 2005|
Electron density along a coronal loop observed with CDS/SOHO
Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland e-mail: firstname.lastname@example.org
2 Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK
3 Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany
4 Department of Solar Physics, Royal Observatory of Belgium, Av. Circulaire 3, 1180 Bruxelles, Belgium
Accepted: 21 April 2005
The analysis of a coronal loop observed by CDS and EIT on board SOHO is presented. The loop was situated above the North-East limb at a latitude of ~48°, being clearly visible in the hottest lines of the dataset, Fe xvi 360.76 Å, i.e. greater than 2 000 000 K. The cooler lines in the sample (i.e. O v 629.73 Å and He i 584.35 Å) showed only a brightening at the footpoints location. Based on the Fe xiv 353.84/334.17 line ratio, the electron density along the loop was determined following three different approaches for the background subtraction. No differences, within the error bars, can be found between the three methods. At the apex, the density is cm-3, while at the footpoint it is 50% greater, i.e. cm-3. The inferred filling factor values along the loop, at the formation temperature of the lines, are in the range 0.2–0.9. One dimensional hydrodynamic modelling of the loop along a given field line, gravity neglected, was performed. A minimum analysis results in a best fit case where the total energy input is directed preferentially to the loop footpoint (the heating rate is three times larger at the base than at the apex). An isochoric solution can not be ruled out completely. The exercise illustrates the necessity of accurate spectral diagnostics in order to derive definite conclusions from theoretical models and suggests the need for simultaneous density and temperature diagnostics.
Key words: Sun: corona / plasmas / hydrodynamics
© ESO, 2005
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