Volume 380, Number 1, December II 2001
|Page(s)||341 - 346|
|Section||Planets and planetary systems|
|Published online||15 December 2001|
Coronal loop hydrodynamics
The solar flare observed on November 12, 1980 revisited: The UV line emission
Osservatorio Astronomico di Palermo, Palazzo dei Normanni, P.zza del Parlamento, 1, 90134 Palermo, Italy
2 Dipartimento di Scienze Fisiche e Astronomiche, Sezione di Astronomia, University of Palermo, Palazzo dei Normanni, P.zza del Parlamento, 1 90134 Palermo, Italy e-mail: firstname.lastname@example.org
Corresponding author: G. Peres, email@example.com
Accepted: 10 October 2001
We revisit a well-studied solar flare whose X-ray emission originating from a simple loop structure was observed by most of the instruments on board SMM on November 12, 1980. The X-ray emission of this flare, as observed with the XRP, was successfully modeled previously. Here we include a detailed modeling of the transition region and we compare the hydrodynamic results with the UVSP observations in two EUV lines, measured in areas smaller than the XRP rasters, covering only some portions of the flaring loop (the top and the foot-points). The single loop hydrodynamic model, which fits well the evolution of coronal lines (those observed with the XRP and the Fe xxi 1354.1 Å line observed with the UVSP) fails to model the flux level and evolution of the O v 1371.3 Å line.
Key words: Sun: corona / Sun: transition region / hydrodynamics / Sun: flares
© ESO, 2001
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