Abstract Post-flare loops are generally observed between two ribbon flares. The formation of post flare loops and active region or plage filaments has been explained in a model based on magnetic reconnection and chromospheric ablation /1,2/. This model uses a magnetic topology which is relevant to solar flares /3/ : a large flare or an instability opens the magnetic lines of a coronal arcade (or arch) and a vertical current sheet forms. Then the reconnection of the magnetic field follows according to the scenario of Kopp and Pneuman /4/. In this magnetic configuration, we show that the formation of condensations or dense loops is induced by reconnection shocks. We give in this communication a new method of diagnostic to derive from Hα profiles physical parameters, i.e. source function, optical depth and velocity. This method called “differential cloud method” is very promising for future observations.


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    Titel :

    Post-flare loops: formation and velocity


    Beteiligte:
    Schmieder, B. (Autor:in) / Mein, P. (Autor:in) / Malherbe, J.-M. (Autor:in) / Forbes, T.G. (Autor:in)

    Erschienen in:

    Advances in Space Research ; 8 , 11 ; 145-148


    Erscheinungsdatum :

    1989-01-01


    Format / Umfang :

    4 pages




    Medientyp :

    Aufsatz (Zeitschrift)


    Format :

    Elektronische Ressource


    Sprache :

    Englisch



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