  This paper presents an improved MHD modeling of the confined filament
eruption in solar active region NOAA~9957 on 2002 May~27 by extending the
parametric studies of the event in Torok & Kliem 2005 and Hassanin & Kliem
2016. Here the initial flux rope equilibrium is chosen to possess a small apex
height identical to the observed initial filament height, which implies a more
realistic inclusion of the photospheric line tying. The model matches the
observations as closely as in the preceding studies, with the closest agreement
again being obtained for an initial average flux rope twist of about $4\pi$.
Thus, the model for strongly writhing confined solar eruptions, which assumes
that a kink-unstable flux rope in the stability domain of the torus instability
exists at the onset of the eruption's main acceleration phase, is further
substantiated.
