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We present a 2.5-dimensional magnetohydrodynamic simulation of asystematically rotating prominence inside its coronal cavity using theopen-source \texttt{MPI-AMRVAC} code. Our simulation starts from anon-adiabatic, gravitationally stratified corona, permeated with a shearedarcade magnetic structure. The flux rope (FR) is formed through converging andshearing footpoints driving, simultaneously applying randomized heating at thebottom. The latter induces a left-right asymmetry of temperature and densitydistributions with respect to the polarity-inversion line. This asymmetrydrives flows along the loops before the FR formation, which gets converted tonet rotational motions upon reconnection of the field lines. As the thermalinstability within the FR develops, angular momentum conservation about itsaxis leads to a systematic rotation of both hot coronal and cold condensedplasma. The initial rotational velocity exceeds $60\ \mathrm{km\ s^{-1}}$. Thesynthesized images confirm the simultaneous rotations of the coronal plasmaseen in 211 and 193 \AA\ and condensations seen in 304 \AA. Furthermore, theformation of the dark cavity is evident in 211 and 193 \AA\ images. Ournumerical experiment is inspired by observations of so-called giant solarprominence tornadoes, and reveals that asymmetric FR formation can be crucialin triggering rotational motions. We reproduce observed spinning motions insidethe coronal cavity, augmenting our understanding of the complex dynamics ofrotating prominences.

Rotational flows in solar coronal flux rope cavities