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In this paper we present a numerical study of the time evolution of solarprominences embedded in sheared magnetic arcades. The prominence is representedby a density enhancement in a background stratified atmosphere and is connectedto the photosphere through the magnetic field. By solving the idealmagnetohydrodynamic (MHD) equations in three dimensions we study the dynamicsfor a range of parameters representative of real prominences. Depending on theparameters considered, we find prominences that are suspended above thephotosphere, i.e., detached prominences, but also configurations resemblingcurtain or hedgerow prominences whose material continuously connects to thephotosphere. The plasma$-\beta$ is an important parameter that determines theshape of the structure. In many cases magnetic Rayleigh-Taylor (MRT)instabilities and oscillatory phenomena develop. Fingers and plumes aregenerated, affecting the whole prominence body and producing verticalstructures in an essentially horizontal magnetic field. However, magnetic shearis able to reduce or even to suppress this instability.

Morphology and dynamics of solar prominences from 3D MHD simulations