Magnetohydrodynamic modeling of prominence formation within a helmet streamer

We present a 2.5-D axisymmetric MHD model to self-consistently describe the formation of a stable prominence that supports cool, dense material in the lower corona. The upper chromosphere and transition region are included in the calculation. Reducing the magnetic flux along the neutral line of a sh eared coronal arcade forms a magnetic field configuration with a flux rope topology. The prominence forms when dense chromospheric material is brought up and condenses in the corona. The prominence sits at the base of a helme t streamer structure. The dense material is supported against gravity in th e dips of the magnetic field lines in the flux rope. Further reduction in m agnetic flux leads to an eruption of the prominence, ejecting material into the solar wind.