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Recent observations of the solar corona with the LASCO coronagraph on boardof the SOHO spacecraft have revealed the occurrence of triple helmet streamerseven during solar minimum, which occasionally go unstable and give rise tolarge coronal mass ejections. There are also indications that the slow solarwind is either a combination of a quasi-stationary flow and a highlyfluctuating component or may even be caused completely by many small eruptionsor instabilities. As a first step we recently presented an analytical method tocalculate simple two-dimensional stationary models of triple helmet streamerconfigurations. In the present contribution we use the equations of time-dependent resistive magnetohydrodynamics to investigate the stability and thedynamical behaviour of these configurations. We particularly focus on thepossible differences between the dynamics of single isolated streamers andtriple streamers and on the way in which magnetic reconnection initiates bothsmall scale and large scale dynamical behaviour of the streamers. Our resultsindicate that small eruptions at the helmet streamer cusp may incessantlyaccelerate small amounts of plasma without significant changes of theequilibrium configuration and might thus contribute to the non-stationary slowsolar wind. On larger time and length scales, large coronal eruptions can occuras a consequence of large scale magnetic reconnection events inside thestreamer configuration. Our results also show that triple streamers are usuallymore stable than a single streamer.

Helmet Streamers with Triple Structures: Simulations of resistive dynamics