Helmet streamers with triple structures: Simulations of resistive dynamics

Recent observations of the solar corona with the LASCO coronagraph on board of the SOHO spacecraft have revealed the occurrence of triple helmet strea mers even during solar minimum, which occasionally go unstable and give ris e to large coronal mass ejections. There are also indications that the slow solar wind is either a combination of a quasi-stationary flow and a highly fluctuating component or may even be caused completely by many small erupt ions or instabilities. As a first step we recently presented an analytical method to calculate simple two-dimensional stationary models of triple helm et streamer configurations. In the present contribution we use the equation s of time-dependent resistive magnetohydrodynamics to investigate the stabi lity and the dynamical behaviour of these configurations. We particularly f ocus on the possible differences between the dynamics of single isolated st reamers and triple streamers and on the way in which magnetic reconnection initiates both small scale and large scale dynamical behaviour of the strea mers. Our results indicate that small eruptions at the helmet streamer cusp may incessantly accelerate small amounts of plasma without significant cha nges of the equilibrium configuration and might thus contribute to the non- stationary slow solar wind. On larger time and length scales, large coronal eruptions can occur as a consequence of large scale magnetic reconnection events inside the streamer configuration. Our results also show that triple streamers are usually more stable than a single streamer.