  In recent years, space weather research has focused on developing modelling
techniques to predict the arrival time and properties of coronal mass ejections
(CMEs) at the Earth. The aim of this paper is to propose a new modelling
technique suitable for the next generation of Space Weather predictive tools
that is both efficient and accurate. The aim of the new approach is to provide
interplanetary space weather forecasting models with accurate time dependent
boundary conditions of erupting magnetic flux ropes in the upper solar corona.
To produce boundary conditions, we couple two different modelling techniques,
MHD simulations and a quasi-static non-potential evolution model. Both are
applied on a spatial domain that covers the entire solar surface. The
non-potential model uses a time series of observed synoptic magnetograms to
drive the non-potential quasi-static evolution of the coronal magnetic field.
This allows us to follow the formation and loss of equilibrium of magnetic flux
ropes. Following this a MHD simulation captures the dynamic evolution of the
erupting flux rope. The present paper focuses on the MHD simulations that
follow the ejection of magnetic flux ropes to 4$R_\odot$. We first propose a
technique for specifying the pre-eruptive plasma properties in the corona.
Next, time dependent MHD simulations describe the ejection of two magnetic flux
ropes, that produce time dependent boundary conditions for the magnetic field
and plasma at 4$R_{\odot}$. In the present paper, we show that the dual use of
quasi-static non-potential magnetic field simulations and full time dependent
MHD simulations can produce realistic inhomogeneous boundary conditions for
space weather forecasting tools. Before a fully operational model can be
produced there are a number of technical and scientific challenges that still
need to be addressed.
