Reconstruction of the Parker spiral with the Reverse In situ data and MHD APproach – RIMAP

The reconstruction of plasma parameters in the interplanetary medium is very important to understand propagation solar eruptions and for Space Weather application purposes. Because only a few spacecraft are measuring situ these parameters, reconstructions currently performed by running complex numerical Magneto-hydrodynamic (MHD) simulations starting from remote sensing observations Sun. Current models apply full 3D MHD corona or extrapolations photospheric magnetic fields combined with semi-empirical relationships derive on sphere centered Sun (inner boundary). then propagated up Earth’s orbit beyond. Nevertheless, this approach requires significant theoretical computational efforts, results partial agreement observations. In paper we describe new problem called RIMAP – Reverse data APproach. inner boundary at 0.1 AU derived directly measurements acquired 1 AU, applying back technique remap them into heliosphere. This remapping done using Weber Davies wind model reconstruct flowlines. re-propagated outward simulation based PLUTO code. spiral obtained not much better observations, but also including many more small-scale longitudinal features that reproduced approaches developed so far.