Studying the internal topology of Heliospheric Flux-ropes

In heliophysics, a flux rope could be defined as a confined magnetized plasma within magnetic field lines wrapping around an axis in a twisting but not necessarily a monotonic way. Nieves-Chinchilla et al. 2016, 2018 describes a flux rope model built on the flexibility of a non-orthogonal coordinate system that adds complexity in the magnetic structure with the  incorporation of current density components that are generalized in a polynomial series. This work aims to develop a methodology to explore the current density distribution within the helispheric flux ropes that will serve as constraint to the flux rope modeling and 3D reconstruction as well as to add understanding on the flux rope formation and evolution in the solar wind.