Multi-species modelling of the forming solar wind from the upper chromosphere to Parker Solar Probe

International audienceThe effects of coronal heating on the properties of the escaping solar wind are still debated. We investigate the development of temperature anisotropies in the middle corona measured by past coronal spectrometers by using a 1-D multi-species model of the forming solar wind. The model assumes a bi-Maxwellian distribution function for all species, couples neutral (hydrogen, helium) and charged particles (electrons, protons, charged helium) and includes a self-consistent treatment of ionisation processes in the upper chromosphere and low corona. Our simulations extend to 70 solar radii and we compare our first results with the bulk properties and anisotropies of the ions and electrons measured in situ by Helios and Parker Solar Probe. We study the effects of ion and electron heating separately as well as wave transport and dissipation on the resulting solar wind properties for different coronal topologies including streamers, pseudo-streamers and interplume regions. A first multi-tube implementation of this kinetic-fluid code allows us to compare our results with past spectroscopic measurements by the Solar and Heliospheric Observatory and the future Solar Orbiter mission. Part of this work was funded by the European Research Council through the project SLOW_SOURCE - DLV-81918