In a nutshell
The project aims at testing theories of the origin of stellar winds, and here in particular the slow solar wind. We are using compositional measurements inferred from remote-sensing and/or in-situ data from Parker Solar Probe and Solar Orbiter spacecraft. We are building a model that accounts not only for the magnetic topology of the coronae but also for the multi-species, multi-temperature, highly structured nature of the solar atmosphere.
Our novel approach
No model has yet explained at the same time the bulk and compositional properties of the SSW. We will develop the first 3-D model of coronal ions solving along realistic magnetic field lines topologies for the coupled transport of important major and minor constituents. The model will compute dynamically for the emissions and the plasma moments of the different particles.
The model results will be evaluated with readily available in situ and remote-sensing data (ACE, Wind, STEREO, SoHO, SDO) as well as Parker Solar Probe (SWEAP, FIELDS, WISPR, first data in November 2018 at 35,7 solar radii from the Sun) and is an excellent preparation for combined multi-instrumental science with Solar Orbiter.
Our key questions
Our project is organised around 5 key scientific questions. Results can be found in our Publications page.
- Q1: Can the SSW bulk properties and composition be explained by quasi steady-state processes?
- Q2: Can the remote observations of the SSW source region be explained by steady-state theories?
- Q3: What causes variations in He abundance and the strong FIP effect in the SSW in steady state?
- Q4: What causes the variability of the SSW?
- Q5: Can we produce a self-consistent model of the SSW?