SOLARNET Conference: The Many Scales of the Magnetic Sun

Modelling solar eruptive events from their onset to their propagation at 1 AU

10 May 2023, 12:10

15m

Haus H, Telegrafenberg

Oral presentation 3) Energy and mass flow through the solar atmosphere – from solar campfires to CME (Observations and Theory) Energy and mass flow through the solar atmosphere – from solar campfires to CME (Observations and Theory)

Speaker

Antoine Strugarek

Description

In the era of Solar Orbiter and Parker Solar Probe, we have now an unprecedented view on eruptive events of the Sun, from their onset to their propagation in the heliosphere. Thanks to the proximity of the probes to the Sun for at least part of their orbit, we are currently acquiring more and more key data on the structuring and the propagation of solar eruptive events, as well as on the acceleration of particles at each stage of the eruption and propagation.

I will report on an on-going modelling effort of solar eruptive events using the versatile PLUTO code within the STORMGENESIS project. I will present a full MHD effort to model idealised and realistic and eruptive active regions, based on the initiation of the magnetic with both non-linear force-free and non force-free extrapolations. I will present very recent result on the modelling of the eruption of active region #12241, which is well reproduced when using a non force-free initiation. Coupled to charged test-particles under the gyrokinetic approximation, and to the heating and cooling associated with magnetic reconnection and radiative losses, I will present first results on the prediction for thermal and non-thermal emission from this active region.

In a second part, I will show how the same simulation framework, now using adaptive mesh refinement, can be used to model the propagation of coronal mass ejections from their onset to their propagation up to 1 AU in a realistically structured solar wind. These results, published recently in Regnault et al. (2023), allow to highlight the generic features of CMES and the simulation results compare very well with superposed-epochs analysis of hundreds of CMEs. In addition, these simulations point towards various rotation patterns of the CMEs that depend on their size and that happen during the initial stage of their propagation within the Alfvén surface. These results warrant further analyses, coupling the two set of simulations presented here to provide a complete picture of the energetics and of thermal and non-thermal emission of solar eruptive events.