The evolution of coronal mass ejections in the inner heliosphere : Implementing the spheromak model with EUHFORIA

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Verbeke , C , Pomoell , J & Poedts , S 2019 , ' The evolution of coronal mass ejections in the inner heliosphere : Implementing the spheromak model with EUHFORIA ' , Astronomy & Astrophysics , vol. 627 , 111 .

Title: The evolution of coronal mass ejections in the inner heliosphere : Implementing the spheromak model with EUHFORIA
Author: Verbeke, C.; Pomoell, J.; Poedts, S.
Contributor: University of Helsinki, Space Physics Research Group
Date: 2019-07-09
Language: eng
Number of pages: 15
Belongs to series: Astronomy & Astrophysics
ISSN: 1432-0746
Abstract: Aims. We introduce a new model for coronal mass ejections (CMEs) that has been implemented in the magnetohydrodynamics (MHD) inner heliosphere model EUHFORIA. Utilising a linear force-free spheromak (LFFS) solution, the model provides an intrinsic magnetic field structure for the CME. As a result, the new model has the potential to predict the magnetic components of CMEs at Earth. In this paper, we present the implementation of the new model and show the capability of the new model. Methods. We present initial validation runs for the new magnetised CME model by considering the same set of events as used in the initial validation run of EUHFORIA that employed the Cone model. In particular, we have focused on modelling the CME that was responsible for creating the largest geomagnetic disturbance (Dst index). Two scenarios are discussed: one where a single magnetised CME is launched and another in which we launch all five Earth-directed CMEs that were observed during the considered time period. Four out of the five CMEs were modelled using the Cone model. Results. In the first run, where the propagation of a single magnetized CME is considered, we find that the magnetic field components at Earth are well reproduced as compared to in-situ spacecraft data. Considering a virtual spacecraft that is separated approximately seven heliographic degrees from the position of Earth, we note that the centre of the magnetic cloud is missing Earth and a considerably larger magnetic field strength can be found when shifting to that location. For the second run, launching four Cone CMEs and one LFFS CME, we notice that the simulated magnetised CME is arriving at the same time as in the corresponding full Cone model run. We find that to achieve this, the speed of the CME needs to be reduced in order to compensate for the expansion of the CME due to the addition of the magnetic field inside the CME. The reduced initial speed of the CME and the added magnetic field structure give rise to a very similar propagation of the CME with approximately the same arrival time at 1 au. In contrast to the Cone model, however, the magnetised CME is able to predict the magnetic field components at Earth. However, due to the interaction between the Cone model CMEs and the magnetised CME, the magnetic field amplitude is significantly lower than for the run using a single magnetised CME. Conclusions. We have presented the LFFS model that is able to simulate and predict the magnetic field components and the propagation of magnetised CMEs in the inner heliosphere and at Earth. We note that shifting towards a virtual spacecraft in the neighbourhood of Earth can give rise to much stronger magnetic field components. This gives the option of adding a grid of virtual spacecrafts to give a range of values for the magnetic field components.
Subject: magnetohydrodynamics (MHD)
methods: numerical
Sun: coronal mass ejections (CMEs)
Sun: magnetic fields
Sun: heliosphere
solar-terrestrial relations
115 Astronomy, Space science

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