Magnetohydrodynamic simulation of a magnetic cloud observed during the near-radial alignment of Solar Orbiter and Wind Spacecraft

In this work, we have used a constant-turn flux rope model to simulate a coronal mass ejection (CME) containing a magnetic cloud (MC) in a data-driven solar wind background. The MC was detected by Solar Orbiter (SO) on 19 April 2020 and the Wind spacecraft on 20 April 2020, when both spacecraft were in near-radial alignment. We constrain the flux rope model using graduated cylindrical shell model parameters for this CME. We have performed an ensemble simulation to obtain a range of reproduced plasma and magnetic field values at SO and Wind. We further used Heliospheric Imager (HI) data of STEREO A to weight the ensemble members and provide an improved hindcast of this CME at SO and Wind. We show that the magnetic field of the magnetic cloud is hindcasted with reasonable accuracy at both SO and Wind in our simulations. We compare the observed and simulated radial evolution of the magnetic cloud to comment on the validity of the constant-turn flux rope model to forecast CMEs.