Publication Date:
2023-06-13
Description:
We have developed a new three-dimensional (3D) MHD simulation model of the propagation of coronal mass ejections (CMEs) through the upper corona and inner solar wind region. We implement a characteristics-based boundary conditions in an existing solar wind simulation model. The new model allows us to obtain the steady-state solar wind in the trans-magnetosonic regions subject to synoptic magnetogram data and simulate CME propagation from the low corona. Specifically, we define an inner boundary surface at 2.5 solar radii (Rs) and use a physics-based erupting flux rope model of CMEs to calculate the 3D CME dynamics from the initial expansion and to 2.5Rs. The passage of the model CME through this spherical surface is numerically implemented by using the values of magnetic field vector, plasma density, and plasma velocity vector on the cross-sectional intersection of the expanding model flux rope and the spherical surface at 2.5 Rs. Here, the initial flux rope is chosen so that the calculated height-time trajectory and synthetic coronagraph images fit the observed CME data in the initial phases. We discuss the simulated propagation of the model CME and its self-consistent interaction with the ambient solar wind beyond the 2.5-Rs boundary surface.
Language:
English
Type:
info:eu-repo/semantics/conferenceObject
Permalink