Can solar wind viscous drag account for CME deceleration?

Abstract

The forces acting on solar Coronal Mass Ejections (CMEs) in the interplanetary medium have been evaluated so far in terms of an empirical drag coefficient $C_{\mathrm{D}}\sim 1$ that quantifies the role of the aerodynamic drag experienced by a typical CME due to its interaction with the ambient solar wind. We use a microphysical prescription for viscosity in the turbulent solar wind to obtain an analytical model for the drag coefficient $C_{\mathrm{D}}$. This is the first physical characterization of the aerodynamic drag experienced by CMEs. We use this physically motivated prescription for $C_{\mathrm{D}}$ in a simple, 1D model for CME propagation to obtain velocity profiles and travel times that agree well with observations of deceleration experienced by fast CMEs.

Accepted for publication in the Geophysical Research Letters

References in corpus (4)

• Comprehensive Analysis of Coronal Mass Ejection Mass and Energy Properties Over a Full Solar Cycle
• Propagation of an Earth-directed coronal mass ejection in three dimensions
• Energetics of solar coronal mass ejections
• Solar Wind Drag and the Kinematics of Interplanetary Coronal Mass Ejections

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