The dynamics of eruptive prominences

TL;DR

This paper reviews the physical and kinematic properties of eruptive prominences and their relationship with CMEs, highlighting their propagation, solar-cycle variation, and deflection effects relevant to space weather.

Contribution

It provides a comprehensive overview of eruptive prominences' dynamics, emphasizing their association with CMEs and implications for modeling and space weather prediction.

Findings

Eruptive prominences are physically and kinematically linked to CMEs.

Polar CMEs are similar to low-latitude CMEs, indicating common eruption mechanisms.

Deflections by coronal holes influence CME trajectories and space weather impacts.

Abstract

This chapter discusses the dynamical properties of eruptive prominences in relation to coronal mass ejections (CMEs). The fact that eruptive prominences are a part of CMEs is emphasized in terms of their physical association and kinematics. The continued propagation of prominence material into the heliosphere is illustrated using in-situ observations. The solar-cycle variation of eruptive prominence locations is discussed with a particular emphasis on the rush-to-the-pole (RTTP) phenomenon. One of the consequences of the RTTP phenomenon is polar CMEs, which are shown to be similar to the low-latitude CMEs. This similarity is important because it provides important clues to the mechanism by which CMEs erupt. The nonradial motion of CMEs is discussed, including the deflection by coronal holes that have important space weather consequences. Finally, the implications of the presented observations for the modeling CME modeling are outlined.