From Jets to CMEs: Observations of the Breakout Continuum

The magnetic breakout model can explain a variety of eruptive solar events, from jets to coronal mass ejections (CMEs). The breakout model is consistent with many observed fast CMEs/eruptive flares, in terms of the underlying multipolar topology, pre-eruption activities, and sequence of reconnection onsets. We have also demonstrated that most observed coronal-hole jets in fan-spine topologies are produced by breakout and flare reconnection above a filament channel (with or without a filament). For eruptions occurring in such topologies, the key question is, why are some events jets while others form slow or fast CMEs? We have analyzed SDO/AIA, LASCO, and RHESSI observations focusing on the initiation of CMEs in large bright points (small active regions) in coronal holes with clear fan-spine topologies. Our analysis revealed pre-eruptive evidence for slow breakout reconnection before the onset of jets, slow CMEs, and fast CMEs from these ARs. We find that this continuum of activity is consistent with the breakout model of solar eruptions, and explore the factors contributing to the different forms of dynamic behavior.