Title and Abstract

Title:  Coronal Jets – the Key to Understanding Solar Eruptions and Plumes

Abstract:  Coronal jets are impulsive collimated outflows originating all over the Sun, in both open- and closed-field regions. Hot jets were first detected in soft X-ray images by Yohkoh in the 1980s, and have been observed with increasing temporal and spatial resolution by subsequent missions such as TRACE, SOHO, STEREO, SDO, and Hi-C. Cooler jets, such as spicules, have been observed for much longer, but apparently share many basic traits with their hotter counterparts. Why do we care about the origins and evolution of coronal jets? First, they occur in relatively simple magnetic-field configurations, compared with CMEs and flares. By studying these miniature outbursts, we gain insight into the fundamental physics of the entire range of solar eruptions. Second, these common events release energy and mass into the atmosphere, driving flows, heating local plasma, and accelerating particles. To understand coronal heating and solar-wind generation, then, we must assess the collective contributions of jets to the energetics and dynamics of the corona and heliosphere.

I will begin by summarizing the key features of coronal jets derived from observations, focusing primarily on those occurring in coronal holes (open flux). My talk will then concentrate on what my colleagues and I have learned from data analysis, theory, and modeling about the nature of their source regions, the energy buildup and release processes that power these jets, and the resulting energetics and dynamics. Finally, I will present open questions that might be answered with new observations and simulations.