Solar Coronal Jets: Observations, Theory, and Modeling

TL;DR

This paper reviews the observations, theoretical understanding, and modeling of solar coronal jets, emphasizing their role in solar activity, coronal heating, and solar wind acceleration, and highlighting their significance in solar physics research.

Contribution

It provides a comprehensive synthesis of current knowledge on coronal jets, integrating observational data, theoretical frameworks, and modeling approaches to advance understanding of their physics.

Findings

Jets are key to understanding solar transients and energy transfer.

Jets share properties with larger solar eruptions like flares and CMEs.

Studying jets offers insights into coronal heating and solar wind acceleration.

Abstract

Coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of "nominal" solar flares and coronal mass ejections (CMEs), jets share many common properties with these phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems.