Modeling Jets in the Corona and Solar Wind

TL;DR

This paper reviews observations and numerical models of coronal jets, highlighting advances in simulations that incorporate thermodynamic MHD and large domains to better understand their role in solar wind acceleration.

Contribution

It introduces next-generation thermodynamic MHD simulations with large spherical domains to study coronal jets and their contribution to the solar wind.

Findings

Enhanced models include energy transfer processes.

Simulations cover large spherical regions.

Potential to answer open questions about jets.

Abstract

Coronal jets are transient, collimated eruptions that occur in regions of predominantly open magnetic field in the solar corona. Our understanding of these events has greatly evolved in recent years but several open questions, such as the contribution of coronal jets to the solar wind, remain. Here we present an overview of the observations and numerical modeling of coronal jets, followed by a brief description of "next-generation" simulations that include an advanced description of the energy transfer in the corona ("thermodynamic MHD"), large spherical computational domains, and the solar wind. These new models will allow us to address some of the open questions.