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.
@article{arxiv.1511.09350,
title = {Modeling Jets in the Corona and Solar Wind},
author = {T. Torok and R. Lionello and V. S. Titov and J. E. Leake and Z. Mikic and J. A. Linker and M. G. Linton},
journal= {arXiv preprint arXiv:1511.09350},
year = {2015}
}