Observations of microwave emission from solar jets and comparison with MHD simulations

TL;DR

This study compares microwave emissions from solar jets observed in reality with those generated by 3D MHD simulations, assessing the models' accuracy in replicating jet features and proposing improvements.

Contribution

It introduces a method to compute microwave emission from 3D MHD simulations and compares these with actual solar jet observations, highlighting model strengths and limitations.

Findings

MHD simulations reasonably reproduce lower-intensity jets.

Discrepancies exist between simulations and stronger observed jets.

Suggestions are made to improve the realism of MHD models.

Abstract

We computed the thermal microwave emission from a 3D magnetohydrodynamic (MHD) simulation and compared it with observations of solar jets. The simulation treats the emergence of magnetic flux into the solar atmosphere and its interaction with a low, pre-existing ambient magnetic field. This interaction leads to the formation and development of a jet, driven by an eruption. The computed 17 GHz radio emission is compared with a number of observed jets, with respect to their morphology, their flux, and the rise time of the radio flux. We find that the MHD model reproduces the characteristics of lower-intensity jets reasonably well, whereas there are differences with stronger jets. We suggest possible ways to obtain more realistic jets from MHD simulations, so that they match better the real jets.