A Search for the Counterparts of Quiet-Sun Radio Transients in Extreme Ultraviolet Data

Nonthermal radio transients from the quiet Sun have been recently discovered and it has been hypothesized using rough calculations that they might be important for coronal heating. It is well realized that energy calculations using coherent emissions are often subject to poorly constrained parameters and hence have large uncertainties. However, energy estimates using observations in the extreme ultraviolet (EUV) and soft X-ray bands are routinely done and the techniques are pretty well established. This work presents the first attempt to identify the EUV counterparts of these radio transients and then use them to estimate the energy deposited into the corona during the event. I show that the group of radio transients studied here is associated with a brightening observed in the EUV waveband and is produced by an energy release of ≈1025\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\approx 10^{25}$\end{document} ergs. The fact that the flux density of the radio transient is only ≈2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\approx 2$\end{document} mSFU suggests that it might be possible to do large statistical studies in the future for understanding the relationship between these radio transients and other EUV and X-ray counterparts, as well as for understanding their importance in coronal heating.