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 \(\approx 10^{25}\) ergs. The fact that the flux density of the radio transient is only \(\approx 2\) 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.

最近发现了来自安静太阳的非热射电瞬变，粗略计算推测它们可能对日冕加热很重要。众所周知，使用相干发射的能量计算通常受到约束条件较差的参数的影响，因此具有很大的不确定性。然而，使用极紫外 (EUV) 和软 X 射线波段观测的能量估计是常规完成的，并且这些技术已经非常成熟。这项工作首次尝试识别这些无线电瞬变的 EUV 对应物，然后使用它们来估计事件期间沉积到日冕中的能量。我表明，这里研究的一组无线电瞬变与在 EUV 波段中观察到的增亮有关，并且是由能量释放产生的\(\大约 10^{25}\) 尔格。无线电瞬变的通量密度仅为\(\approx 2\)  mSFU 这一事实表明，未来有可能进行大型统计研究，以了解这些无线电瞬变与其他 EUV 和 X 射线对应物之间的关系，以及了解它们在日冕加热中的重要性。