Birth places of extreme ultraviolet waves driven by impingement of solar jets upon coronal loops

TL;DR

This study investigates the origins of EUV waves driven by solar jets interacting with coronal loops, revealing they tend to originate at the weakest magnetic field regions of the loops.

Contribution

It provides new insights into the formation sites of jet-driven EUV waves, emphasizing the role of magnetic field strength at loop ends during jet interactions.

Findings

EUV waves form at the weakest magnetic field regions of loops.

Jet-driven EUV waves can occur without associated CMEs.

Interactions occur at different parts of the loops, including top and ends.

Abstract

Solar extreme ultraviolet (EUV) waves are large-scale propagating disturbances in the corona. It is generally believed that the vital key for the formation of EUV waves is the rapid expansion of the loops that overlie erupting cores in solar eruptions, such as coronal mass ejections (CMEs) and solar jets. However, the details of the interaction between the erupting cores and overlying loops are not clear, because that the overlying loops are always instantly opened after the energetic eruptions. Here, we present three typical jet-driven EUV waves without CME to study the interaction between the jets and the overlying loops that remained closed during the events. All three jets emanated from magnetic flux cancelation sites in source regions. Interestingly, after the interactions between jets and overlying loops, three EUV waves respectively formed ahead of the top, the near end (close to the jet source), and the far (another) end of the overlying loops. According to the magnetic field distribution of the loops extrapolated from Potential Field Source Surface method, it is confirmed that the birth places of three jet-driven EUV waves were around the weakest magnetic field strength part of the overlying loops. We suggest that the jet-driven EUV waves preferentially occur at the weakest part of the overlying loops, and the location can be subject to the magnetic field intensity around the ends of the loops.