  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.
