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Jets often have a helical structure containing ejected plasma that is bothhot and also cooler and denser than the corona. Various mechanisms have beenproposed to explain how jets are primarily attributed to a magneticreconnection between the emergence of magnetic flux and environment or that oftwisted photospheric motions that bring the system into a state of instability.Multi-wavelength observations of a twisted jet observed with AIA and IRIS wereused to understand how the twist was injected into the jet. We followed themagnetic history of the active region based on the analysis of HMI vectormagnetic field computed with the UNNOFIT code. This region is the result of thecollapse of two emerging magnetic fluxes (EMFs) overlaid by arch filamentsystems that have been well-observed with AIA, IRIS, and NVST in H-alpha. Inthe magnetic field maps, we found evidence of the pattern of a long sigmoidalflux rope (FR) along the polarity inversion line between the two EMFs, which isthe site of the reconnection. Before the jet, an extension of the FR waspresent and a part of it was detached and formed a small bipole with a baldpatch (BP) region, which dynamically became an X-current sheet over the dome ofone EMF where the reconnection took place. At the time of the reconnection, theMg II spectra exhibited a strong extension of the blue wing that is decreasingover a distance of 10 Mm (from -300 km/s to a few km/s). This is the signatureof the transfer of the twist to the jet. A comparison with numericalmagnetohydrodynamics (MHD) simulations confirms the existence of the long FR.We conjecture that there is a transfer of twist to the jet during the extensionof the FR to the reconnection site without FR eruption. There connection wouldstart in the low atmosphere in the BP reconnection region and extend at anX-point along the current sheet formed above.

The role of small-scale surface motions in the transfer of twist to a solar jet from a remote stable flux rope