Cheung, Mark C.M.De Pontieu, B.Tarbell, Ted D.Fu, Y.Tian, HuiTesta, PaolaReeves, Kathy K.Martínez-Sykora, J.Boerner, B.Wülser, J.P.Lemen, JamesTitle, Alan M.Hurlburt, Neal E.Kleint, LuciaKankelborg, CharlesJaeggli, SarahGolub, LeonMcKillop, SeanSaar, StevenCarlsson, MatsHansteen, Viggo H.2016-03-152016-03-152015-03-05Cheung, Mark C. M., B. De Pontieu, T. D. Tarbell, Y. Fu, H. Tian, P. Testa, K. K. Reeves, et al. “Homologous Helical Jets: Observations By IRIS, SDO , AND Hinode and Magnetic Modeling with Data-Driven Simulations.” The Astrophysical Journal 801, no. 2 (March 5, 2015): 83. doi:10.1088/0004-37x/801/2/83.0004-637Xhttps://scholarworks.montana.edu/handle/1/9621We report on observations of recurrent jets by instruments on board the Interface Region Imaging Spectrograph, Solar Dynamics Observatory (SDO), and Hinode spacecraft. Over a 4 hr period on 2013 July 21, recurrent coronal jets were observed to emanate from NOAA Active Region 11793. Far-ultraviolet spectra probing plasma at transition region temperatures show evidence of oppositely directed flows with components reaching Doppler velocities of ±100 km s−1. Raster Doppler maps using a Si iv transition region line show all four jets to have helical motion of the same sense. Simultaneous observations of the region by SDO and Hinode show that the jets emanate from a source region comprising a pore embedded in the interior of a supergranule. The parasitic pore has opposite polarity flux compared to the surrounding network field. This leads to a spine-fan magnetic topology in the coronal field that is amenable to jet formation. Time-dependent data-driven simulations are used to investigate the underlying drivers for the jets. These numerical experiments show that the emergence of current-carrying magnetic field in the vicinity of the pore supplies the magnetic twist needed for recurrent helical jet formation.Article