Chun-Fan Liu (ASIAA), Hsien Shang (ASIAA), Gregory J. Herczeg (KIAA/PKU), Frederick M. Walter (Stony Brook Univ.)
Spatially resolved [Ne III] spectra in the Sz 102 microjets were obtained through the Hubble Space Telescope Imaging Spectrograph (HST/STIS) at a spatial resolution of ∼0.′′1. The majority of the microjet emission is confined within ∼0.′′25 from the star, but with a fainter extension up to ∼0.′′5. The blueshifted and redshifted [Ne III] emission both show peak intensity within ∼0.′′1 of the star and gradually decay along the flow. Ca II H and K lines are also detected from the redshifted microjet, atop a 300-km/s wide stellar component. The spatial distribution and extent of the [Ne III] microjet is consistent with the scenario that the jet is ionized close to the base, most probably by X-rays hardened by magnetic reconnection induced by star–disk interactions above the disk mid-plane, and subsequently recombines with a recombination timescale longer than the flow time.