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We present the first observation, analysis and modeling of solar coronal twinjets, which occurred after a preceding jet. Detailed analysis on the kineticsof the preceding jet reveals its blowout-jet nature, which resembles the onestudied in Liu et al. 2014. However the erupting process and kinetics of thetwin jets appear to be different from the preceding one. In lack of thedetailed information on the magnetic fields in the twin jet region, we insteaduse a numerical simulation using a three-dimensional (3D) MHD model asdescribed in Fang et al. 2014, and find that in the simulation a pair of twinjets form due to reconnection between the ambient open fields and a highlytwisted sigmoidal magnetic flux which is the outcome of the further evolutionof the magnetic fields following the preceding blowout jet. Based on thesimilarity between the synthesized and observed emission we propose thismechanism as a possible explanation for the observed twin jets. Combining ourobservation and simulation, we suggest that with continuous energy transportfrom the subsurface convection zone into the corona, solar coronal twin jetscould be generated in the same fashion addressed above.

On the Observation and Simulation of Solar Coronal Twin Jets