  We present the first observation, analysis and modeling of solar coronal twin
jets, which occurred after a preceding jet. Detailed analysis on the kinetics
of the preceding jet reveals its blowout-jet nature, which resembles the one
studied in Liu et al. 2014. However the erupting process and kinetics of the
twin jets appear to be different from the preceding one. In lack of the
detailed information on the magnetic fields in the twin jet region, we instead
use a numerical simulation using a three-dimensional (3D) MHD model as
described in Fang et al. 2014, and find that in the simulation a pair of twin
jets form due to reconnection between the ambient open fields and a highly
twisted sigmoidal magnetic flux which is the outcome of the further evolution
of the magnetic fields following the preceding blowout jet. Based on the
similarity between the synthesized and observed emission we propose this
mechanism as a possible explanation for the observed twin jets. Combining our
observation and simulation, we suggest that with continuous energy transport
from the subsurface convection zone into the corona, solar coronal twin jets
could be generated in the same fashion addressed above.
