  We performed a 3D radiative MHD simulation of the solar atmosphere. This
simulation shows a jet-like feature that shows similarities to the type II
spicules observed for the first time with Hinode. Rapid Blueshifted Events
(RBEs) on the solar disk are associated with these spicules. Observational
results suggest they may contribute significantly in supplying the corona with
hot plasma. We perform a detailed comparison of the properties of the simulated
jet with those of type II spicules (observed with Hinode) and RBEs (with
ground-based instruments). We analyze variety of synthetic emission and
absorption lines from the simulations including chromospheric Ca II and Ha to
TR and coronal temperatures (10E4 to several 10E6K). We compare their synthetic
intensities, line profiles, Doppler shifts, line widths and asymmetries with
observations from Hinode/SOT and EIS, SOHO/SUMER, SST and SDO/AIA. Many
properties of the synthetic observables resemble the observations, and we
describe in detail the physical processes that lead to these observables.
Detailed analysis of the synthetic observables provides insight into how
observations should be analyzed to derive information about physical variables
in such a dynamic event. For example, we find that LOS superposition in the
optically thin atmosphere requires the combination of Doppler shifts and
spectral line asymmetry to determine the velocity in the jet. Other properties
differ from the observations, especially in the chromospheric lines. The mass
density of the part of the spicule with a chromospheric temperature is too low
to produce significant opacity in chromospheric lines. These and other
discrepancies are described in detail, and we discuss which mechanisms and
physical processes may need to be included in the MHD simulations to mimic the
thermodynamic processes of the chromosphere and corona, in particular to
reproduce type II spicules.
