  Transient collimated plasma eruptions in the solar corona, commonly known as
coronal (or X-ray) jets, are among the most interesting manifestations of solar
activity. It has been suggested that these events contribute to the mass and
energy content of the corona and solar wind, but the extent of these
contributions remains uncertain. We have recently modeled the formation and
evolution of coronal jets using a three-dimensional (3D) magnetohydrodynamic
(MHD) code with thermodynamics in a large spherical domain that includes the
solar wind. Our model is coupled to 3D MHD flux-emergence simulations, i.e, we
use boundary conditions provided by such simulations to drive a time-dependent
coronal evolution. The model includes parametric coronal heating, radiative
losses, and thermal conduction, which enables us to simulate the dynamics and
plasma properties of coronal jets in a more realistic manner than done so far.
Here we employ these simulations to calculate the amount of mass and energy
transported by coronal jets into the outer corona and inner heliosphere. Based
on observed jet-occurrence rates, we then estimate the total contribution of
coronal jets to the mass and energy content of the solar wind to (0.4-3.0) %
and (0.3-1.0) %, respectively. Our results are largely consistent with the few
previous rough estimates obtained from observations, supporting the conjecture
that coronal jets provide only a small amount of mass and energy to the solar
wind. We emphasize, however, that more advanced observations and simulations
are needed to substantiate this conjecture.
