  In a previous paper we simulated the orbital evolution of dust particles from
the Jupiter Trojan asteroids ejected by the impacts of interplanetary
particles, and evaluated their overall configuration in the form of dust arcs.
Here we compare the orbital properties of these Trojan dust particles and the
Trojan asteroids. Both Trojan asteroids and most of the dust particles are
trapped in the Jupiter 1:1 resonance. However, for dust particles, this
resonance is modified because of the presence of solar radiation pressure,
which reduces the peak value of the semi-major axis distribution. We find also
that some particles can be trapped in the Saturn 1:1 resonance and higher order
resonances with Jupiter. The distributions of the eccentricity, the longitude
of pericenter, and the inclination for Trojans and the dust are compared. For
the Trojan asteroids, the peak in the longitude of pericenter distribution is
about 60 degrees larger than the longitude of pericenter of Jupiter; in
contrast, for Trojan dust this difference is smaller than 60 degrees, and it
decreases with decreasing grain size. For the Trojan asteroids and most of the
Trojan dust, the Tisserand parameter is distributed in the range of two to
three.
