English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In a previous paper we simulated the orbital evolution of dust particles fromthe Jupiter Trojan asteroids ejected by the impacts of interplanetaryparticles, and evaluated their overall configuration in the form of dust arcs.Here we compare the orbital properties of these Trojan dust particles and theTrojan asteroids. Both Trojan asteroids and most of the dust particles aretrapped in the Jupiter 1:1 resonance. However, for dust particles, thisresonance is modified because of the presence of solar radiation pressure,which reduces the peak value of the semi-major axis distribution. We find alsothat some particles can be trapped in the Saturn 1:1 resonance and higher orderresonances with Jupiter. The distributions of the eccentricity, the longitudeof pericenter, and the inclination for Trojans and the dust are compared. Forthe Trojan asteroids, the peak in the longitude of pericenter distribution isabout 60 degrees larger than the longitude of pericenter of Jupiter; incontrast, for Trojan dust this difference is smaller than 60 degrees, and itdecreases with decreasing grain size. For the Trojan asteroids and most of theTrojan dust, the Tisserand parameter is distributed in the range of two tothree.

Comparison of the orbital properties of Jupiter Trojan asteroids and Trojan dust