Dynamics of charged dust in the orbit of Venus

Abstract

We study the dynamics of co-orbital dust in the inner solar system, i.e. the role of the solar radiation pressure, Poynting-Robertson effect, solar wind, and the interplanetary magnetic field on the location, width and stability of resonant motion of charged, and micron sized dust grains situated in the 1:1 mean motion resonance with planet Venus. We find deviations and asymmetry between $L_4$ and $L_5$ in locations of libration centers and libration width under the influence of non-gravitational effects via both analytical and numerical methods. The triangular Lagrangian points become unstable once we take into consideration solar radiation pressure, the Poynting-Robertson effect and solar wind drag. The Lorentz force could further destabilize the orbits, especially for small dust particles. We also make a comparison between the circular, elliptic restricted three-body model and a more complete model including all planets.

39 pages, 17 figures, to be published in A&A

References in corpus (6)

• The effect of Poynting-Robertson drag on the triangular Lagrangian points
• Evidence for dust accumulation just outside the orbit of Venus
• Co-orbital Asteroids as the Source of Venus's Zodiacal Dust Ring
• Charged dust grain dynamics subject to solar wind, Poynting-Robertson drag, and the interplanetary magnetic field
• A systematic survey of the dynamics of Uranus Trojans
• Charged dust close to outer mean-motion resonances in the heliosphere

Cited by in corpus (3)

• Tadpole type motion of charged dust in the Lagrange problem with planet Jupiter
• Secular Structure of 1:2 and 1:3 Resonances with Neptune
• Trojan asteroids and co-orbital dust ring of Venus