On the dynamical evolution of 2002 VE68

Abstract: Minor planet 2002 VE68 was identified as a quasi-satellite of Venus shortly after its discovery. At that time its data-arc span was only 24 days, now it is 2,947 days. Here we revisit the topic of the dynamical status of this remarkable object as well as look into its dynamical past and explore its future orbital evolution which is driven by close encounters with both the Earth-Moon system and Mercury. In our calculations we use a Hermite integration scheme, the most updated ephemerides and include the perturbations by the eight major planets, the Moon and the three largest asteroids. We confirm that 2002 VE68 currently is a quasi-satellite of Venus and it has remained as such for at least 7,000 yr after a close fly-by with the Earth. Prior to that encounter the object may have already been co-orbital with Venus or moving in a classical, non-resonant Near-Earth Object (NEO) orbit. The object drifted into the quasi-satellite phase from an L4 Trojan state. We also confirm that, at aphelion, dangerously close encounters with the Earth (under 0.002 AU, well inside the Hill sphere) are possible. We find that 2002 VE68 will remain as a quasi-satellite of Venus for about 500 yr more and its dynamical evolution is controlled not only by the Earth, with a non-negligible contribution from the Moon, but by Mercury as well. 2002 VE68 exhibits resonant (or near resonant) behavior with Mercury, Venus and the Earth. Our calculations indicate that an actual collision with the Earth during the next 10,000 yr is highly unlikely but encounters as close as 0.04 AU occur with a periodicity of 8 years.

• The paper confirms that 2002 VE68 is a quasi-satellite of Venus, maintaining this state for over 7,000 years as shown by numerical integrations.
• It demonstrates that the asteroid transitions from an L₄ Trojan state to various co-orbital configurations, evidencing complex gravitational interactions.
• The study quantifies resonant behavior, noting near 8:13 resonance with Earth and low collision probability over the next 10,000 years.

On the Dynamical Evolution of 2002 VE68

The paper "On the dynamical evolution of 2002 VE$_{68}$" by C. de la Fuente Marcos and R. de la Fuente Marcos provides a detailed analysis of the dynamical behavior of the minor planet 2002 VE$_{68}$, identified as a quasi-satellite of Venus. This object exhibits a unique orbital configuration within the inner solar system, making it an intriguing subject for dynamical studies.

Summary of Findings

1. Quasi-Satellite Nature: The research confirms that 2002 VE$_{68}$ is a quasi-satellite of Venus, a status it has maintained for at least 7,000 years. This identification is supported by numerical integrations that show the asteroids' mean longitude librating around that of Venus. This quasi-satellite state will persist for approximately another 500 years before transitioning.
2. Orbital Transition: Prior to its current quasi-satellite state, 2002 VE$_{68}$ transitioned from an L$_4$ Trojan state, highlighting the dynamic nature of its orbit. Post-quasi-satellite phase, it is expected to transition through various co-orbital configurations including Trojan and horseshoe states.
3. Close Encounters and Influences: The asteroid undergoes close encounters with both the Earth-Moon system and Mercury. The Earth exerts the most significant influence on 2002 VE$_{68}$'s orbital evolution, capable of bringing the asteroid within 0.002 AU, which is under Earth's Hill sphere. The Moon is noted to have a non-negligible influence in these dynamics.
4. Resonant Behavior: The minor planet exhibits resonant or near-resonant behavior with Mercury, Venus, and Earth. Particularly significant is a near 8:13 resonance with Earth, causing periodic close approaches every eight years. These resonances indicate a complex interplay of gravitational influences shaping the object's trajectory.
5. Collision Probability: The probability of a collision with Earth within the next 10,000 years remains low. The analysis predicts periodic close approaches with Earth, the closest within the next 100 years being at 0.02482 AU.

Theoretical and Practical Implications

• Planetary Co-orbital Dynamics: The study enhances the understanding of co-orbital dynamics, particularly for quasi-satellites in chaotic resonance states influenced by multiple planets. It also suggests potential scenarios for quasi-satellite capture and ejection driven by perturbative interactions.
• Asteroid Hazard Assessment: By affirming the low collision risk with Earth, the research contributes to ongoing assessments of near-Earth objects (NEOs) and planetary defense strategies.
• Future Research Directions: The findings lay a foundation for future investigations into similar co-orbital bodies and resonant dynamics within other planetary systems. They also encourage the exploration of the roles of smaller bodies, such as the Moon and major asteroids, in altering the orbits of quasi-satellites.

Overall, the study of 2002 VE$_{68}$ offers insight into the complex dynamics of quasi-satellites and their interactions in a multi-body celestial environment. It underscores the intricate influences of gravitational forces shaping the behaviors of minor planets in the solar system. As computational models and observational technologies advance, such research can expand to include more comprehensive scenarios and refined data, further enhancing our understanding of the dynamical processes governing these fascinating objects.