Defensive Programming

Wang, Wallace

doi:10.1007/978-1-4842-1233-2_21

Cited by 2 publications

(2 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Actually, a longer evolution time will lead to the same appearance as the Yarkovsky force acts like a cumulative effect. Wang & Hou (2017) proved that the libration amplitude of the semi-major axis in the 1:1 MMR undergoes remarkable variation when the Yarkovsky effect works. For prograde rotators, the amplitudes decrease with time while for retrograde rotators, the contrary is the case.…”

Section: Asymmetry Of the Stabilitymentioning

confidence: 98%

Orbital stability of Earth Trojans

Zhou

et al. 2019

A&A

View full text Add to dashboard Cite

The only discovery of Earth Trojan 2010 TK7 and the subsequent launch of OSIRIS-REx motive us to investigate the stability around the triangular Lagrange points L4 and L5 of the Earth. In this paper we present detailed dynamical maps on the (a0, i0) plane with the spectral number (SN) indicating the stability. Two main stability regions, separated by a chaotic region arising from the ν3 and ν4 secular resonances, are found at low (i0 ≤ 15 • ) and moderate (24 • ≤ i0 ≤ 37 • ) inclinations respectively. The most stable orbits reside below i0 = 10 • and they can survive the age of the Solar System. The nodal secular resonance ν13 could vary the inclinations from 0 • to ∼ 10 • according to their initial values while ν14 could pump up the inclinations to ∼ 20 • and upwards. The fine structures in the dynamical maps are related to higher-degree secular resonances, of which different types dominate different areas. The dynamical behaviour of the tadpole and horseshoe orbits, reflected in their secular precession, show great differences in the frequency space. The secular resonances involving the tadpole orbits are more sensitive to the frequency drift of the inner planets, thus the instabilities could sweep across the phase space, leading to the clearance of tadpole orbits. We are more likely to find terrestrial companions on horseshoe orbits. The Yarkovsky effect could destabilize Earth Trojans in varying degrees. We numerically obtain the formula describing the stabilities affected by the Yarkovsky effect and find the asymmetry between the prograde and retrograde rotating Earth Trojans. The existence of small primordial Earth Trojans that avoid being detected but survive the Yarkovsky effect for 4.5 Gyr is substantially ruled out.

show abstract

Section: Asymmetry Of the Stabilitymentioning

confidence: 98%

Orbital stability of Earth Trojans

Zhou

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…The shape, size and thermal properties of an asteroid determine the migration rate (e.g. Vokrouhlicky 1998;Brož 2006;Wang & Hou 2017), may change with time, and are linked with YORP spin changes. Despite these complexities, a common simplification for Yarkovsky-based studies of solar system asteroids is to assume that only their semimajor axes change.…”

Section: Link With Giant Branch Yarkovsky Forcesmentioning

confidence: 99%

Speeding past planets? Asteroids radiatively propelled by giant branch Yarkovsky effects

Veras

Higuchi

Ida

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Understanding the fate of planetary systems through white dwarfs which accrete debris crucially relies on tracing the orbital and physical properties of exo-asteroids during the giant branch phase of stellar evolution. Giant branch luminosities exceed the Sun's by over three orders of magnitude, leading to significantly enhanced Yarkovsky and YORP effects on minor planets. Here, we place bounds on Yarkovsky-induced differential migration between asteroids and planets during giant branch mass loss by modelling one exo-Neptune with inner and outer exo-Kuiper belts. In our bounding models, the asteroids move too quickly past the planet to be diverted from their eventual fate, which can range from: (i) populating the outer regions of systems out to 10 4 − 10 5 au, (ii) being engulfed within the host star, or (iii) experiencing Yarkovsky-induced orbital inclination flipping without any Yarkovsky-induced semimajor axis drift. In these violent limiting cases, temporary resonant trapping of asteroids with radii of under about 10 km by the planet is insignificant, and capture within the planet's Hill sphere requires fine-tuned dissipation. The wide variety of outcomes presented here demonstrates the need to employ sophisticated structure and radiative exo-asteroid models in future studies. Determining where metal-polluting asteroids reside around a white dwarf depends on understanding extreme Yarkovsky physics.

show abstract

Defensive Programming

Cited by 2 publications

References 0 publications

Orbital stability of Earth Trojans

Orbital stability of Earth Trojans

Speeding past planets? Asteroids radiatively propelled by giant branch Yarkovsky effects

Contact Info

Product

Resources

About