Influence of the Yarkovsky force on Jupiter Trojan asteroids

Hellmich, S.; Mottola, S.; Hahn, Gerhard; Kührt, Ekkehard; Niem, D. de

doi:10.1051/0004-6361/201834715

Cited by 16 publications

(14 citation statements)

References 42 publications

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“…We first note that the formation of the three small body populations, the MBAs, JTAs, and TNOs have been greatly shaped by the early solar system history (see Nesvorný 2018, for a review) and since then they have been evolving under a quiescent environment for 4 Gyr. As a consequence, the dynamical (Minton & Malhotra 2010;Di Sisto et al 2014;Muñoz-Gutiérrez et al 2019) and collisional (Bottke et al 2005;Hellmich et al 2019;Durda & Stern 2000) erosion over the next several Gyr before the Sun reaches the giant brach will be mild and the majority of mass contained (in large objects) within the three populations will not be affected.…”

Section: Discussionmentioning

confidence: 99%

Metal pollution of the solar white dwarf by solar system small bodies

Li,

Mustill,

Davies

2021

Preprint

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White dwarfs (WDs) often show metal lines in their spectra, indicating accretion of asteroidal material. Our Sun is to become a WD in several Gyr. Here, we examine how the solar WD accretes from the three major small body populations: the main belt asteroids (MBAs), Jovian trojan asteroids (JTAs), and trans-Neptunian objects (TNOs). Owing to the solar mass loss during the giant branch, 40% of the JTAs are lost but the vast majority of MBAs and TNOs survive. During the WD phase, objects from all three populations are sporadically scattered onto the WD, implying ongoing accretion. For young cooling ages 100 Myr, accretion of MBAs predominates; our predicted accretion rate ∼ 10 6 g/s falls short of observations by two orders of magnitude. On Gyr timescales, thanks to the consumption of the TNOs that kicks in 100 Myr, the rate oscillates around 10 6 − 10 7 g/s until several Gyr and drops to ∼ 10 5 g/s at 10 Gyr. Our solar WD accretion rate from 1 Gyr and beyond agrees well with those of the extrasolar WDs. We show that for the solar WD, the accretion source region evolves in an inside-out pattern. Moreover, in a realistic small body population with individual sizes covering a wide range as WD pollutants, the accretion is dictated by the largest objects. As a consequence, the accretion rate is lower by an order of magnitude than that from a population of bodies of a uniform size and the same total mass and shows greater scatter.

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Section: Discussionmentioning

confidence: 99%

Metal pollution of the solar white dwarf by solar system small bodies

Li,

Mustill,

Davies

2021

Preprint

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“…This thrust will gradually change the semimajor axis of a body, with the scale and direction of the induced drift dependent on the thermal properties, axis of rotation and size of the object (Brož et al 2005;Bottke et al 2006). In the case of the Jovian Trojans, simulations of hypothetical objects have indicated that at small sizes (<1 km), the Yarkovsky effect could impact the stability of the objects (Wang & Hou 2017;Hellmich et al 2019). As we are simulating known Jovian Trojans, the majority of the objects are greater than several kilometres in size (Emery et al 2015), and have unknown or highly uncertain thermal properties (Slyusarev & Belskaya 2014;Sharkey et al 2019).…”

Section: E T H O D Smentioning

confidence: 99%

Stability of Jovian Trojans and their collisional families

Holt

Nesvorný

Horner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Jovian Trojans are two swarms of objects located around the L4 and L5 Lagrange points. The population is thought to have been captured by Jupiter during the Solar system’s youth. Within the swarms, six collisional families have been identified in previous work, with four in the L4 swarm, and two in the L5. Our aim is to investigate the stability of the two Trojan swarms, with a particular focus on these collisional families. We find that the members of Trojan swarms escape the population at a linear rate, with the primordial L4 (23.35 per cent escape) and L5 (24.89 per cent escape) population sizes likely 1.31 and 1.35 times larger than today. Given that the escape rates were approximately equal between the two Trojan swarms, our results do not explain the observed asymmetry between the two groups, suggesting that the numerical differences are primordial in nature, supporting previous studies. Upon leaving the Trojan population, the escaped objects move on to orbits that resemble those of the Centaur and short-period comet populations. Within the Trojan collisional families, the 1996 RJ and 2001 UV209 families are found to be dynamically stable over the lifetime of the Solar system, whilst the Hektor, Arkesilos and Ennomos families exhibit various degrees of instability. The larger Eurybates family shows 18.81 per cent of simulated members escaping the Trojan population. Unlike the L4 swarm, the escape rate from the Eurybates family is found to increase as a function of time, allowing an age estimation of approximately 1.045 ± 0.364 × 109 yr.

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“…This is due to the dependence of the Yarkovsky effect on the Solar flux. At the 5.2au mean semi-major axis of the Jovian Trojans, the mean Yarkovsky effect is minimal, particularly for Trojans over 1km in diameter (Wang & Hou 2017;Hellmich et al 2019).…”

Section: Clustering Methodsmentioning

confidence: 96%

Astrocladistics of the Jovian Trojan Swarms

Holt,

Horner,

Nesvorný

et al. 2021

Preprint

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The Jovian Trojans are two swarms of small objects that share Jupiter's orbit, clustered around the leading and trailing Lagrange points, L 4 and L 5 . In this work, we investigate the Jovian Trojan population using the technique of astrocladistics, an adaptation of the 'tree of life' approach used in biology. We combine colour data from WISE, SDSS, Gaia DR2 and MOVIS surveys with knowledge of the physical and orbital characteristics of the Trojans, to generate a classification tree composed of clans with distinctive characteristics. We identify 48 clans, indicating groups of objects that possibly share a common origin. Amongst these are several that contain members of the known collisional families, though our work identifies subtleties in that classification that bear future investigation. Our clans are often broken into subclans, and most can be grouped into 10 superclans, reflecting the hierarchical nature of the population. Outcomes from this project include the identification of several high priority objects for additional observations and as well as providing context for the objects to be visited by the forthcoming Lucy mission. Our results demonstrate the ability of astrocladistics to classify multiple large and heterogeneous composite survey datasets into groupings useful for studies of the origins and evolution of our Solar system.

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Influence of the Yarkovsky force on Jupiter Trojan asteroids

Cited by 16 publications

References 42 publications

Metal pollution of the solar white dwarf by solar system small bodies

Metal pollution of the solar white dwarf by solar system small bodies

Stability of Jovian Trojans and their collisional families

Astrocladistics of the Jovian Trojan Swarms

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