Oppositions‐Ephemeride des Planeten (624) Hektor

Strömgren, Elis

doi:10.1002/asna.19081770808

Cited by 6 publications

(5 citation statements)

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“…The Jovian Trojans were discovered in the early 20th Century, with the first (588 Achilles, Wolf 1907) being quickly followed by 617 Patroclus, 624 Hektor, and 659 Nestor (Heinrich 1907;Strömgren 1908;Ebell 1909;Kopff 1909). These objects were the first confirmation of a stable solution to the restricted three-body problem that had been proposed over a century earlier by Lagrange (1772).…”

Section: Introductionmentioning

confidence: 96%

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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Section: Introductionmentioning

confidence: 96%

Stability of Jovian Trojans and their collisional families

Holt

Nesvorný

Horner

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The Jovian Trojans were discovered in the early 20th Century, with the first, (588 Achilles, Wolf 1907) being quickly followed by 617 Patroclus, 624 Hektor and 659 Nestor (Heinrich 1907;Strömgren 1908;Ebell 1909;Kopff 1909). These objects were the first confirmation of a stable solution to the restricted three-body problem that had been proposed over a century earlier by Lagrange (1772).…”

Section: Introductionmentioning

confidence: 96%

Stability of Jovian Trojans and their collisional families

Holt,

Nesvorny,

Horner

et al. 2020

Preprint

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The Jovian Trojans are two swarms of objects located around the L 4 and L 5 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 L 4 swarm, and two in the L 5 . 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 L 4 (23.35% escape) and L 5 (24.89% 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 onto orbits that resemble those of the Centaur and short-period comet populations. Within the Trojan collisional families, the 1996 RJ and 2001 UV 209 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% 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 × 10 9 years.

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“…The first Hilda asteroid to be discovered was that after which the family is named -(153) Hilda, which was found in 1875 November by Johann Palisa, 2 some 30 yr before the discovery of the first Jovian Trojans (e.g. Heinrich 1907;Wolf 1907;Strömgren 1908). Although the Hildas orbit markedly closer to the Sun than the Jovian Trojans, and their population is comparable to that of their more famous cousins, they remain relatively poorly studied.…”

Section: Introductionmentioning

confidence: 99%

A thermophysical and dynamical study of the Hildas, (1162) Larissa, and (1911) Schubart

Chavez

Müller

Marshall

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The Hilda asteroids are among the least studied populations in the asteroid belt, despite their potential importance as markers of Jupiter’s migration in the early Solar system. We present new mid-infrared observations of two notable Hildas, (1162) Larissa and (1911) Schubart, obtained using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST), and use these to characterise their thermal inertia and physical properties. For (1162) Larissa, we obtain an effective diameter of 46.5$^{+2.3}_{-1.7}$ km, an albedo of 0.12 ± 0.02, and a thermal inertia of 15$^{+10}_{-8}$ Jm−2s1/2K−1. In addition, our Larissa thermal measurements are well matched with an ellipsoidal shape with an axis ratio a/b=1.2 for the most-likely spin properties. Our modelling of (1911) Schubart is not as refined, but the thermal data point towards a high-obliquity spin-pole, with a best-fit a/b=1.3 ellipsoidal shape. This spin-shape solution is yielding a diameter of 72$^{+3}_{-4}$ km, an albedo of 0.039± 0.02, and a thermal inertia below 30 Jm−2s1/2K−1 (or 10$^{+20}_{-5}$ Jm−2s1/2K−1). As with (1162) Larissa, our results suggest that (1911) Schubart is aspherical, and likely elongated in shape. Detailed dynamical simulations of the two Hildas reveal that both exhibit strong dynamical stability, behaviour that suggests that they are primordial, rather than captured objects. The differences in their albedos, along with their divergent taxonomical classification, suggests that despite their common origin, the two have experienced markedly different histories.

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Oppositions‐Ephemeride des Planeten (624) Hektor

Cited by 6 publications

References 0 publications

Stability of Jovian Trojans and their collisional families

Stability of Jovian Trojans and their collisional families

Stability of Jovian Trojans and their collisional families

A thermophysical and dynamical study of the Hildas, (1162) Larissa, and (1911) Schubart

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