The Trojan Color Conundrum

Jewitt, David

doi:10.3847/1538-3881/aaa1a4

Cited by 39 publications

(56 citation statements)

References 47 publications

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“…Neptune Trojans are bodies from Neptune's core feeding zone at about 24 au, but also scattered bodies from the formation locations of the other planets (17-25 au). This is consistent with new results about the colour of the Jupiter Trojans being indistinguishable from the Neptune Trojans, but statistically different from the hot KBOs (Jewitt 2018). The Hilda asteroids, instead, are trapped from a region between 5-8 au.…”

Section: Discussionsupporting

confidence: 91%

Consequences of planetary migration on the minor bodies of the early solar system

Pirani

Johansen

Bitsch

et al. 2019

A&A

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Pebble accretion is an efficient mechanism that is able to build up the core of the giant planets within the lifetime of the protoplanetary disc gas-phase. The core grows via this process until the protoplanet reaches its pebble isolation mass and starts to accrete gas. During the growth, the protoplanet undergoes a rapid, large-scale, inward migration due to the interactions with the gaseous protoplanetary disc. In this work, we have investigated how this early migration would have affected the minor body populations in our solar system. In particular, we focus on the Jupiter Trojan asteroids (bodies in the coorbital resonance 1:1 with Jupiter, librating around the L 4 and L 5 Lagrangian points called, respectively, the leading and the trailing swarm) and the Hilda asteroids. We characterised their orbital parameter distributions after the disc dispersal and their formation location and compare them to the same populations produced in a classical in situ growth model. We find that a massive and eccentric Hilda group is captured during the migration from a region between 5 and 8 au and subsequently depleted during the late instability of the giant planets. Our simulations also show that inward migration of the giant planets always produces a Jupiter Trojans' leading swarm more populated than the trailing one, with a ratio comparable to the current observed Trojan asymmetry ratio. The in situ formation of Jupiter, on the other hand, produces symmetric swarms. The reason for the asymmetry is the relative drift between the migrating planet and the particles in the coorbital resonance. The capture happens during the growth of Jupiter's core and Trojan asteroids are afterwards carried along during the giant planet's migration to their final orbits. The asymmetry and eccentricity of the captured Trojans correspond well to observations, but their inclinations are near zero and their total mass is three to four orders of magnitude higher than the current population. Future modelling will be needed to understand whether the dynamical evolution of the Trojans over billions of years will raise the inclinations and deplete the masses to observed values.

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Section: Discussionsupporting

confidence: 91%

Consequences of planetary migration on the minor bodies of the early solar system

Pirani

Johansen

Bitsch

et al. 2019

A&A

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“…Upon discovery, Chiron was thought to be an asteroid, but it has since exhibited outbursting behaviour and is co-designated as comet 95P/Chiron (e.g. Luu & Jewitt 1990, Hartmann et al 1990, Meech & Belton 1990, Jewitt 2009, Bauer et al 2004). Chiron's brightness varies over both short (hour) and long (decade) timescales, and is remarkably uncorrelated with heliocentric distance (e.g.…”

Section: Introductionmentioning

confidence: 99%

Characterization of material around the centaur (2060) Chiron from a visible and near-infrared stellar occultation in 2011

Sickafoose

Bosh

Emery

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The centaur (2060) Chiron exhibits outgassing behaviour and possibly hosts a ring system. On 2011 November 29, Chiron occulted a fairly bright star (R~15 mag) as observed from the 3m NASA Infrared Telescope Facility (IRTF) on Mauna Kea and the 2-m Faulkes Telescope North (FTN) at Haleakala. Data were taken as visible wavelength images and simultaneous, low-resolution, near-infrared (NIR) spectra. Here, we present a detailed examination of the light-curve features in the optical data and an analysis of the NIR spectra. We place a lower limit on the spherical diameter of Chiron's nucleus of 160.2±1.3 km. Sharp, narrow dips were observed between 280-360 km from the centre (depending on event geometry). For a central chord and assumed ring plane, the separated features are 298.5-302 and 308-310.5 km from the nucleus, with normal optical depth ~0.5-0.9, and a gap of 9.1±1.3 km. These features are similar in equivalent depth to Chariklo's inner ring. The absence of absorbing/scattering material near the nucleus suggests that these sharp dips are more likely to be planar rings than a shell of material. The region of relatively-increased transmission is within the 1:2 spin-orbit resonance, consistent with the proposed clearing pattern for a non-axisymmetric nucleus. Characteristics of possible azimuthally incomplete features are presented, which could be transient, as well as a possible shell from ~900-1500 km: future observations are needed for confirmation. There are no significant features in the NIR light curves, nor any correlation between optical features and NIR spectral slope.

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“…Jupiter's co-orbital region is known to host the Trojan asteroids that were captured mostly permanently by the planet during the late stage of Solar System formation (Tsiganis et al 2005;Robutel & Gabern 2006;Nesvorný et al 2013;Jewitt 2018). Asteroid 2015 BZ509 shares the co-orbital region with the Trojans ⋆ E-mail: namouni@obs-nice.fr (FN) ; helena.morais@rc.unesp.br (MHMM) but moves in the opposite orbital direction.…”

Section: Introductionmentioning

confidence: 99%

An interstellar origin for Jupiter’s retrograde co-orbital asteroid

Namouni

Morais

2018

Monthly Notices of the Royal Astronomical Society: Letters

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Asteroid (514107) 2015 BZ509 was discovered recently in Jupiter's co-orbital region with a retrograde motion around the Sun. The known chaotic dynamics of the outer Solar System have so far precluded the identification of its origin. Here, we perform a high-resolution statistical search for stable orbits and show that asteroid (514107) 2015 BZ509 has been in its current orbital state since the formation of the Solar System. This result indicates that (514107) 2015 BZ509 was captured from the interstellar medium 4.5 billion years in the past as planet formation models cannot produce such a primordial large-inclination orbit with the planets on nearly-coplanar orbits interacting with a coplanar debris disk that must produce the low-inclination small-body reservoirs of the Solar System such as the asteroid and Kuiper belts. This result also implies that more extrasolar asteroids are currently present in the Solar System on nearly-polar orbits.

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The Trojan Color Conundrum

Cited by 39 publications

References 47 publications

Consequences of planetary migration on the minor bodies of the early solar system

Consequences of planetary migration on the minor bodies of the early solar system

Characterization of material around the centaur (2060) Chiron from a visible and near-infrared stellar occultation in 2011

An interstellar origin for Jupiter’s retrograde co-orbital asteroid

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