Transitional and temporary objects in the Jupiter Trojan area

Karlsson, O.

doi:10.1051/0004-6361:20031543

Cited by 24 publications

(28 citation statements)

References 20 publications

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“…9 Karlsson (2004) has identified $20 known asteroids that sometime within 1000 yr of the current epoch occupy horseshoe-like orbits with Jupiter. These objects transition often between resonant and nonresonant motion.…”

Section: Methods Of Computing F Colmentioning

confidence: 99%

Neptune Trojans as a Test Bed for Planet Formation

Chiang

Lithwick

2005

ApJ

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The problem of accretion in the Trojan 1:1 resonance is akin to the standard problem of planet formation, transplanted from a star-centered disk to a disk centered on the Lagrange point. The newly discovered class of Neptune Trojans promises to test theories of planet formation by coagulation. Neptune Trojans resembling the prototype 2001 QR 322 (''QR'')-whose radius of $100 km is comparable to that of the largest Jupiter Trojan-may outnumber their Jovian counterparts by a factor of $10. We develop and test three theories for the origin of large Neptune Trojans: pull-down capture, direct collisional emplacement, and in situ accretion. These theories are staged after Neptune's orbit anneals, that is, after dynamical friction eliminates any large orbital eccentricity and after the planet ceases to migrate. We discover that seeding the 1:1 resonance with debris from planetesimal collisions and having the seed particles accrete in situ naturally reproduces the inferred number of QR-sized Trojans. We analyze accretion in the Trojan subdisk by applying the two-groups method, accounting for kinematics specific to the resonance. We find that a Trojan subdisk comprising decimeter-sized seed particles and having a surface density $10 À3 times that of the local minimum-mass disk produces $10 QR-sized objects in $1 Gyr, in accord with observation. Further growth is halted by collisional diffusion of seed particles out of resonance. In our picture, the number and sizes of the largest Neptune Trojans represent the unadulterated outcome of dispersion-dominated, oligarchic accretion. Large Neptune Trojans, perhaps the most newly accreted objects in our solar system, may today have a dispersion in orbital inclination of less than $10 , despite the existence of niches of stability at higher inclinations. Such a vertically thin disk, born of a dynamically cold environment necessary for accretion and raised in minimal contact with external perturbations, contrasts with the thick disks of other minor body belts.

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Section: Methods Of Computing F Colmentioning

confidence: 99%

Neptune Trojans as a Test Bed for Planet Formation

Chiang

Lithwick

2005

ApJ

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“…The orbital elements used were not extracted from this page but form the orbit database at MPC. There was no removal of any orbits from this sample, although it contains e.g., short arc orbits, objects not observed recently and even possibly non-Trojans (Karlsson 2004). The temporarily designated Trojans were compared against all designations and possible numbering so as not to mismatch any objects.…”

Section: Known Trojansmentioning

confidence: 99%

“…There are five objects outside this limit in the true Trojan sample. (Karlsson 2004). However, the number of Trojans in horseshoe orbits compared to the tadpole population should be small because of the relatively short transition period.…”

Section: Fictitious Trojansmentioning

confidence: 99%

On the observational bias of the Trojan swarms

Karlsson¹

2010

A&A

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Aims. I investigate whether the Trojan swarms are observationally biased and place a completion limit on their absolute magnitude. Methods. Observations including Trojans from a number of observation sites are cross-checked with orbital integration of known Trojans and a set of fictitious Trojan orbits. Results. The completion limit for the Trojans swarms can be set to be H = 11.5 mag. The L 5 swarm is 71% of the L 4 size down to this limit. It is not likely that any existing set of orbital elements can have escaped detections. However, parts of the orbital element space, especially in the inclination, are biased for Trojans fainter than the completion limit. In the absolute magnitude interval 11.5−13 mag, 65% of new objects should have inclinations 15−40 • , while this inclination interval currently contains 49% of Trojans in the complete interval 9.5−11.5 mag. Trojans fainter than an absolute magnitude of 13 mag are also clearly biased in the ascending node at values coinciding with the Milky Way.

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“…The observations revealed a small non-gravitational acceleration of NEO 6489 Gulevka caused by anisotropic reemission of sunlight. Among the transient Trojans, 588 Achilles and 617 Patroclus were the first discovered at L4 and L5 back in 1906 (Karlsson 2004). They are now in the process of leaving.…”

Section: Asteroids Comets Both Neithermentioning

confidence: 99%