Population and Size Distribution of Small Jovian Trojan Asteroids

Jewitt, David; Trujillo, C. A.; Luu, Jane

doi:10.1086/301453

Cited by 173 publications

(233 citation statements)

References 20 publications

(18 reference statements)

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“…At the 2 km size limit (H ≈ 17.6 mag), Yoshida & Nakamura (2005) estimated about 4 times as many Trojans as Jewitt et al (2000) in a similar type of survey. However, apart from making the same type of size overestimation as Jewitt et al (2000), Yoshida & Nakamura (2005) also misplaced the L 4 point since the 60 • longitude of the Lagrangian point applies to the heliocentric system, while Yoshida & Nakamura (2005) used a geocentric system. The L 5 side was far less well examined than L 4 .…”

Section: Introductionmentioning

confidence: 82%

“…A completion limit of H ≈ 10.5 mag was used, based on the discovery statistics obtained between 1999 to 2001. In the search for Trans-Neptunian objects, Jewitt et al (2000) analyzed coincidental Trojan observations and deduced that there should be between 1700 and 5700 L 4 Trojans to H ≈ 13 mag. However, they observed an area between L 4 and L 3 , where the Trojan distribution is more stretched out than between L 4 and Jupiter.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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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Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

On the observational bias of the Trojan swarms

Karlsson¹

2010

A&A

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“…The number, N r , of such projectiles is unknown. If the size distribution of Neptune Trojans resembles that of Jupiter Trojans (Jewitt et al 2000), then N r $ 6000, which would imply…”

Section: Past Number: Collisional Attritionmentioning

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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“…In our solar system, the asteroid belt and Edgeworth-Kuiper belt are the two best known reservoirs of objects that remain from the planet formation process and range in size from hundreds of kilometers in diameter to meter-scale bodies (e.g. Jewitt et al 2000;Sheppard & Trujillo 2006). Such reservoirs are highly sculpted by the evolution of the planetary system in which they form (e.g.…”

Section: Introductionmentioning

confidence: 99%

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Lestrade

Matthews

Sibthorpe

et al. 2012

A&A

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Debris disks have been found primarily around intermediate and solar mass stars (spectral types A-K) but rarely around low mass M-type stars. We have spatially resolved a debris disk around the remarkable M3-type star GJ 581 hosting multiple planets using deep PACS images at 70, 100 and 160 μm as part of the DEBRIS Program on the Herschel Space Observatory. This is the second spatially resolved debris disk found around an M-type star, after the one surrounding the young star AU Mic (12 Myr). However, GJ 581 is much older (2-8 Gyr), and is X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images and found that the best fit model is for a disk extending radially from 25 ± 12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper belt but it surrounds a low mass star (0.3 M ) and its fractional dust luminosity L dust /L * of ∼10 −4 is much higher. The inclination limits of the disk found in our analysis make the masses of the planets small enough to ensure the long-term stability of the system according to some dynamical simulations. The disk is collisionally dominated down to submicron-sized grains and the dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. We suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars. Finally, the known planets, of low masses and orbiting within 0.3 AU from the star, cannot dynamically perturb the disk over the age of the star, suggesting that an additional planet exists at larger distance that is stirring the disk to replenish the dust.

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Population and Size Distribution of Small Jovian Trojan Asteroids

Cited by 173 publications

References 20 publications

On the observational bias of the Trojan swarms

On the observational bias of the Trojan swarms

Neptune Trojans as a Test Bed for Planet Formation

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

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