Size Distribution of Faint Jovian L4 Trojan Asteroids

Yoshida, Fumi; Nakamura, T.

doi:10.1086/497571

Cited by 75 publications

(103 citation statements)

References 21 publications

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“…with α ¼ 0:44 AE 0:05 and valid for 9 < H < 13:5, similar to the results found by Jewitt et al (2000) and Yoshida and Nakamura (2005). In this work we assume that there is no difference in the size distribution between the two swarms (which seems to be the case for H < 13:5; Szab´o et al 2007).…”

Section: The Jovian Trojanssupporting

confidence: 82%

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

Grav

Jedicke

Denneau

et al. 2011

Publications of the Astronomical Society of the Pacific

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ABSTRACT. We present here the Pan-STARRS Moving Object Processing System (MOPS) Synthetic Solar System Model (S3M), the first-ever attempt at building a comprehensive flux-limited model of the major small-body populations in the solar system. The goal of the S3M is to provide a valuable tool in the design and testing of the MOPS software, and will be used in the monitoring of the upcoming Pan-STARRS 1 all-sky survey, which started science operations during late spring of 2010. The model is composed of synthetic populations of near-Earth objects (NEOs with a subpopulation of Earth impactors), the main-belt asteroids (MBAs), Jovian Trojans, Centaurs, trans-Neptunian objects (classical, resonant, and scattered trans-Neptunian objects [TNOs]), Jupiter-family comets (JFCs), long-period comets (LPCs), and interstellar comets. The model reasonably reproduces the true populations to a minimum of V ¼ 24:5, corresponding to approximately the expected limiting magnitude for Pan-STARRS's ability to detect moving objects. The NEO synthetic population has been extended to H < 25 (corresponding to objects of about 50 m in diameter), allowing for close flybys of the Earth to be modeled.

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Section: The Jovian Trojanssupporting

confidence: 82%

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

Grav

Jedicke

Denneau

et al. 2011

Publications of the Astronomical Society of the Pacific

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“…1, along with the observational data derived by Jewitt et al (2000) and the fit proposed by these authors. Yoshida & Nakamura (2005), Szabó et al (2007), and Yoshida & Nakamura (2008) developed studies concerning the size distribution for small jovian Trojans, which are consistent with Jewitt et al (2000).…”

Section: Initial Populationssupporting

confidence: 60%

Studying the jovian Trojan dust

Elía

Brunini

2010

A&A

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Aims. We analyze the jovian Trojan dust in the L 4 swarm. Methods. To do this, we use a modification of the numerical code developed by us and previously applied to the collisional and dynamical evolution of the L 4 jovian Trojans. This algorithm considers catastrophic collisions and cratering events, includes a dynamical treatment that takes the stability and instability zones of the L 4 jovian swarm into account, and incorporates the effects of the Poynting-Robertson radiation.Results. From this analysis, we infer that the time evolution of the L 4 jovian Trojan dust luminosity has the characteristics of a diffusion process, since its current value is fairly insensitive to variations in the initial size distribution. Moreover, our results indicate that the current luminosity of the dust in the L 4 jovian swarm ranges from ∼3.2 × 10 −8 to 3.4 × 10 −8 L . Conclusions. From these estimates, we conclude that the current luminosity of the dust in the L 4 jovian swarm is comparable to the luminosity of the inner Solar System dust, and, at least, one order of magnitude lower than the luminosity of the outer Solar System dust.

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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: 84%

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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Size Distribution of Faint Jovian L4 Trojan Asteroids

Cited by 75 publications

References 21 publications

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

Studying the jovian Trojan dust

On the observational bias of the Trojan swarms

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