Properties of the Trans-Neptunian Belt: Statistics from the Canada-France-Hawaii Telescope Survey

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

doi:10.1086/321117

Cited by 200 publications

(223 citation statements)

References 42 publications

(81 reference statements)

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“…Inferred from Gomes (2004), only about 20% of objects (i.e., ∼0.2 M ⊕ ) may persist over the Solar System's age. Nevertheless, this estimated mass of the remnant belt is still a bit higher than the one we observed (Chiang & Brown 1999;Trujillo et al 2001;Gladman et al 2001). Unfortunately, considering the total systematic error in the integration, a complete exploration of a time evolution that is as long as the Solar System's age does not seem reliable for our code.…”

Section: Implication For the Kuiper Beltmentioning

confidence: 62%

Evolution of Jovian planets in a self-gravitating planetesimal disk

Zhou

Sun

2011

A&A

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Aims. We explore the orbital evolution of the four Jovian planets embedded in a self-gravitating planetesimal disk, along with the simultaneous accretion of small bodies by proto-Uranus and proto-Neptune. Methods. We adopt the code NBODY4 running on the GRAPE-type special-purpose computer for numerically simulating the primordial evolution of the outer Solar System, where the total gravitational forces due to the Sun, the four Jovian planets, and the massive planetesimals are all taken into account.Results. There is no significant accretion of proto-Uranus and proto-Neptune during their migration stage, only on the order of 0.1 Earth mass. The self-gravitating disk can provide a new replenishment of planetesimals outside a few AU beyond Neptune into the scattering zone, resulting in larger radial displacement of Neptune than in the non-self-gravitating disk. The present location of Neptune requires an original planetesimal disk outer edge at ∼35 AU. The distribution of the surviving planetesimals is very similar to the observed Kuiper belt.

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Section: Implication For the Kuiper Beltmentioning

confidence: 62%

Evolution of Jovian planets in a self-gravitating planetesimal disk

Zhou

Sun

2011

A&A

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“…Only the steepest part of the SPCs distribution reaches q ∼ 3. Analyses based on controlled samples designed for size analyses have found much steeper power-laws of from q = 3.0 (Trujillo et al 2001) to 3.5 (Kenyon & Bromley 2004), i.e. distributions much richer in small/faint objects.…”

Section: Absolute Magnitudementioning

confidence: 99%

Colours of minor bodies in the outer solar system

Hainaut

Boehnhardt

Protopapa

2012

A&A

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We present an update of the visible and near-infrared colour database of Minor Bodies in the Outer Solar System (MBOSSes), which now includes over 2000 measurement epochs of 555 objects, extracted from over 100 articles. The list is fairly complete as of December 2011. The database is now large enough to enable any dataset with a large dispersion to be safely identified and rejected from the analysis. The selection method used is quite insensitive to individual outliers. Most of the rejected datasets were observed during the early days of MBOSS photometry. The individual measurements are combined in a way that avoids possible rotational artifacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M(1, 1). The average colours, absolute magnitude, and spectral gradient are listed for each object, as well as the physico-dynamical classes using a classification adapted from Gladman and collaborators. Colour-colour diagrams, histograms, and various other plots are presented to illustrate and investigate class characteristics and trends with other parameters, whose significances are evaluated using standard statistical tests. Except for a small discrepancy for the J − H colour, the largest objects, with M(1, 1) < 5, are indistinguishable from the smaller ones. The larger ones are slightly bluer than the smaller ones in J − H. Short-period comets, Plutinos and other resonant objects, hot classical disk objects, scattered disk objects and detached disk objects have similar properties in the visible, while the cold classical disk objects and the Jupiter Trojans form two separate groups of their spectral properties in the visible wavelength range. The well-known colour bimodality of Centaurs is confirmed. The hot classical disk objects with large inclinations, or large orbital excitations are found to be bluer than the others, confirming a previously known result. Additionally, the hot classical disk objects with a smaller perihelion distance are bluer than those that do not come as close to the Sun. The bluer hot classical disk objects and resonant objects have fainter absolute magnitudes than the redder ones of the same class. Finally, we discuss possible scenarios for the origin of the colour diversity observed in MBOSSes, i.e. colouration caused by evolutionary or formation processes. The colour tables and all plots are also available on the MBOSS colour web page , which will be updated when new measurements are published

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“…Most of the observational studies of the TNOs are astrometric; a few studies of the luminosity distribution have also been done to constrain the formation and collisional evolution processes (Gladman et al 2001;Trujillo et al 2001). Some objects are bright enough (R ≤ 21) to achieve spectrophotometric and/or low resolution spectroscopic observations which give a better knowledge of their physical and chemical properties (Barucci et al 2000;Brown et al 2000;Davies et al 2000;Hainaut & Delsanti 2002;Jewitt & Luu 1998Trujillo & Brown 2002).…”

Section: Introductionmentioning

confidence: 99%

Photometry of the Kuiper-Belt object 1999 TD$_{\sf\sl 10}$ at different phase angles

Rousselot

Petit

Poulet

et al. 2003

A&A

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Abstract. We present photometric observations of the Kuiper-Belt object 1999 TD 10 at different phase angles and for three different broad band filters (B, V and R). This object was observed with the Danish 1.54-m telescope of ESO in Chile during six different observing nights corresponding to a phase angle of 0. 30, 0.37, 0.92, 3.43, 3.48 and 3.66 • . Extra observations were obtained in September 2002 with the VLT UT1/FORS1 combination to confirm that 1999 TD 10 does not exhibit any cometary activity, and in October 2001 with the Sierra Nevada Observatory 1.50-m telescope in order to add relative magnitudes to improve the determination of the rotation period. The observations are compatible with a single-peaked rotational lightcurve with a 7h41.5min ± 0.1 min period or a doublepeaked lightcurve with a 15h22.9min ± 0.1 min period. If a single-peaked rotational lightcurve is assumed the amplitude is 0.51 ± 0.03, 0.49 ± 0.05 and 0.60 ± 0.09 mag for the R, V and B bands, respectively. We present the phase curve obtained when assuming that the lightcurve is single-peaked. This phase curve reveals clearly an increase of about 0.3 mag and of similar importance for the three bands when phase angle decreases from 3.7 • to 0.3 • . The phase curve reveals a linear increase of the brightness with the decreasing phase angle and, consequently, does not permit a modeling of the opposition surge. Neverthless the poor repartition of the observational data does not permit a firm conclusion concerning the presence or absence of an opposition surge on the phase angle range covered by our data. Complementary observations are needed.

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Properties of the Trans-Neptunian Belt: Statistics from the Canada-France-Hawaii Telescope Survey

Cited by 200 publications

References 42 publications

Evolution of Jovian planets in a self-gravitating planetesimal disk

Evolution of Jovian planets in a self-gravitating planetesimal disk

Colours of minor bodies in the outer solar system

Photometry of the Kuiper-Belt object 1999 TD$_{\sf\sl 10}$ at different phase angles

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