On the existence of a comet belt beyond Neptune

Fernández, Julio A.

doi:10.1093/mnras/192.3.481

Cited by 298 publications

(151 citation statements)

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“…Fernández (1980) argued that an origin in a flattened disklike region beyond Neptune was more probable, and the first member of this Kuiper belt was discovered in 1992 (Jewitt & Luu 1993). Now, the nuclei of JFCs are widely considered to be fragments produced collisionally in the Kuiper belt (Farinella & Davis 1996).…”

Section: Shapes Of Cometary Nucleimentioning

confidence: 99%

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

Jewitt¹,

Sheppard²,

Fernández³

2003

Astron J

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We add 143P/Kowal-Mrkos to the small but growing sample of well-observed cometary nuclei. Photometric observations from 3.4 to 4.0 AU heliocentric distance reveal a pointlike object with no detectable outgassing. Periodic modulation of the scattered light (Dm R = 0.45 AE 0.05) is attributed to rotation of the bare nucleus with a double-peaked period 17.21 AE 0.10 hr and a projected ratio of the shortest to longest axis of about 0.67/1. We also measured the phase coefficient (0.043 AE 0.014 mag deg À1 ), the BVRI colors (VÀR = 0.58 AE 0.02), and the absolute red magnitude [m R (1, 1, 0) = 13.49 AE 0.20]. The effective circular radius is 5.7 AE 0.6 km (geometric albedo 0.04 assumed). We study the properties of 11 well-observed Jupiterfamily comet (JFC) nuclei. On average, the nuclei are systematically more elongated (average photometric range Dm R = 0.54 AE 0.07) than main-belt asteroids of comparable size (Dm R = 0.32 AE 0.05) and more elongated than fragments produced in laboratory impact experiments. We attribute the elongation of the nuclei to an evolutionary effect, most likely driven by sublimation-induced mass loss. However, we find no evidence for any relation between the nucleus shape and the sublimation timescale. This may be because the timescale for evolution of the nucleus shape is very short compared with the dynamical timescale for the JFCs, meaning that most nuclei in our sample are already highly physically evolved.

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Section: Shapes Of Cometary Nucleimentioning

confidence: 99%

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

Jewitt¹,

Sheppard²,

Fernández³

2003

Astron J

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“…Presently, ∼1600 KBOs have been identified and classified into several dynamical families (see Appendix A and Gladman et al 2008, for a review). Kuiper belt objects, which dynamically evolve to become Jupiter family comets (JFCs), form a transient population, the Centaurs, with short-lived chaotic orbits between Jupiter and Neptune (Kowal et al 1977;Fernandez 1980;Levison & Duncan 1997).…”

Section: Introductionmentioning

confidence: 99%

The bimodal colors of Centaurs and small Kuiper belt objects

Peixinho

Delsanti

Guilbert-Lepoutre³

et al. 2012

A&A

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Ever since the very first photometric studies of Centaurs and Kuiper belt objects (KBOs) their visible color distribution has been controversial. This controversy has triggered to a prolific debate on the origin of the surface colors of these distant icy objects of the solar system. Two scenarios have been proposed to interpret and explain the large variability of colors, hence surface composition. Are the colors mainly primordial and directly related to the formation region, or are they the result of surface evolution processes? To date, no mechanism has been found that successfully explains why Centaurs, which are escapees from the Kuiper belt, exhibit two distinct color groups, whereas KBOs do not. We readdress this issue using a carefully compiled set of B − R colors and H R (α) magnitudes (as proxy for size) for 253 objects, including data for 10 new small objects. We find that the bimodal color distribution of Centaurs is a size-related phenomenon, common to both Centaurs and small KBOs, i.e. independent of dynamical classification. Furthermore, we find that large KBOs also have a bimodal distribution of surface colors, albeit distinct from the small objects and strongly dependent on the "Haumea collisional family" objects. When plotted in B − R, H R (α) space, the colors of Centaurs and KBOs display a peculiar N shape.

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“…The study of the physical properties of these asteroid populations provide tests of dynamical models. In particular it is very important to compare them with that of Jupiter family comets, as the latter are small TNOs scattered to the inner planetary region (Fernández 1980). At visible wavelengths, Trojan, Hilda and Cybele asteroids are classified primarily as D-and P-type asteroids, with a small fraction of C-type.…”

Section: Introductionmentioning

confidence: 99%

(65) Cybele: detection of small silicate grains, water-ice, and organics

Licandro

Campins

Kelley

et al. 2010

A&A

111

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Context. (65) Cybele is the most representative member of a population of primitive asteroids in the outer edge of the main belt, the Cybele asteroids. Recent dynamical models suggest that a significant fraction of them originated in the primordial transneptunian disk, so the study of the physical properties of these asteroids is potentially a useful test of these models. Aims. Our aim is to obtain information on the surface composition of this asteroid. In particular we want to obtain information on the composition and properties of the regolith and the possible presence of ices and organic materials. Methods. We present 2-4 μm and 5-14 μm spectroscopy of (65) Cybele obtained with the NASA IRTF telescope and Spitzer Space Telescope respectively. We compare the results with spectra of Trojan asteroids and asteroid (24) Themis. We analyze the 2-4 μm spectrum using scattering models and we apply thermal models to the 5-14 μm data. Results. The 2-4 μm spectrum of (65) Cybele presents an absorption band centered at ∼3.1 μm and more weaker bands in the 3.2-3.6 μm region, very similar to those observed in (24) Themis. No hydrated silicates are detected. From the spectrum in the 5-14 μm region an effective diameter D = 290 ± 5 km, a beaming paramete η = 0.967 ± 0.014, and a geometric visible albedo p V = 0.05 ± 0.01 are derived using the NEATM thermal model. The emisivity spectrum in the 5-14 μm range exhibits an emission plateau at about 9 to 12 μm with an spectral contrast of ∼5%. This emission is similar to that of Trojan asteroids and active comets and may be due to small silicate grains being imbedded in a relatively transparent matrix, or to a very under-dense (fairy-castle) surface structure. The lower amplitude of the silicate emission in Cybele's spectrum with respect to that of Trojan asteroids could be attributed to larger dust particles and/or a slightly denser structure. Conclusions. The surface of (65) Cybele is covered by a fine anhydrous silicate grains mantle, with a small amount of water ice and complex organic solids. This is similar to comet surface where non-equilibrium phases coexist. The presence of water-ice and anhydrous silicates is indicative that hydration did not happened or is incomplete, suggesting that the temperatures were always sufficiently low.

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On the existence of a comet belt beyond Neptune

Cited by 298 publications

References 0 publications

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

143P/Kowal-Mrkos and the Shapes of Cometary Nuclei

The bimodal colors of Centaurs and small Kuiper belt objects

(65) Cybele: detection of small silicate grains, water-ice, and organics

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