Physical characteristics of Comet Nucleus C/2001 OG108 (LONEOS)

Abell, P. A.; Fernández, Yanga; Pravec, Petr; French, Linda M.; Farnham, T. L.; Gaffey, M. J.; Hardersen, P. S.; Kušnirák, P.; Šarounová, L.; Sheppard, Scott S.

doi:10.1016/j.icarus.2005.06.012

Cited by 46 publications

(40 citation statements)

References 103 publications

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“…This paucity of deep absorption features is common among low-albedo asteroids and the few comet nuclei observed in this spectral region (e.g., Abell et al 2005;Campins et al 2003;Emery & Brown 2003;Licandro et al 2002Licandro et al , 2003Fernández et al 2004;Soderblom et al 2004). However, the overall shape of the spectrum can yield significant constraints on the surface composition.…”

Section: Analysis and Resultsmentioning

confidence: 94%

“…In Table 2 the value of S 0 for124P/Mrkos is from Licandro et al (2003). For comets 19P/Borrelly and C/2001 OG 108 , S 0 was estimated from plots in Soderblom et al (2004) and Abell et al (2005) (OG 108 ).…”

Section: Near-infrared Spectramentioning

confidence: 99%

“…Our averaged near-IR spectrum of 162P is plotted from 1 to 2 m in Figure 6, along with the near-IR spectra of comets 19P/ Borrelly, 124P/Mrkos, and LONEOS OG 108 (Soderblom et al 2004;Licandro et al 2003;Abell et al 2005). Each of these comet spectra is featureless within the noise, and they have slopes S 0 ¼ 7:7%; 3:0%; and 2:1% per 1000 8, respectively (Table 2).…”

Section: Comparison With Spectra Of Other Cometsmentioning

confidence: 99%

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Nuclear Spectra of Comet 162P/Siding Spring (2004 TU12)

et al. 2006

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We present visible and near-IR spectra of the nucleus of comet 162P/Siding Spring (also known as 2004 TU12) obtained in 2004 December, while it had no detectable coma. This is the third object observed to have intermittent cometary activity even when relatively close to the Sun. The spectra show no strong features in this wavelength range. This paucity of deep absorptions is common among low-albedo asteroids and the few comet nuclei observed in this spectral region. Marginal spectral structure is observed in the visible spectrum, and beyond 2 m the flux from the nucleus is dominated by thermal emission. We compare the spectrum of 162P with published spectra of other comet nuclei, primitive asteroids, and meteorites. Comet nuclei display a range of spectral shapes and slopes not unlike those observed among outer main-belt asteroids but closest to Trojan asteroids. No suitable spectral matches to comet 162P were found among primitive (chondritic) meteorites. We modeled our visible and near-IR spectra using the scattering theory described by Shkuratov et al. (1999), and our approach is similar to that used by Emery and Brown for modeling Trojan asteroids. Our best fits to the spectral shape and albedo include mixtures containing amorphous carbons, organics, and silicates. The absence of strong spectral features prevents the identification of specific minerals, and the resulting model compositions are not unique. The observations beyond 2 m are interpreted in a companion publication by Fernández and coworkers.

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Section: Analysis and Resultsmentioning

confidence: 94%

Section: Near-infrared Spectramentioning

confidence: 99%

Section: Comparison With Spectra Of Other Cometsmentioning

confidence: 99%

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Nuclear Spectra of Comet 162P/Siding Spring (2004 TU12)

et al. 2006

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“…Secondly, remote sensing indicates several compositional similarities between some asteroids and some comets, e.g. asteroids rich in water ice (Thomas et al, 2005;Marchis et al, 2006) and comets with albedos similar to D-type asteroids (Licandro et al, 2003;Abell et al, 2005). Observations indicate similar silicate mineralogy between Trojan asteroids and comet HaleBopp (Emery et al, 2006).…”

Section: Relationship Between Hydrated and Anhydrous Chondritic Idpsmentioning

confidence: 98%

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

Adnot

Engrand

Leshin

et al. 2009

Geochimica et Cosmochimica Acta

108

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. Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets. Geochimica et Cosmochimica Acta, Elsevier, 2009, 73, pp.4558-4575. 10 Abstract Oxygen isotopes were measured in four chondritic hydrated interplanetary dust particles (IDPs) and five chondritic anhydrous IDPs including two GEMS-rich particles (Glass embedded with metal and sulfides) by a combination of high precision and high lateral resolution ion microprobe techniques.All IDPs have isotopic compositions tightly clustered around that of solar system planetary materials. Hydrated IDPs have mass-fractionated oxygen isotopic compositions similar to those of CI and CM carbonaceous chondrites, consistent with hydration of initially anhydrous protosolar dust. Anhydrous IDPs have small 16 O excesses and depletions similar to those of carbonaceous chondrites, the largest 16 O variations being hosted by the two GEMS-rich IDPs. Coarse-grained forsteritic olivine and enstatite in anhydrous IDPs are isotopically similar to their counterparts in comet Wild 2 and in chondrules suggesting a high temperature inner solar system origin. The small variations in the 16 O content of GEMS-rich IDPs suggest that most GEMS either do not preserve a record of interstellar processes or the initial interstellar dust is not 16 O-rich as expected by self-shielding models, although a larger dataset is required to verify these conclusions.Together with other chemical and mineralogical indicators, O isotopes show that the parent-bodies of carbonaceous chondrites, of chondritic IDPs, of most Antarctic micrometeorites, and comet Wild 2 belong to a single family of objects of carbonaceous chondrite chemical affinity as distinct from ordinary, enstatite, K-and R-chondrites. Comparison with astronomical observations thus suggests a chemical continuum of objects including main belt and outer solar system asteroids such as C-type, P-type and D-type asteroids, Trojans and Centaurs as well as short-period comets and other Kuiper Belt Objects.

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“…The color distribution of these populations indicate that the fraction of C-type asteroids decreases with increasing a. The few properly observed cometary nuclei also have D-, or P-type spectra (Licandro et al 2002;Abell et al 2005;Campins et al 2006Campins et al , 2007. C-type asteroids are the dominant spectral type of asteroids in the 3 AU region.…”

Section: Introductionmentioning

confidence: 95%

(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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Physical characteristics of Comet Nucleus C/2001 OG108 (LONEOS)

Cited by 46 publications

References 103 publications

Nuclear Spectra of Comet 162P/Siding Spring (2004 TU12)

Nuclear Spectra of Comet 162P/Siding Spring (2004 TU12)

Oxygen isotopic composition of chondritic interplanetary dust particles: A genetic link between carbonaceous chondrites and comets

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

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