Solid CN bearing material on outer solar system bodies

Cruikshank, D. P.; Allamandola, Louis J.; Hartmann, W. K.; Tholen, David J.; Brown, R. H.; Matthews, Clifford N.; Bell, J. F.

doi:10.1016/0019-1035(91)90233-j

Cited by 109 publications

(60 citation statements)

References 37 publications

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“…If we assume that the red visible color and the blue infrared color are both due to a single absorbing component, we derive an absorption spectrum reminiscent of the visible red, infrared blue tholins such as those created in gas-phase experiments intended to reproduce Titan hazes (Cruikshank et al 1991). We cannot match the spectrum, however, by simply assuming that the nonmethane component is tholin, as having only 20% of the surface with a tholin-like spectrum cannot provide a sufficiently red optical spectrum.…”

Section: Low-resolution Spectroscopymentioning

confidence: 99%

“…Unfortunately, a few different tholins have had optical constants measured, including those that appear to be the best match to the red optical, blue infrared component on 2005 FY9. We therefore artificially construct optical constants to match the bihemispheric reflectance spectrum of the gas-phase tholins shown in Cruikshank et al (1991). While such artificially constructed optical constants are clearly insufficient for detailed modeling, they are used here to represent the general class of visible red, infrared blue tholins.…”

Section: High-resolution Spectroscopymentioning

confidence: 99%

“…The spectral mixture is constructed from a modeled surface with 70% by weight 1 cm methane grains, 20% 100 m ethane grains, and the remainder an artificial approximation of the optical properties of a tholin. We construct the artificial approximation to the tholin component by estimating the single-scattering albedo of tholin from the bihemispheric reflectance spectrum of the gas-phase tholins shown in Cruikshank et al (1991) by equations (8.25) and (10.23) of Hapke and assuming an arbitrary grain size. The derived optical properties are likely a poor representation of the true optical properties of this or any other tholin, but they spectrally represent the important visible red, infrared blue colors of the spectrum that are typical of many laboratory spectra of tholins.…”

Section: Appendix Spectral Modelsmentioning

confidence: 99%

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Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

et al. 2006

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The spectrum of the bright Kuiper Belt object 2005 FY9 from 0.34 to 2.5 m is dominated by the red coloring of many outer solar system objects in the optical wavelength regime and by absorption due to methane in the near-infrared. The solid methane absorption lines are significantly broader on 2005 FY9 than on any other solar system body, indicating long optical path lengths through the methane. These long path lengths can be parameterized as a methane grain size of approximately 1 cm in a Hapke reflectance model. In addition to large-grained methane, the infrared spectrum also indicates the clear presence of ethane, an expected product of UV photolysis of methane. No evidence for N 2 or CO, both known to be present on Pluto, is found. We suggest that the large differences between the spectrum of 2005 FY9 and that of Pluto and 2003 UB313 is due to a depletion of nitrogen on the surface of 2005 FY9 that leads to large methane grains, abundant sites for ethane formation through UV photolysis, and highly irradiated tholin-like material.

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Section: Low-resolution Spectroscopymentioning

confidence: 99%

Section: High-resolution Spectroscopymentioning

confidence: 99%

Section: Appendix Spectral Modelsmentioning

confidence: 99%

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Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

et al. 2006

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“…The properties of the residues from the UV-and e − -irradiated ices are also compared to samples of poly-HCN provided by Bob Minard (Minard et al 1998) and later analyzed by Hiroshi Imanaka (Imanaka & Smith 2010). Poly-HCN has been suggested as a possible component of the refractory carbonaceous material found on comets and on the surfaces of objects in the outer Solar System (e.g., Cruikshank et al 1991;Matthews 1992) and has been previously compared to Titan-like tholins produced in the laboratory (Vuitton et al 2010). …”

Section: Introductionmentioning

confidence: 99%

ICE CHEMISTRY ON OUTER SOLAR SYSTEM BODIES: ELECTRON RADIOLYSIS OF N₂-, CH₄-, AND CO-CONTAINING ICES

Materese

Cruikshank

Sandford

et al. 2015

ApJ

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Radiation processing of the surface ices of outer Solar System bodies may be an important process for the production of complex chemical species. The refractory materials resulting from radiation processing of known ices are thought to impart to them a red or brown color, as perceived in the visible spectral region. In this work, we analyzed the refractory materials produced from the 1.2-keV electron bombardment of low-temperature N 2 -, CH 4 -, and CO-containing ices (100:1:1), which simulates the radiation from the secondary electrons produced by cosmic ray bombardment of the surface ices of Pluto. Despite starting with extremely simple ices dominated by N 2 , electron irradiation processing results in the production of refractory material with complex oxygen-and nitrogenbearing organic molecules. These refractory materials were studied at room temperature using multiple analytical techniques including Fourier-transform infrared spectroscopy, X-ray absorption near-edge structure (XANES) spectroscopy, and gas chromatography coupled with mass spectrometry (GC-MS). Infrared spectra of the refractory material suggest the presence of alcohols, carboxylic acids, ketones, aldehydes, amines, and nitriles. XANES spectra of the material indicate the presence of carboxyl groups, amides, urea, and nitriles, and are thus consistent with the IR data. Atomic abundance ratios for the bulk composition of these residues from XANES analysis show that the organic residues are extremely N-rich, having ratios of N/C ∼ 0.9 and O/C ∼ 0.2. Finally, GC-MS data reveal that the residues contain urea as well as numerous carboxylic acids, some of which are of interest for prebiotic and biological chemistries.

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“…Fitzsimmons et al (1990) discovered three broad absorption features (at 416, 441 and 515 nm) in the reflectance spectrum of the outer-belt asteroids 1269 Rollandia and 279 Thule. Cruikshank et al (1991b) identified cyano-group containing molecules in the very dark solids of the surfaces of a few D-class asteroids, the dust of some comets, the low-albedo hemisphere of Iapetus, and the rings of Uranus. The occurrence of this band may establish a link between outer solar system and interstellar materials.…”

Section: Spectra and Compositionsmentioning

confidence: 99%

Commission 15: Physical Study of Comets. Minor Planets and meteorites (L’etude Physique des Cometes. des Petites Planetes Et des Meteorites)

1994

Trans. Int. Astron. Union

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Solid CN bearing material on outer solar system bodies

Cited by 109 publications

References 37 publications

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

ICE CHEMISTRY ON OUTER SOLAR SYSTEM BODIES: ELECTRON RADIOLYSIS OF N₂-, CH₄-, AND CO-CONTAINING ICES

Commission 15: Physical Study of Comets. Minor Planets and meteorites (L’etude Physique des Cometes. des Petites Planetes Et des Meteorites)

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Solid CN bearing material on outer solar system bodies

Cited by 109 publications

References 37 publications

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9

ICE CHEMISTRY ON OUTER SOLAR SYSTEM BODIES: ELECTRON RADIOLYSIS OF N2-, CH4-, AND CO-CONTAINING ICES

Commission 15: Physical Study of Comets. Minor Planets and meteorites (L’etude Physique des Cometes. des Petites Planetes Et des Meteorites)

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ICE CHEMISTRY ON OUTER SOLAR SYSTEM BODIES: ELECTRON RADIOLYSIS OF N₂-, CH₄-, AND CO-CONTAINING ICES