Color Patterns in the Kuiper Belt: A Possible Primordial Origin

Tegler, S. C.; Romanishin, W.; Consolmagno, S. J. Guy

doi:10.1086/381076

Cited by 96 publications

(86 citation statements)

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“…Surfaces made up of organics exposed to high amounts of radiation (e.g., inner solar system, or older surfaces in the outer solar system) get darker and blacker (or grayer), whereas organic-containing surfaces exposed to less radiation are redder (Andronico et al 1987). This explanation has been used, for instance, to explain the (visible) gray color of Phoebe compared to the red color of the dark material on Iapetus (Strazzulla 1986; Thompson et al 1987;Allamandola et al 1988;Owen et al 2001) as well as the gray color of KBOs of large eccentricity with aphelions >70 AU compared to visibly redder, cold outer solar system KBOs (perihelion >40 AU; Tegler et al 2003). We postulate here that the corresponding trend in the UV is toward older, more weathered regions on Callisto becoming darker and the 350 nm absorption band strength decreasing, which tends to give the spectrum an overall redder slope in the UV.…”

Section: Discussionmentioning

confidence: 99%

Callisto: New Insights fromGalileoDisk‐resolved UV Measurements

Hendrix

Johnson

2008

Astrophysical Journal

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The entire set of observations from the Galileo Ultraviolet Spectrometer (UVS) is analyzed to look for spectral trends across the surface of Callisto, and to probe the spectral shapes in the near-UV. At low resolution, the leading hemisphere is slightly redder than the trailing hemisphere at k > 280 nm; this has been interpreted by past researchers to indicate the presence of SO 2 on the leading hemisphere. Here we point out that such an ''absorption feature'' can be induced when ratioing hemispherical spectra. High-resolution observations are used to detect the presence of an absorption band at high southern latitudes, interpreted to be due to some organic species that is weathered away (carbonized ) at lower latitudes. The presence of CO 2 in the surface and in the atmosphere of Callisto and the dark nature of the surface suggest that carbon-based species are present across the surface associated with either endogenic or delivered organics. These organics experience chemical modification by UV radiation and are mixed into the regolith by meteoritic bombardment. Subject headingg s: planets and satellites: general -planets and satellites: individual (Callisto) -ultraviolet: solar system

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Section: Discussionmentioning

confidence: 99%

Callisto: New Insights fromGalileoDisk‐resolved UV Measurements

Hendrix

Johnson

2008

Astrophysical Journal

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“…comm. ); ( j) Grundy et al (2008); (k) Perna et al (2010); (m) Peixinho et al (2004); (n) Sheppard & Jewitt (2002); (o) Belskaya et al (2003); (p) Sheppard (2007); (q) Tegler & Romanishin (1998); (r) Jewitt & Luu (1998); (s) Barucci et al (1999); (t) Tegler et al (2003); (u) Trujillo & Brown (2002); (v) Boehnhardt et al (2002); (w) Tegler (2011, priv. comm.…”

Section: Observationsmentioning

confidence: 99%

“TNOs are Cool”: A survey of the trans-Neptunian region

Santos-Sanz

Lellouch

Fornasier

et al. 2012

A&A

145

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Context. Physical characterization of trans-Neptunian objects, a primitive population of the outer solar system, may provide constraints on their formation and evolution. Aims. The goal of this work is to characterize a set of 15 scattered disk (SDOs) and detached objects, in terms of their size, albedo, and thermal properties. Methods. Thermal flux measurements obtained with the Herschel-PACS instrument at 70, 100 and 160 μm, and whenever applicable, with Spitzer-MIPS at 24 and 70 μm, are modeled with radiometric techniques, in order to derive the objects' individual size, albedo and when possible beaming factor. Error bars are obtained from a Monte-Carlo approach. We look for correlations between these and other physical and orbital parameters. Results. Diameters obtained for our sample range from 100 to 2400 km, and the geometric albedos (in V band) vary from 3.8% to 84.5%. The unweighted mean V geometric albedo for the whole sample is 11.2% (excluding Eris); 6.9% for the SDOs, and 17.0% for the detached objects (excluding Eris). We obtain new bulk densities for three binary systems: Ceto/Phorcys, Typhon/Echidna and Eris/Dysnomia. Apart from correlations clearly due to observational bias, we find significant correlations between albedo and diameter (more reflective objects being bigger), and between albedo, diameter and perihelion distance (brighter and bigger objects having larger perihelia). We discuss possible explanations for these correlations.

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“…TNOs, in general, have red optical colors in g-, r-, and i-bands; even the "neutral" TNO surfaces, sometimes referred to as "blue" in the literature, are slightly redder than solar. It is well accepted that the small dynamically excited TNOs and Centaurs exhibit a bimodal color distribution, with red and neutral classes (e.g., Tegler & Romanishin 1998;Peixinho et al 2003Peixinho et al , 2012Peixinho et al , 2015Tegler et al 2003Tegler et al , 2016Wong & Brown 2017).…”

Section: Introductionmentioning

confidence: 99%

Col-OSSOS: z-Band Photometry Reveals Three Distinct TNO Surface Types

Pike

Fraser

Schwamb

et al. 2017

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Several different classes of trans-Neptunian objects (TNOs) have been identified based on their optical and near-infrared colors. As part of the Colours of the Outer Solar System Origins Survey (Col-OSSOS), we have obtained g-, r-, and z-band photometry of 26 TNOs using Subaru and Gemini Observatories. Previous color surveys have not utilized z-band reflectance, and the inclusion of this band reveals significant surface reflectance variations between sub-populations. The colors of TNOs in g−r and r−z show obvious structure, and appear consistent with the previously measured bi-modality in g−r. The distribution of colors of the two dynamically excited surface types can be modeled using the two-component mixing models from Fraser & Brown. With the combination of g−r and r−z, the dynamically excited classes can be separated cleanly into red and neutral surface classes. In g−r and r−z, the two dynamically excited surface groups are also clearly distinct from the cold classical TNO surfaces, which are red, with  -g r 0.85 and r−z  0.6, while all dynamically excited objects with similar g−r colors exhibit redder r−z colors. The z-band photometry makes it possible for the first time to differentiate the red excited TNO surfaces from the red cold classical TNO surfaces. The discovery of different r−z colors for these cold classical TNOs makes it possible to search for cold classical surfaces in other regions of the Kuiper Belt and to completely separate cold classical TNOs from the dynamically excited population, which overlaps in orbital parameter space.

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Color Patterns in the Kuiper Belt: A Possible Primordial Origin

Cited by 96 publications

References 20 publications

Callisto: New Insights fromGalileoDisk‐resolved UV Measurements

Callisto: New Insights fromGalileoDisk‐resolved UV Measurements

“TNOs are Cool”: A survey of the trans-Neptunian region

Col-OSSOS: z-Band Photometry Reveals Three Distinct TNO Surface Types

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