http://www.astrochem.org/docs/Cruikshanketal1998.pdf

The Composition of Centaur 5145 Pholus

Visible and Near-Infrared Photometry of the Centaur Objects 1995 GO and 5145 Pholus

We present visible and near-infrared broadband photometry of the Centaur objects 1995 GO and 5145 Pholus. Our data confirm the extremely redV−Jcolor and nearly solarJ−HandH−Kcolors of 5145 Pholus. OurV−Jdata reveal that 1995 GO is as red as the reddest D-type asteroid, 1748 Mauderli, but not nearly as red as 5145 Pholus. We suggest that the red color of 1995 GO is probably due to the presence of organic-rich materials produced by eons of particle bombardment and ultraviolet irradiation of surface grains, a process that may be widespread among the Centaur and trans-neptunian object populations. We show that theV−Jdata for the Centaurs suggest thatV−Jincreases with increasing semimajor axis. If this correlation is correct, then the red colors of the Centaurs 5145 Pholus and 1993 HA2may be typical of fairly pristine Centaur objects. In contrast, the progressively less red colors of 1995 GO and 2060 Chiron may be the result of an increased rate of resurfacing of these objects as they migrate progressively closer to the Sun.

Visible and Near Infrared Photometry of the Centaur Objects 1995 GO and 5145 Pholus

Dark matter in the outer solar system.

This brief overview will cover some recent work on solar system ices. The focus is on the origin, physical properties, composition, and radiation-induced chemistry of ices dominated by water, with an emphasis on comets and water-rich ices on satellites such as Europa. Understanding the physical characteristics and chemistry of these ices is important for explaining observations such as the albedo and sublimation of ice from planetesimals and comets, the formation of molecules that may have led to life, and planning present and future space missions.

Water Ice on Comets and Satellites

We present a new spectrum of 5145 Pholus between 1.15 and 2.4 microns. We model this, and the previously published (0.4-1.0 microns) spectrum, using Hapke scattering theory. The 2.04 micron band of H2O ice is seen in absorption, as well as a strong band at 2.27 Am, interpreted as frozen methanol and/or the methanol photo product hexamethylenetetramine (HMT). The presence of small molecules is indicative of a chemically primitive surface, since heating removes the light hydrocarbons in favor of macromolecular carbon typically found in carbonaceous meteorites. The unusually red slope of Pholus' spectrum is matched by fine grains of Titan tholin, as found previously. Object 1993 HA2, which has an orbit similar to that of 5145 Pholus, is similarly red, but there are as yet no observations of absorption bands in its spectrum. We present a model for the composite spectrum of all spectroscopic and photometric data available for 5145 Pholus and conclude that this is a primitive object which has yet to be substantially processed by solar heat.

The Composition of Planetesimal 5145 Pholus

Asphaltite-like Organics on Planetesimal 5145 Pholus

Composition of 5145 Pholus

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The Composition of Planetesimal 5145 Pholus

Asphaltite-like Organics on Planetesimal 5145 Pholus

Composition of 5145 Pholus