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Pluto and Charon: Surface Colors and Compositions — a Hypothesis 47th Lunar and Planetary Science Conference (2016) 1696.pdf PLUTO AND CHARON: SURFACE COLORS AND COMPOSITIONS--A HYPOTHESIS D. P Cruikshank1 S. A. Stern2, W. M. Grundy3, J. M. Moore1 L. A. Young2, C. B. Olkin2, H. A. Weaver4 , K. Ennico1, J. C. Cook2, and the New Horizons Composition Theme Team 1NASA Ames Research Center ([email protected]), 2Southwest Research Institute, 3Lowell Observatory, 4Appl. Phys. Lab Johns Hopkins Univ. Introduction: The surface of Pluto displays an ence of a number of small molecules, including NH3, array of colors ranging from yellow to red to brown, plus complex macromolecular carbonaceous material. while the surface of Charon is largely gray with a north Mass spectra of organic molecules desorbed from the polar zone of red color similar to regions on Pluto[1,2]. residue show a high degree of aromatization, while UV Pluto’s surface shows layers of intensely colored mate- fluorescence imaging shows an overall high concentra- rial in tilted and transported blocks, and fractured geo- tion of organics. The yellow-to-brown colors of the graphical units. This arrangement suggests episodes of residue are consistent with the presence of conjugated formation or deposition of that material interspersed carbon-carbon chains. Material of comparable com- with episodes of emplacement of ices having little or plexity characterizes the insoluble organic matter no color. The ices identified on the surfaces of these (IOM) in carbonaceous meteorites[11]. IOM is found two bodies (N2, CH4, CO, C2H6, H2O on Pluto, and to contain small molecules and radicals trapped in the H2O and NH3 on Charon)[3,4] are colorless, as are carbonaceous complex for astronomical time scales. nearly all ices in a powdery state. The colors on Pluto The PIT also contains small molecules, notably NH3, probably arise from the in situ formation of a macro- and probably radicals that are stable on long time- molecular carbonaceous material generated by energet- scales. ic processing of the ices on the surface[5]. Laboratory The low albedo and neutrally colored regions of experiments producing refractory tholins particularly Charon may be caused by the presence of tholin, possi- relevant to Pluto explored the chemistry of both UV bly PIT, that has largely been radiation processed to and low-energy electron bombardment of a mix of the point where most of the hydrogen is lost and the Pluto ices (N2:CH4:CO = 100:1:1)[6,7]. We can term color has consequently vanished. This over- this Pluto ice tholin PIT. processing, or carbonization of tholins is known from Water ice in the crystalline state characterizes early work[e.g., 12]. Such over-processing would be Charon’s surface, and while most of Charon’s surface expected for an old surface that is not refreshed with is neutral in color, with geometric albedo ~0.38 [2,3], PIT, which might either be excavated from depth, the polar zone and a light cover of fainter but similar where it was made in a previous epoch of this body's reddish color over some surface regions suggest a history, or made currently or recently from an invento- common origin with the colored material on Pluto. ry of N2 and CH4 ices. In this view, the surface under- NH3 or NH3•nH2O was identified from disk-integrated lying the gray material bears orange PIT that has been Earth-based spectra[e.g.,8,9], and a few concentrated protected from overprocessing, or possibly a mix of NH3 exposures have been found in the New Horizons CH4 and N2 ices in which PIT has been made relatively spectral images [10]. recently through the same or similar processes as are Open Questions: In terms of the composition and currently active on Pluto itself. The visible surface ice evolution of the surfaces of Pluto and Charon, a num- layer(s) of Charon are dominantly composed of the ber of puzzles present themselves. Why does H2O ice very refractory crystalline H2O ice, as noted above, and dominate the surface of Charon? What is the origin of its low albedo is a consequence of intermixing or light the NH3 or NH3 hydrate found in low abundance over blanketing by carbon-dominated, over-processed most of the surface, with a few isolated outcrops of tholin. higher concentration? How can NH3 persist on Charon Concerning the current presence of NH3 or when it is readily destroyed by UV radiation? Why is NH3•H2O exposed over most of Charon, NH3 synthe- the overall albedo of Charon rather low and the color sized in the tholin-making process and trapped for a mostly neutral, except for the north polar region, which long time can slowly diffuse out of the complex tholin displays a color similar to many regions on Pluto? matrix, diffuse through the overlayer of H2O ice, and Why is NH3 or its hydrate not identified on Pluto, appear in small concentration on the optical surface, as while a number of other molecules are? detected spectroscopically. The destruction by UV and Toward an Understanding: Turning first to recent replenishment by upward diffusion would, in principle, laboratory studies of the refractory residues left from reach some balance, and that balance could be different the UV or electron irradiation of the Pluto ice mix in different epochs of the evolution of the Pluto-Charon (PIT) noted above, chemical analysis shows the pres- system. It is also noteworthy that NH3 diffusing 47th Lunar and Planetary Science Conference (2016) 1696.pdf through H2O results in the hydration of the ammonia, formation of the coloring agent(s) are most likely de- thus producing NH3•nH2O[13,14]. The hydration is pendent on the ages of surface units and the atmos- facilitated if the ice structure is disrupted, as can occur pheric density and composition over time. by sputtering or micrometeoroid impacts. Other small NH3 found on Charon may be explained as a prod- molecules may also diffuse out of the tholin, but either uct of the radiation processing of the same simple mol- fail to emerge on the surface with the H2O ice, or go ecules as now found on Pluto and sequestered in the undetected because of low concentration or spectro- resulting complex organic material that is referenced scopic insensitivity. Other such molecules could in- here as Pluto ice tholin (PIT). While the modern sur- clude H2CO, HCOOH, and N-bearing species. There face of Charon is denuded of N2 and (possibly) CH4 has been no detection of NH3 or its hydrate(s) on Pluto ices, the PIT generated in an earlier epoch underlies the to date, but they may be present and undetectable be- H2O ice surface. NH3 diffuses out of the PIT and cause of low concentration and the interference of oth- through the H2O to emerge on the surface, where it er, stronger absorption bands of the known constitu- soon is lost by dissociation. Some or all of the NH3 is ents. hydrated by the process of diffusion through H2O ice. In order for tholin to be made on Charon's surface, The colored region at Charon's north pole results the necessary ingredients must be present, at least for from the excavation of PIT formed in an earlier epoch some period of time. A nitrogen-bearing molecule is by the removal of the H2O-ice-dominated overlayer. clearly needed to produce the NH3 now seen. PIT is The region around the crater informally called N-rich (N/C~0.9 for the electron-generated tholin[6]), Organa[10] is enriched in NH3 by some aspect of the so the very volatile N2 is needed, in addition to CH4, impact process that produced it, perhaps by reducing which is significantly less volatile. The presence of the overburden of H2O ice, thus exposing a layer in colored PIT or similar material on Charon is indicated which NH3 that diffused out of tholin had accumulated. by the coloration of the north polar region. Thus, while The hypothesis presented here challenges scenarios a primordial inventory of NH3 could be native to Char- of the formation of the Pluto-Charon binary and con- on, it appears more likely that N2 was an initial compo- cepts of volatile retention by both components in the nent of the body, as it apparently was for Pluto. If, face of the energetics of formation and tidal locking. It then, Pluto and Charon shared a common inventory of further invites a closer look at the formation and evolu- primordial ices, there could have been an epoch in tion of the coloring components of the surfaces of both Charon's history when a PIT-like material would form bodies. there before all the N2 was lost. Remaining CH4 ice Counter arguments to the hypothesis present here would be radiation processed to the point of the loss include (but are not limited to) the means by which the (or near loss) of the CH4 spectral signature and its con- present-day H2O ice cover on Charon came to overlie version to elemental carbon, which now appears as a an ancient tholin. Ejecta from impacts penetrating to neutral, albedo-lowering component of the H2O ice the H2O ice mantle may have been effective in this surface. sense. It is also noted that fractured blocks seen in This view of the chemical evolution of Charon's press release images of Charon’s surface do not expose surface appears to require that some amount of N2 and any clear layer(s) of colored material. CH4 survived the event of its formation so that the raw materials for tholin formation were available for the References: synthesis of the colored and neutral components.
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