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We investigate the effect of electron irradiation by coronal discharge on several simple hydrocarbons enclathrated in or mixed with H<jats:sub>2<\/jats:sub>O or H<jats:sub>2<\/jats:sub>O+NH<jats:sub>3<\/jats:sub> in simulation of the effects of the solar wind, planetary magnetospheric particles, and cosmic rays on surfaces containing these ices in the outer solar system and interstellar space. H<jats:sub>2<\/jats:sub>O+CH<jats:sub>4<\/jats:sub> clathrate, H<jats:sub>2<\/jats:sub>O+C<jats:sub>2<\/jats:sub>H<jats:sub>6<\/jats:sub>, H<jats:sub>2<\/jats:sub>O+CH<jats:sub>4<\/jats:sub>+NH<jats:sub>3<\/jats:sub>, H<jats:sub>2<\/jats:sub>O+C<jats:sub>2<\/jats:sub>H<jats:sub>6<\/jats:sub>+NH<jats:sub>3<\/jats:sub>, and H<jats:sub>2<\/jats:sub>O+C<jats:sub>2<\/jats:sub>H<jats:sub>2<\/jats:sub> are all initially white ices, and all produce yellowish to brownish organic products upon charged particle irradiation. Significant coloration occurs with doses of 10<jats:sup>9<\/jats:sup> erg cm<jats:sup>\u22122<\/jats:sup>, corresponding to short interplanetary irradiation times. Uranian magnetospheric electrons penetrate to \u223c1 mm depth and deposit this dose in 8, 30, 65, 200, and 500 years into the surfaces of Miranda, Ariel, Umbriel, Titania, and Oberon, respectively. Further irradiation of the laboratory ice surface results in a progressive darkening and a more subdued color. For a conversion efficiency to solids <jats:italic>G<\/jats:italic> \u2243 1 molecule keV<jats:sup>\u22121<\/jats:sup>, the upper limit for the time for total destruction of CH<jats:sub>4<\/jats:sub> and other simple hydrocarbons in the upper 1 mm is 5 \u00d7 10<jats:sup>4<\/jats:sup> years (Miranda) to 3 \u00d7 10<jats:sup>6<\/jats:sup> years (Oberon). Remote detection of CH<jats:sub>4<\/jats:sub> is possible only when its replenishment rate exceeds the destruction rate at the depth probed by spectroscopy. Reflection spectroscopy of irradiated H<jats:sub>2<\/jats:sub>O+CH<jats:sub>4<\/jats:sub> frost is compared with the spectra of several outer solar system objects and to other relevant organic and inorganic materials. Ultraviolet\u2010visible and infrared transmission spectroscopy of the postirradiation residues is presented. Persistence of color and of CH<jats:sub>4<\/jats:sub> ice bands on Triton and Pluto suggests ongoing surface activity and\/or atmospheric haze. Over 4 \u00d7 10<jats:sup>9<\/jats:sup> year time scales, \u2265 10 m of satellite and cometary surface material is processed by cosmic rays to a radiation\u2010hardened ice\u2010tholin mixture devoid of CH<jats:sub>4<\/jats:sub>. Preaccretional chemistry, exogenous materials, and endogenous organic chemistry all contribute to the spectral properties of icy satellites which accreted simple CH(O) molecules. Radiation darkening traces the deposition of mobilized or impact\u2010exposed carbon\u2010bearing volatiles on these satellites. More exhaustive experiments are necessary to work out the detailed relationships between initial composition, exposure age, and color\/albedo.<\/jats:p>","DOI":"10.1029\/ja092ia13p14933","type":"journal-article","created":{"date-parts":[[2008,2,6]],"date-time":"2008-02-06T18:07:10Z","timestamp":1202321230000},"page":"14933-14947","source":"Crossref","is-referenced-by-count":120,"title":["Coloration and darkening of methane clathrate and other ices by charged particle irradiation: Applications to the outer solar system"],"prefix":"10.1029","volume":"92","author":[{"given":"W. Reid","family":"Thompson","sequence":"first","affiliation":[],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"B. G. J. P. T.","family":"Murray","sequence":"additional","affiliation":[],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"B. 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