Control of amorphous solid water morphology using molecular beams. I. Experimental results

By G. Kimmel, K. Stevenson, Z. Dohnálek, R. Smith, B. D. Kay. 2001

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Carbon Monoxide Entrapment in Interstellar Ice Analogs (2003, unknown): “Entrapment of other species is expected and has been observed for N2 (Kimmel et al. 2001b).”
Formation of compact solid water after ion irradiation at 15 K (2006, methodology): “If diffusion takes place and a H2O:CO mixture is obtained, CO remains partially trapped in H2O at higher temperatures and up to the crystallization temperature of water ice (about 150 K; Schmitt et al. 1989; Kimmel et al. 2001a; Fraser et al. 2004; Collings et al. 2004).”
Desorption rates and sticking coefficients for CO and N2 interstellar ices (2006, background): “The CO-H2O system has been extensively studied by Collings et al. (2003), who found a binding energy of CO to H2O of 1180 K. Kimmel et al. (2001) derive a binding energy of ≥950 K for N2 on H2O.”
Photodesorption of water ice - A molecular dynamics study (2008, background): “However, it is debated whether the ice is mostly porous, as found in vapor deposited ice (Mayer & Pletzer 1986; Kimmel et al. 2001a,b), or more compact (Fraser et al. 2004; Palumbo 2006).”
Experimental evidence for water formation on interstellar dust grains by hydrogen and oxygen atoms (2009, background): “The annealed water ice substrate is still porous (Kimmel et al. 2001) and mimics an amorphous ice processed by UV and cosmic rays (Palumbo 2006) that is thought to constitute the icy mantle of interstellar grains.”