Photodestruction of Relevant Interstellar Molecules in Ice Mixtures

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Formation rates of complex organics in UV irradiated CH3OH-rich ices I: Experiments (2009, methodology): “This explains the higher cross-section value obtained in these experiments compared to Gerakines et al. (1996) and Cottin et al. (2003), who recorded 1.6× 10−18 cm2 and 6× 10−19 cm2, respectively.”
PHOTODESORPTION OF ICES. II. H2O AND D2O (2008, methodology): “The ice loss is modelled by a combination of an exponential function and a linear function, where the exponential function describes the photolysis of bulk D2O as a first order process similarly to Cottin et al. (2003).”
Photodesorption of ices I: CO, N₂, and CO₂ (2008, methodology): “In the case of CO, there is no measurable photodissociation in this wavelength range and the measured photon-induced loss yield is the photodesorption yield (Gerakines et al. 1996; Cottin et al. 2003; Öberg et al. 2007).”
Mechanisms of Amino Acid Formation in Interstellar Ice Analogs (2007, background): “The flux of such lamps has been shown to vary with time and operating conditions, but in this work we have assumed a nominal flux of �2 ; 1015 photons cm-2 s-1 (Warneck 1962; Cottin et al. 2003; Loeffler et al. 2005).”
Amino acid photostability on the Martian surface (2005, methodology): “With the optically-thin assumption verified, first order reaction kinetics (Cottin et al. 2003) were applied to calculate the half-life and the UV destruction cross section of the solid glycine and D-alanine.”