[astro-ph.IM] Ultraviolet (UV) photodesorption regulates the partitioning of water between interstellar ice mantles and the gas phase, yet laboratory yields are generally measured on planar substrates rather than on surfaces […]
![Effect of substrate morphology and composition on the UV photodesorption of water ice at 12 K. (A) Evolution of the XPS-derived ice coverage as a function of photon fluence for an initial coverage of approximately 4 ML deposited on planar gold, planar olivine crystal, olivine microparticle powder, and soot at 12 K. Linear fits to the coverage curves give photodesorption yields of 1.5 × 10−3 , 1.8 × 10−3 , 7.2 × 10−4 , and 7.2 × 10−5 molecule photon−1 , respectively (see Table 1). (B) Scanning electron microscopy image of the olivine powder film, showing micrometer- and submicrometer-sized angular particles. (C) Scanning electron microscopy image of the soot film, showing highly aggregated carbon nanoparticles with a much finer and more ramified morphology. (D) Coverage derived from XPS measurements as a function of UV fluence at 12 K for 2 ML ice films deposited at 120 K (nonporous ice) and 12 K (porous ice), giving photodesorption yields of 4.6 × 10−5 and 1.4 × 10−5 molecule photon−1 , respectively -- [astro-ph.IM]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/11/Suppression.png?resize=1200%2C720&ssl=1)
[astro-ph.IM] Ultraviolet (UV) photodesorption regulates the partitioning of water between interstellar ice mantles and the gas phase, yet laboratory yields are generally measured on planar substrates rather than on surfaces […]