Diogo V. Gonçalves
Instituto Superior Técnico, Universidade de Lisboa

Abstract
Titan's cryovolcanism may erupt water-ammonia flows onto the moon's surface. These water-ammonia environments can then hydrolyze Titan’s organic aerosols to produce prebiotic molecules. Such transition to prebiotic chemistry – accelerated by the presence of ammonia – is most likely to occur on Titan's polar regions, where cryovolcanic geomorphological features are most common. Unfortunately, NASA's upcoming Dragonfly lander is due to explore equatorial locations, hindering the investigation of the prebiotic potential of Titan’s cryovolcanism. I will present a scenario through which cryo-volcanogenic alanine and glycine may be transported from Titan’s poles to its equator, where Dragonfly may detect them. I will also show how the interaction between alanine and glycine influences their individual photodegradation rates, expanding the traditional focus on the interaction with inorganic surfaces alone. Lastly, I will present ongoing efforts to produce a proof-of-concept fiber optic chemical sensor designed to characterize, in-situ, the composition of Titan's lakes.

2025 May 16, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Auditorium)
Rua das Estrelas, 4150-762 Porto