Towards RNA life on Early Earth: From atmospheric HCN to biomolecule production in warm little ponds

<p><span>The origin of life on Earth involves the early appearance of an information-containing molecule such as RNA. Warm little ponds are ideal sites for the emergence of RNA, as their periodic wet-dry cycles provide conditions favorable for polymerization </span><span>(e.g. Da Silva et al. 2015, Ross & Dea</span><span>mer 2016</span><span>)</span><span>.</span></p><p><span> How did the</span><span> building blocks of </span><span>RNA</span> <span>come to be in warm little ponds </span><span>on early Earth? Is it necessary that they were delivered by meteorites or interplanetary dust? Or was early Earth capable of producing </span><span>them</span><span> on its own? In the latter case, </span><span>the process </span><span>can begin</span><span> with the production of HCN in the atmosphere, which </span><span>reacts in aqueous solution to produce several </span><span>key</span><span> RNA </span><span>precursors such as nucleobases, ribose, and 2-aminooxazole</span> <span>(e.g. Yi et al. 2020, Hill & Orgel 2002, Becker et al. 2018, Powner et al. 2009).</span></p><p><span> Here, we construct a robust physical and non-equilibrium chemical model of the early Earth atmosphere in which lightning and external UV-driven chemistry produce HCN. The atmosphere is supplied with hydrogen from impact degassing of meteorites, sourced with water evaporated from the oceans, carbon dioxide from volcanoes, and methane from undersea hydrothermal vents. This </span><span>model </span><span>allows us to calculate the rain-out of HCN into warm little ponds (WLPs). We then use a comprehensive sources and sinks numerical model to compute the resulting abundances of nucleobases, ribose, and nucleotide precursors such as 2-aminooxazole resulting from aqueous and UV-driven chemistry within them. We find that at 4.4 bya (billion years ago) peak adenine concentrations in ponds can be maintained at &#8764;2.8&#956;M for more than 100 Myr. Meteorite delivery of adenine to WLPs produce similar peaks </span><span>in concentration, but are destroyed within months by UV photodissociation, seepage, and hydrolysis. The early evolution of the atmosphere is dominated by the decrease of hydrogen due to falling impact rates and atmospheric escape, and the rise of oxygenated species such as OH from H₂O photolysis. Our work points to an early origin of RNA on Earth within ~200 Myr of the Moon-forming impact.</span></p>