In the present review we analyze the available literature on the distribution of dust in the Universe, methods of its observation and determination of the chemical composition, and the roles for terrestrial prebiotic chemistry. The most plausible natural sources of dust on the Earth in the prebiotic era are sedimentation of interplanetary dust, meteoritic and cometary impacts, volcanic eruptions, and soil microparticulates; the interplanetary medium being among the most powerful supplier of the dust matter. Two fundamental roles of dust particles for the origins of life are considered: (1) catalytic formation of prebiotic compounds; and (2) delivery of organic matter to the Earth by space dust particles. Due to the fact that there is only approximate information on the chemical composition and properties of interstellar, circumstellar, and major part of interplanetary dust, even the simulating experiments are difficult to perform. Until these gaps are filled, it seems reasonable to focus efforts of the scientists dealing with dust-driven catalytic formation of prebiotically important compounds on the volcanic and meteoritic/cometary impact environments.

Dust in the Universe: implications for terrestrial prebiotic chemistry.

Some earlier equilibrium calculations with different C/O ratios involving the gas phase and several condensed phase species were repeated here with a considerably more extensive chemistry. As before, condensation substantially changes the partial pressure of HCN, and the similarities with the earlier work suggest that the chemistry is relatively complete.

Some condensation calculations for different C/O ratios

Millimeter-wave observations of the extremely carbon-rich circumstellar envelope of IRC +10°216 show several emission lines that we identify with rotational transitions of methanol. We describe our observations and the reasoning that led to this identification. We argue that shock chemistry, ion-molecule reactions, and grain surface reactions might all be potential sources of circumstellar methanol. Each of these pathways either requires or produces H2O in the envelope of IRC +10°216.

https://iopscience.iop.org/article/10.1086/310046/pdf

Methanol in the Circumstellar Envelope of IRC +10°216

We have performed some equilibrium calculations using a modified form of the computer code SOLGASMIX to calculate the abundances of a number of important gas phase and condensed phase species at temperatures below 2000K which are relevant to very cool stellar atmospheres and circumstellar shells. Calculations have been done for a number of different C/O ratios from oxygen rich to carbon rich, and the condensation of grains can significantly alter the C/O ratio of the gas phase, which can have a large effect on a number of molecular species. It was found that for some moderately oxygen rich mixtures the condensation of silicates can substantially enhance the abundance of gas phase species like HCN which was looked at in some detail.

Condensation calculations in circumstellar shells for different C/O ratios.

Condensation Calculations in Circumstellar Shells for Different C/O Ratios

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Condensation calculations in circumstellar shells for different C/O ratios.

Condensation Calculations in Circumstellar Shells for Different C/O Ratios