A radiolytic origin of organic matter in primitive chondrites and trans-neptunian objects? New clues from ion irradiation experiments
Mathilde Faure, Eric Quirico, Alexandre Faure, Philippe Boduch, Hermann Rothard, Emmanuel Balanzat, Donia Baklouti, Rosario Brunetto, Lydie Bonal, Pierre Beck, Bernard Schmitt
In Press, Journal Pre-proof, Available online 3 April 2021
• Ion irradiation experiments at low and high energy were run on different organic targets to simulate the formation of chondritic Insoluble Organic Matter (IOM).
• Above a critical nuclear dose of 10−7+10 eV.atom−1, any carbonaceous precursor transforms into a sp2-rich amorphous carbon with negligible precursor effect.
• Below this dose, the precursor effect is very significant and chondritic IOM cannot be formed from aromatic-free precursors.
• An IOM formation scenario based on Galactic Cosmic Rays irradiation of aromatic interstellar carbonaceous dust mixed with ices appears plausible.
• Carbonaceous species at the surface of Trans-Neptunian Objects exposed to Solar Wind transform into sp2-rich amorphous carbon that generate a red slope in the visible range.”
“We question here the radiolytic origin of (i) polyaromatic insoluble organic matter (IOM) recovered from primitive chondrites, and (ii) organics at the surface of reddish Trans-Neptunian Objects (TNOs), some minor planets and icy satellites. Organic synthesis by ion irradiation was investigated through experiments on a variety of targets: Polyethylene glycol 1450, lignin, cellulose and sucrose, exposed to low (C 40 keV and Ne 170 keV) and high energy (C 12 MeV, Ni 17 MeV, 78Kr 59 MeV) ions. These experiments show that all carbonaceous precursors evolve towards a sp2-rich amorphous carbon (a-C) above a critical nuclear dose of 10−7+10 eV.atom−1. A thorough review of the literature shows that this value applies for a large range of carbonaceous materials, including C-rich simple ices. Below this critical dose, irradiated targets are carbonized and transformed into cross-linked polymeric disordered solids, with abundant olefinic and acetylenic bonds, but devoid of aromatic or polyaromatic species. Ion irradiation of simple compounds, e.g. ices, is thereby not a viable process to synthesize IOM. However, in the case of aromatic-rich precursors, swift heavy ions irradiation leads to polyaromatic materials, by bridging existing aromatic or polyaromatic units. In the context of Early Solar System, i.e. Galactic Cosmic Rays (GCR) irradiation during 10–20 Myr, the formation of chondritic IOM from simple ices mixed with interstellar Polycyclic Aromatic Hydrocarbons (PAHs) appears as a plausible mechanism. This scenario, based on the recycling of existing carbonaceous interstellar grains under low-temperature conditions, would account for the heterogeneity of the D, 15N and 13C isotopic fractionations at the molecular scale, and the preservation of deuterium hot spots that are highly sensitive to high-temperature conditions (> 300 °C). At the surface of TNOs, sp2-rich amorphous carbons are formed by the implantation of GCRs and Solar wind ions. The electronic dose is also very high for an irradiation time of several Gyr (> 100 eV.atom−1), leading to the formation of reddish disordered solids, provided that the surface contains a minimum abundance of carbonaceous species. Finally, sp2-rich amorphous carbons produced in the laboratory (e.g. the ACAR compound from Zubko et al., 1996) are fair analogues of the darkening agent produced by radiolysis.”