Structural Organization of Space Polymers

TL;DR

This paper investigates the structural organization of space polymers derived from meteoritic material, proposing a super-polymerization model that explains observed morphologies and their potential role in planetary formation.

Contribution

It introduces a novel super-polymerization model for space polymers, linking macro-structural morphologies to a specific three-dimensional hexagonal diamond structure.

Findings

Identification of macro-structural morphologies in space polymers

Proposal of a super-polymerization process guided by tetragonal symmetry

Hypothesis that low-density structures facilitated planetary accretion

Abstract

Extra-terrestrial polymers of glycine with iron have been characterized by mass spectrometry to have a core mass of 1494Da with dominant rod-like variants at m/z 1567 and m/z 1639 [1]. Several principal macro-structural morphologies are observed in solvent extracts from CV3 class meteoritic material. The first is an extended sheet of linked triskelia containing the 1494Da core entity that encloses gas bubbles in the solvent [1]. A second is of fiber-like crystals found here, via X-ray diffraction, to be multiple-walled nanotubes made from a square lattice of the 1494Da polymer. A third is a dispersion of floating phantom-like short tubes of up to 100micron length [1] with characteristic angled bends that suggest the influence of a specific underlying protein structure. Here it is proposed that the angled tubes are the observable result of a space-filling super-polymerization of 1638Da polymer subunits guided by the tetragonal symmetry of linking silicon bonds. Distorted hexagonal sheets are linked by perpendicular subunits in a three-dimensional hexagonal diamond structure to fill the largest possible volume. This extended very low-density structure is conjectured to have dominated in a process of chemical selection because it captured a maximum amount of molecular raw material in the ultra-low density of molecular clouds or of the proto-solar nebula. This could have led ultimately to the accretion of the earliest planetary bodies.