Abstract:Abstract. In the presence of a base such as ammonia liquid HCN (bp 25 °C) polymerizes readily to a black solid from which a yellow-brown powder can be extracted by water and further hydrolyzed to yield c~-amino acids. These macromolecules could be major components of the dark matter observed on many bodies in the outer solar system. The non-volatile black crust of comet Halley, for example, may consist largely of such polymers, since the original presence on cometary nuclei of frozen volatiles such as methane,… Show more
“…The formation of HCN or nitrile-rich materials is of great interest with regard to multiple planetary bodies within the Solar System because of the strong spectral features and prebiological potential of these types of molecules (Matthews, 1992). Thus, it is important to understand the complete range of formation conditions given the wide array of radiation and compositional constraints of different planetary environments.…”
Nitrile incorporation into Titan aerosol accompanying hydrocarbon chemistry is thought to be driven by extreme UV wavelengths (k < 120 nm) or magnetospheric electrons in the outer reaches of the atmosphere. Far UV radiation (120-200 nm), which is transmitted down to the stratosphere of Titan, is expected to affect hydrocarbon chemistry only and not initiate the formation of nitrogenated species. We examined the chemical properties of photochemical aerosol produced at far UV wavelengths, using a high-resolution time-of-flight aerosol mass spectrometer (HR-ToF-AMS), which allows for elemental analysis of particle-phase products. Our results show that aerosol formed from CH 4 /N 2 photochemistry contains a surprising amount of nitrogen, up to 16% by mass, a result of photolysis in the far UV. The proportion of nitrogenated organics to hydrocarbon species is shown to be correlated with that of N 2 in the irradiated gas. The aerosol mass greatly decreases when N 2 is removed, which indicates that N 2 plays a major role in aerosol production. Because direct dissociation of N 2 is highly improbable given the immeasurably low cross section at the wavelengths studied, the chemical activation of N 2 must occur via another pathway. Any chemical activation of N 2 at wavelengths > 120 nm is presently unaccounted for in atmospheric photochemical models. We suggest that reaction with CH radicals produced from CH 4 photolysis may provide a mechanism for incorporating N into the molecular structure of the aerosol. Further work is needed to understand the chemistry involved, as these processes may have significant implications for how we view prebiotic chemistry on early Earth and similar planets.
“…The formation of HCN or nitrile-rich materials is of great interest with regard to multiple planetary bodies within the Solar System because of the strong spectral features and prebiological potential of these types of molecules (Matthews, 1992). Thus, it is important to understand the complete range of formation conditions given the wide array of radiation and compositional constraints of different planetary environments.…”
Nitrile incorporation into Titan aerosol accompanying hydrocarbon chemistry is thought to be driven by extreme UV wavelengths (k < 120 nm) or magnetospheric electrons in the outer reaches of the atmosphere. Far UV radiation (120-200 nm), which is transmitted down to the stratosphere of Titan, is expected to affect hydrocarbon chemistry only and not initiate the formation of nitrogenated species. We examined the chemical properties of photochemical aerosol produced at far UV wavelengths, using a high-resolution time-of-flight aerosol mass spectrometer (HR-ToF-AMS), which allows for elemental analysis of particle-phase products. Our results show that aerosol formed from CH 4 /N 2 photochemistry contains a surprising amount of nitrogen, up to 16% by mass, a result of photolysis in the far UV. The proportion of nitrogenated organics to hydrocarbon species is shown to be correlated with that of N 2 in the irradiated gas. The aerosol mass greatly decreases when N 2 is removed, which indicates that N 2 plays a major role in aerosol production. Because direct dissociation of N 2 is highly improbable given the immeasurably low cross section at the wavelengths studied, the chemical activation of N 2 must occur via another pathway. Any chemical activation of N 2 at wavelengths > 120 nm is presently unaccounted for in atmospheric photochemical models. We suggest that reaction with CH radicals produced from CH 4 photolysis may provide a mechanism for incorporating N into the molecular structure of the aerosol. Further work is needed to understand the chemistry involved, as these processes may have significant implications for how we view prebiotic chemistry on early Earth and similar planets.
“…Matthews (1,54) proposes that this is due to poly-HCN and generated from HCN in the Titanian atmosphere. In Fig.…”
Section: Comparison With Other Bodies In the Solar Systemmentioning
confidence: 99%
“…Specifically, claims are made for the dark involatile surface of the nucleus of Comet Halley, D-class asteriods, the rings of Uranus, the dark hemisphere of Iapetus, the orange-brown clouds of Jupiter and Saturn, and the haze of Titan (1)(2)(3).…”
Section: Introductionmentioning
confidence: 99%
“…72, 678 (1994). Matthews (1992) has proposed that HCN "polymer" is ubiquitous in the solar system. We apply vacuum deposition and spectroscopic techniques previously used on synthetic organic heteropolymers (tholins), kerogens, and meteoritic organic residues to the measurement of the optical constants of poly-HCN in the wavelength range 0.05-40 pm.…”
Can. J. Chem. 72, 678 (1994). Matthews (1992) has proposed that HCN "polymer" is ubiquitous in the solar system. We apply vacuum deposition and spectroscopic techniques previously used on synthetic organic heteropolymers (tholins), kerogens, and meteoritic organic residues to the measurement of the optical constants of poly-HCN in the wavelength range 0.05-40 pm. These measurements allow quantitative comparison with spectrophotometry of organic-rich bodies in the outer solar system. In a specific test of Matthews' hypothesis, poly-HCN fails to match the optical constants of the haze of the Saturnian moon, Titan, in the visible and near-infrared, derived from astronomical observations and standard models of the Titan atmosphere. In contrast, a tholin produced from a simulated Titan atmosphere matches within the probable errors. Poly-HCN is much more N-rich than Titan tholin. [Traduit par la rCdaction]
“…The reaction conditions which produce adenine, when maintained for a period of days, also produce cyanide polymer as a reaction product (Volker 1960). Moreover, what appear to be similar materials can be produced by an electrical discharge in gaseous HCN, or by adding base to liquid HCN (Mathews 1992, Minard et al 1998. In general, the polymeric materials formed in these reactions seem to be heterogeneous in color, structure, and chemical properties depending on the conditions under which the polymer is formed (Ferris et al 1981, Liebman et al 1995, Minard et al 1998.…”
Summary: Aqueous solutions of potassium cyanide and ammonium hydroxide are known to yield a heterogeneous cyanide polymer, containing paramagnetic sites and biologically significant substructures including polypeptides. Here, such solutions were used to prepare various samples of polymer for study by X-band and W-band electron spin resonance (ESR), scanning electron microscopy (SEM), and scanning force microscopy (SFM). Elemental composition of a typical sample of the polymer was C-35.2%, N-38.47%, O-14.51%, and H-4.13%, exposing the polymer to 6M HCl hydrolyzed portions of the polymer and released glycine and traces of other amino acids. The X-band ESR spectra consist of a single slightly asymmetric line centered at g = 2.003; spin concentration measurements made at X-band using a nitroxide radical standard yield approximate radical concentrations of 10 18 spins/gm. W-band ESR indicates the presence of a single rhombic paramagnetic site with g x = 2.0025, g y = 2.0030, and g z = 2.0048 and the possibility of small 14 N hyperfine splittings. The ESR spin echo studies yield a longitudinal relaxation time, T 1, of 75 µS and a short-phase memory relaxation time, T m , of about 300 nS. Scanning electron microscopy studies of the polymer show that it is made of ellipsoidal particles about one micron in size. The particles tend to clump together when suspended in aqueous solution. The particles disperse and dissolve in dimethyl sulfoxide (DMSO); when these solutions dry on microscope slides, optical microscopy shows a branched island morphology for the polymer. This morphology is reminiscent of snowflakes and is identified as dendritic. Phase contrast SFM of the dendritic arms show a striking segregation and ordering of various components of the polymer. Paramagnetic sites are conserved in the series of steps leading to dendritic structures.
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