Cyanoacetylene (HCCCN), the first member of the cyanopolyyne family (HC n N, where n = 3, 5, 7, ...), is of particular interest in astrochemistry being ubiquitous in space (molecular clouds, solar-type protostars, protoplanetary disks, circumstellar envelopes, and external galaxies) and also relatively abundant. It is also abundant in the upper atmosphere of Titan and comets. Since oxygen is the third most abundant element in space, after hydrogen and helium, the reaction O + HCCCN can be of relevance in the chemistry of extraterrestrial environments. Despite that, scarce information exists not only on the reactions of oxygen atoms with cyanoacetylene but with nitriles in general. Here, we report on a combined experimental and theoretical investigation of the reactions of cyanoacetylene with both ground 3P and excited 1D atomic oxygen and provide detailed information on the primary reaction products, their branching fractions (BFs), and the overall reaction mechanisms. More specifically, the reactions of O(3P, 1D) with HCCCN(X1Σ+) have been investigated under single-collision conditions by the crossed molecular beams scattering method with mass spectrometric detection and time-of-flight analysis at the collision energy, E c, of 31.1 kJ/mol. From product angular and time-of-flight distributions, we have identified the primary reaction products and determined their branching fractions (BFs). Theoretical calculations of the relevant triplet and singlet potential energy surfaces (PESs) were performed to assist the interpretation of the experimental results and clarify the reaction mechanism. Adiabatic statistical calculations of product BFs for the decomposition of the main triplet and singlet intermediates have also been carried out. Merging together the experimental and theoretical results, we conclude that the O(3P) reaction is characterized by a minor adiabatic channel leading to OCCCN (cyanoketyl) + H (experimental BF = 0.10 ± 0.05), while the dominant channel (BF = 0.90 ± 0.05) occurs via intersystem crossing to the underlying singlet PES and leads to formation of 1HCCN (cyanomethylene) + CO. The O(1D) reaction is characterized by the same two channels, with the relative CO/H yield being slightly larger. Considering the recorded reactive signal and the calculated entrance barrier, we estimate that the rate coefficient for reaction O(3P) + HC3N at 300 K is in the 10–12 cm3 molec–1 s–1 range. Our results are expected to be useful to improve astrochemical and photochemical models. In addition, they are also relevant in combustion chemistry, because the thermal decomposition of pyrrolic and pyridinic structures present in fuel-bound nitrogen generates many nitrogen-bearing compounds, including cyanoacetylene.

The reaction of excited nitrogen atoms N( 2 D) with CH 3 CCH (methylacetylene) was investigated under single-collision conditions by the crossed molecular beams (CMB) scattering method with mass spectrometric detection and time-of-flight analysis at the collision energy ( E c ) of 31.0 kJ/mol. Synergistic electronic structure calculations of the doublet potential energy surface (PES) were performed to assist the interpretation of the experimental results and characterize the overall reaction micromechanism. Theoretically, the reaction is found to proceed via a barrierless addition of N( 2 D) to the carbon–carbon triple bond of CH 3 CCH and an insertion of N( 2 D) into the CH bond of the methyl group, followed by the formation of cyclic and linear intermediates that can undergo H, CH 3 , and C 2 H elimination or isomerize to other intermediates before unimolecularly decaying to a variety of products. Kinetic calculations for addition and insertion mechanisms and statistical (Rice-Ramsperger-Kassel-Marcus) computations of product branching fractions (BFs) on the theoretical PES were performed at different values of total energy, including the one corresponding to the temperature (175 K) of Titan’s stratosphere and that of the CMB experiment. Up to 14 competing product channels were statistically predicted, with the main ones, at E c = 31.0 kJ/mol, being the formation of CH 2 NH (methanimine) + C 2 H (ethylidyne) (BF = 0.41), c -C(N)CH + CH 3 (BF = 0.32), CH 2 CHCN (acrylonitrile) + H (BF = 0.12), and c -CH 2 C(N)CH + H (BF = 0.04). Of the 14 possible channels, seven correspond to H displacement channels of different exothermicity, for a total H channel BF of ∼0.25 at E c = 31.0 kJ/mol. Experimentally, dynamical information could only be obtained about the overall H channels. In particular, the experiment corroborates the formation of acrylonitrile + H, which is the most exothermic of all 14 reaction channels and is theoretically calculated to be the dominant H-forming channel (BF = 0.12). The products containing a novel C–N bond could be potential precursors to form other nitriles (C 2 N 2 , C 3 N) or more complex organic species containing N atoms in planetary atmospheres, such as those of Titan and Pluto. Overall, the results are expected to have a potentially significant impact on the understanding of the gas-phase chemistry of Titan’s atmosphere and the modeling of that atmosphere.

The reaction of electronically excited nitrogen atoms, N( 2 D), with vinyl cyanide, CH 2 CHCN, has been investigated under single-collision conditions by the crossed molecular beam (CMB) scattering method with mass spectrometric detection and time-of-flight (TOF) analysis at the collision energy, E c , of 31.4 kJ/mol. Synergistic electronic structure calculations of the doublet potential energy surface (PES) have been performed to assist in the interpretation of the experimental results and characterize the overall reaction micromechanism. Statistical (Rice–Ramsperger–Kassel–Marcus, RRKM) calculations of product branching fractions (BFs) on the theoretical PES have been carried out at different values of temperature, including the one corresponding to the temperature (175 K) of Titan’s stratosphere and at a total energy corresponding to the E c of the CMB experiment. According to our theoretical calculations, the reaction is found to proceed via barrierless addition of N( 2 D) to the carbon–carbon double bond of CH 2 =CH–CN, followed by the formation of cyclic and linear intermediates that can undergo H, CN, and HCN elimination. In competition, the N( 2 D) addition to the CN group is also possible via a submerged barrier, leading ultimately to N 2 + C 3 H 3 formation, the most exothermic of all possible channels. Product angular and TOF distributions have been recorded for the H-displacement channels leading to the formation of a variety of possible C 3 H 2 N 2 isomeric products. Experimentally, no evidence of CN, HCN, and N 2 forming channels was observed. These findings were corroborated by the theory, which predicts a variety of competing product channels, following N( 2 D) addition to the double bond, with the main ones, at E c = 31.4 kJ/mol, being six isomeric H forming channels: c -CH(N)CHCN + H (BF = 35.0%), c -CHNCHCN + H (BF = 28.1%), CH 2 NCCN + H (BF = 26.3%), c -CH 2 (N)CCN(cyano-azirine) + H (BF = 7.4%), trans -HNCCHCN + H (BF = 1.6%), and cis -HNCCHCN + H (BF = 1.3%), while C–C bond breaking channels leading to c -CH 2 (N)CH(2H-azirine) + CN and c -CH 2 (N)C + HCN are predicted to be negligible (0.02% and 0.2%, respectively). The highly exothermic N 2 + CH 2 CCH (propargyl) channel is also predicted to be negligible because of the very high isomerization barrier from the initial addition intermedia...

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The reaction between cyano radicals (CN, X 2 Σ + ) and cyanoethene (C 2 H 3 CN) has been investigated by a combined approach coupling crossed molecular beam (CMB) experiments with mass spectrometric detection and time-of-flight analysis at a collision energy of 44.6 kJ mol –1 and electronic structure calculations to determine the relevant potential energy surface. The experimental results can be interpreted by assuming the occurrence of a dominant reaction pathway leading to the two but-2-enedinitrile (1,2-dicyanothene) isomers ( E - and Z -NC–CH=CH–CN) in a H-displacement channel and, to a much minor extent, to 1,1-dicyanoethene, CH 2 C(CN) 2 . In order to derive the product branching ratios under the conditions of the CMB experiments and at colder temperatures, including those relevant to Titan and to cold interstellar clouds, we have carried out RRKM statistical calculations using the relevant potential energy surface of the investigated reaction. We have also estimated the rate coefficient at very low temperatures by employing a semiempirical method for the treatment of long-range interactions. The reaction has been found to be barrierless and fast also under the low temperature conditions of cold interstellar clouds and the atmosphere of Titan. Astrophysical implications and comparison with literature data are also presented. On the basis of the present work, 1,2-dicyanothene and 1,1-dicyanothene are excellent candidates for the search of dinitriles in the interstellar medium.

We report on a combined experimental and theoretical investigation of the N( 2 D) + CH 2 CCH 2 (allene) reaction of relevance in the atmospheric chemistry of Titan. Experimentally, the reaction was investigated (i) under singlecollision conditions by the crossed molecular beams (CMB) scattering method with mass spectrometric detection and time-offlight analysis at the collision energy (E c ) of 33 kJ/mol to determine the primary products and the reaction micromechanism and (ii) in a continuous supersonic flow reactor to determine the rate constant as a function of temperature from 50 to 296 K. Theoretically, electronic structure calculations of the doublet C 3 H 4 N potential energy surface (PES) were performed to assist the interpretation of the experimental results and characterize the overall reaction mechanism. The reaction is found to proceed via barrierless addition of N( 2 D) to one of the two equivalent carbon− carbon double bonds of CH 2 CCH 2 , followed by the formation of several cyclic and linear isomeric C 3 H 4 N intermediates that can undergo unimolecular decomposition to bimolecular products with elimination of H, CH 3 , HCN, HNC, and CN. The kinetic experiments confirm the barrierless nature of the reaction through the measurement of rate constants close to the gas-kinetic rate at all temperatures. Statistical estimates of product branching fractions (BFs) on the theoretical PES were carried out under the conditions of the CMB experiments at room temperature and at temperatures (94 and 175 K) relevant for Titan. Up to 14 competing product channels were statistically predicted with the main ones at E c = 33 kJ/mol being formation of cyclic-CH 2 C(N)CH + H (BF = 87.0%) followed by CHCCHNH + H (BF = 10.5%) and CH 2 CCNH + H (BF = 1.4%) the other 11 possible channels being negligible (BFs ranging from 0 to 0.5%). BFs under the other conditions are essentially unchanged. Experimental dynamical information could only be obtained on the overall H-displacement channel, while other possible channels could not be confirmed within the sensitivity of the method. This is also in line with theoretical predictions as the other possible channels are predicted to be negligible, including the HCN/HNC + C 2 H 3 (vinyl) channels (overall BF < 1%). The dynamics and product distributions are dramatically different with respect to those observed in the isomeric reaction N( 2 D) + CH 3 CCH (propyne), where at a similar E c the main product channels are CH 2 NH (methanimine) + C 2 H (BF = 41%), c-C(N)CH + CH 3 (BF = 32%), and CH 2 CHCN (vinyl cyanide) + H (BF = 12%). Rate coefficients (the recommended value is 1.7 (±0.2) × 10 −10 cm 3 s −1 over the 50−300 K range) and BFs have been used in a photochemical model of Titan's atmosphere to simulate the effect of the title reaction on the species abundance (including any new products formed) as a function of the altitude.

The reaction between the ground-state hydroxyl radical, OH(2Π), and ethylene, C2H4, has been investigated under single-collision conditions by the crossed molecular beam scattering technique with mass-spectrometric detection and time-of-flight analysis at the collision energy of 50.4 kJ/mol. Electronic structure calculations of the underlying potential energy surface (PES) and statistical Rice–Ramsperger–Kassel–Marcus (RRKM) calculations of product branching fractions on the derived PES for the addition pathway have been performed. The theoretical results indicate a temperature-dependent competition between the anti-/syn-CH2CHOH (vinyl alcohol) + H, CH3CHO (acetaldehyde) + H, and H2CO (formaldehyde) + CH3 product channels. The yield of the H-abstraction channel could not be quantified with the employed methods. The RRKM results predict that under our experimental conditions, the anti- and syn-CH2CHOH + H product channels account for 38% (in similar amounts) of the addition mechanism yield, the H2CO + CH3 channel for ∼58%, while the CH3CHO + H channel is formed in negligible amount (<4%). The implications for combustion and astrochemical environments are discussed.

&lt;p&gt;Cyanopolyynes are a family of carbon-chain molecules that have been detected in numerous objects of the interstellar medium (ISM), such as hot cores, star forming regions and cold clouds [1&amp;#8211;4]. The simplest cyanopolyyne, HC&lt;sub&gt;3&lt;/sub&gt;N, has been among the first organic molecules to be observed in the ISM [5] and up to date also HC&lt;sub&gt;5&lt;/sub&gt;N, HC&lt;sub&gt;7&lt;/sub&gt;N, HC&lt;sub&gt;9&lt;/sub&gt;N and HC&lt;sub&gt;11&lt;/sub&gt;N have been detected [6, 7]. HC&lt;sub&gt;3&lt;/sub&gt;N and HC5N are also abundant in solar-type protostars (see for instance a recent work on IRAS 16293-2422 by Jaber Al-Edhari et al. [8]). Remarkably, HC&lt;sub&gt;3&lt;/sub&gt;N has also been detected in comet C/1995 O1 (Hale-Bopp) and, together with other organic molecules, could be a part of the legacy of interstellar organic chemistry to the newly formed solar systems [9,10].&lt;/p&gt; &lt;p&gt;Cyanoacetylene has been suggested as an important brick in chain elongation processes, via its reaction with the C&lt;sub&gt;2&lt;/sub&gt;H radical producing HC&lt;sub&gt;5&lt;/sub&gt;N. Its reaction with the CN radical, instead, results in a chain termination reaction with the formation of dicyanoacetylene, NC-CC-CN (C&lt;sub&gt;4&lt;/sub&gt;N&lt;sub&gt;2&lt;/sub&gt;). Dicyanoacetylene and higher dicyanopolyynes have not been observed in the ISM so far because they lack a permanent electric dipole moment and cannot be detected through their rotational spectrum. However, it has been suggested that they are abundant in interstellar and circumstellar clouds [11] and account for a significant fraction of the total carbon budget. The reaction between CN radical and cyanoacetylene is also believed to be the main source of C&lt;sub&gt;4&lt;/sub&gt;N&lt;sub&gt;2&lt;/sub&gt;, an observed species in the upper atmosphere of Titan, the massive moon of Saturn [12].&lt;/p&gt; &lt;p&gt;To characterize the chemistry of cyanoacetylene in various extraterrestrial environments, in our laboratory, we have undertaken a systematic investigation of the reactions involving cyanoacetylene and atomic or diatomic radicals which are relatively abundant in space. The investigated reactions include CN + HC&lt;sub&gt;3&lt;/sub&gt;N, O+HC&lt;sub&gt;3&lt;/sub&gt;N and N+HC&lt;sub&gt;3&lt;/sub&gt;N. We have used a sophisticated experimental technique to investigate these reactive systems under single collision conditions in order to be able to establish the nature of the primary products and their branching ratio without ambiguity (for some details see [13]). In addition, we have performed dedicated electronic structure and kinetic calculations to derive the relevant parameters to be included in astrochemical models. Implications for the chemistry of interstellar objects as well as the chemistry of cometary comae and the upper atmosphere of Titan will be noted.&lt;/p&gt; &lt;p&gt;This project has received funding from the European Union&amp;#8217;s Horizon 2020 research and innovation programme under the Marie Sklodowska Curie grant agreement No 811312 for the project &amp;#8221;Astro-Chemical Origins&amp;#8221;.&lt;/p&gt; &lt;p&gt;[1] Wyrowski, F., Schilke, P., Walmsley, C.: Vibrationally excited HC3N toward hot cores. Astronomy and Astrophysics 341 (1999) 882&amp;#8211;895&lt;/p&gt; &lt;p&gt;[2] Taniguchi, K., Saito, M., Sridharan, T., Minamidani, T.: Survey observations to study chemical evolution from high-mass starless cores to high-mass protostellar objects I: HC3N and HC5N. The Astrophysical Journal 854(2) (2018) 133&lt;/p&gt; &lt;p&gt;[3] Mendoza, E., Lefloch, B., Ceccarelli, C., Kahane, C., Jaber, A., Podio, L., Benedettini, M., Codella, C., Viti, S., Jimenez-Serra, I., et al.: A search for cyanopolyynes in L1157-B1. Monthly Notices of the Royal Astronomical Society 475(4) (2018) 5501&amp;#8211;5512&lt;/p&gt; &lt;p&gt;[4] Takano, S., Masuda, A., Hirahara, Y., Suzuki, H., Ohishi, M., Ishikawa, S.i., Kaifu, N., Kasai, Y., Kawaguchi, K., Wilson, T.: Observations of 13C isotopomers of HC3N and HC5N in TMC-1: evidence for isotopic fractionation. Astronomy and Astrophysics 329 (1998) 1156&amp;#8211;1169&lt;/p&gt; &lt;p&gt;[5] Turner, B.E.: Detection of interstellar cyanoacetylene. The Astrophysical Journal 163 (1971) L35&amp;#8211;L39&lt;/p&gt; &lt;p&gt;[6] Broten, N.W., Oka, T., Avery, L.W., MacLeod, J.M., Kroto, H.W.: The detection of HC9N in interstellar space. 223 (July 1978) L105&amp;#8211;L107&lt;/p&gt; &lt;p&gt;[7] Bell, M., Feldman, P., Travers, M., McCarthy, M., Gottlieb, C., Thaddeus, P.: Detection of HC11N in the cold dust cloud TMC-1. The Astrophysical Journal Letters 483(1) (1997) L61&amp;#8211;L64&lt;/p&gt; &lt;p&gt;[8] Jaber Al-Edhari, A., Ceccarelli, C., Kahane, C., Viti, S., Balucani, N., Caux, E., Faure, A., Lefloch, B., Lique, F., Mendoza, E., Quenard, D., Wiesenfeld, L.: History of the solar-type protostar IRAS 16293-2422 as told by the cyanopolyynes. A&amp;A 597 (2017) A40&lt;/p&gt; &lt;p&gt;[9] Mumma, M.J., Charnley, S.B. The Chemical Composition of Comets&amp;#8212;Emerging Taxonomies and Natal Heritage. Annu. Rev. Astron. Astrophys. 49 (2011) 471&amp;#8211;524&lt;/p&gt; &lt;p&gt;[10] Bockel&amp;#233;e-Morvan, D., Lis, D. C., Wink, J. E., Despois, D., Crovisier, J., Bachiller, R., et al. New molecules found in comet C/1995 O1 (Hale-Bopp). Investigating the link between cometary and interstellar material.&lt;br /&gt;A&amp;A 353 (2000) 1101&lt;/p&gt; &lt;p&gt;[11] Petrie, S., Millar, T., Markwick, A.: NCCN in TMC-1 and IRC+ 10216. Monthly Notices of the Royal Astronomical Society 341(2) (2003) 609&amp;#8211;616&lt;/p&gt; &lt;p&gt;[12] Petrie, S., Osamura, Y.: NCCN and NCCCCN formation in titan&amp;#8217;s atmosphere: 2. HNC as a viable precursor. The Journal of Physical Chemistry A 108 (2004) 3623&amp;#8211;3631&lt;/p&gt; &lt;p&gt;[13] Casavecchia, P., Leonori, L., Balucani, N. Reaction dynamics of oxygen atoms with unsaturated hydrocarbons from crossed molecular beam studies: primary products, branching ratios and role of intersystem crossing. Int. Rev. Phys. Chem. 34 (2015) 161-204&lt;/p&gt;