2005
DOI: 10.1016/j.ijms.2004.10.015
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Reactions of Cn (n=1–3) with ions stored in a temperature-variable radio-frequency trap

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Cited by 23 publications
(38 citation statements)
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“…have been performed by Savić et al (2005) at an estimated translational temperature of ∼ 1, 000 K (see Section 9.2 for a discussion of both the translational and internal temperatures in their work). Throughout this paper, we use the term "translational temperature" to refer to the reaction center-of-mass velocity distribution when it is described by a Maxwell-Boltzmann distribution.…”
Section: Introductionmentioning
confidence: 99%
“…have been performed by Savić et al (2005) at an estimated translational temperature of ∼ 1, 000 K (see Section 9.2 for a discussion of both the translational and internal temperatures in their work). Throughout this paper, we use the term "translational temperature" to refer to the reaction center-of-mass velocity distribution when it is described by a Maxwell-Boltzmann distribution.…”
Section: Introductionmentioning
confidence: 99%
“…1 These so-called Swings emission bands 2 of C 3 were first reproduced in the laboratory by Herzberg 3 in 1942, although the final assignment of the rovibronic spectra was attributed to Douglas 4 and Gausset et al 5,6 Since then, the C 3 radical has been observed in a wide range of astrophysical sources, 7,8 including circumstellar shells of carbon stars, [9][10][11] interstellar molecular clouds, [12][13][14][15] and comets. 1,10 As the most abundant small pure carbon molecule in the interstellar medium, [16][17][18] C 3 along with its smaller congener C 2 are the central key to the formation of more complex carbon clusters, long-chain cyanopolyynes, carbon dust, and polycyclic aromatic hydrocarbons. 2,19,20 Mebel and Kaiser 21 provided alternative pathways, besides the C( 3 P j ) + C 2 H 2 (X 1 Σ + g ) reaction, 22 through which linear C 3 (  X 1 Σ + g ) would be formed in interstellar environments, i.e., in the reactions CH(X 2 Π Ω ) + C 2 (X 1 Σ + g ) and C( 3 P j ) + C 2 H(X 2 Σ + ), the latter being most relevant in interstellar space.…”
Section: Introductionmentioning
confidence: 99%
“…40,41 These methods also cannot be used to study reactions with C which, due to its high reactivity, cannot be generated in sufficient quantities in the flows. 40,42,43 Lastly, the measured rate coefficients can vary by orders of magnitude as a function of parent and buffer gas pressures. 44 Thus a systematic study of rate coefficient versus these gas pressures may be necessary to generate reliable measurements.…”
Section: Introductionmentioning
confidence: 99%