Vacuum UV spectrum of C3 trapped in argon at 8 K

Chang, Kok Wai

doi:10.1063/1.444431

Cited by 34 publications

(17 citation statements)

References 28 publications

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“…3 and one can see that they vary smoothly with chain length. The filled circles are experimental points for odd n from [16] and [18]. We see rather good agreement for the larger Fig.…”

Section: Resultssupporting

confidence: 53%

Optical response of small carbon clusters

Yabana

Bertsch

1997

Z Phys D - Atoms, Molecules and Clusters

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We apply the time-dependent local density approximation (TDLDA) to calculate dipole excitations in small carbon clusters. A strong low-frequency mode is found which agrees well with observation for clusters C_n with n in the range 7-15. The size dependence of the mode may be understood simply as the classical resonance of electrons in a conducting needle. For a ring geometry, the lowest collective mode occurs at about twice the frequency of the collective mode in the linear chain, and this may also be understood in simple terms.Comment: 19 pages, Latex(Revtex), and 7 figures Postscript; to be published in Zeit. Phys. D; contact is bertsch@phys.washington.ed

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“…3 and one can see that they vary smoothly with chain length. The filled circles are experimental points for odd n from [16] and [18]. We see rather good agreement for the larger Fig.…”

Section: Resultssupporting

confidence: 53%

Optical response of small carbon clusters

Yabana

Bertsch

1997

Z Phys D - Atoms, Molecules and Clusters

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“…We have collected here the optical response of several carbon chains. Chains have been unambiguously observed up to 15 C atoms [19,20]. The extension to 32 atoms, as presented in the figure, is thus somewhat academic.…”

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confidence: 55%

“…For completeness we have also reported the experimental results of [19,20] and the theoretical results of [21] (TDLDA calculations) and [17,18] [19] and [20], and various calculations: TDLDA from [21], quantum chemistry (CI) calculations from [17] and [18]. We now turn towards an exploration of non-linear excitations.…”

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confidence: 99%

Dynamical Effects in the Optical Response of Carbon Chains

Berkus

Reinhard

Suraud³

2002

IJMS

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Abstract:We discuss the optical response of small carbon chains from the linear to the non linear domain in the framework of Time Dependent Local Density Approximation. We show that even for moderate ionizations, corresponding to a moderately intense excitation, the optical response exhibits significant alteration with respect to the truly linear domain response. This reflects non trivial dynamical effects at the level of electrons.Keywords: optical response; carbon chains; linear and non-linear excitations.The physics of clusters in intense fields, in particular intense lasers fields, is currently motivating many experimental and theoretical studies [1][2][3][4][5][6][7][8][9][10]. Several experiments have been performed on rare gas clusters [3,5,6] as well as on metal clusters [2,4]. In both, rare gas and noble metal clusters, intense fields can easily ionize semi-core electrons which immediately take part into the response of the system. The details of the behavior of these stripped semi-core electrons is not yet fully understood. In particular, it is expected that these electrons remain for a sizable amount of time inside the clusters, and thus actively participate into the further excitation of the system. They can thus be heated up to keV energies and behave as a plasma which can undergo giant dipole oscillations, both effects leading to a complete and very energetic destruction of the system [2,6,11]. The theoretical description of such highly non-linear situations is still at its beginning [6,[8][9][10][11]. In particular, a proper understanding of the behavior of the (originally) rather deeply bound electrons requires the use of sophisticated microscopic methods. A good starting point is the fully fledged Time Dependent Local Density Approximation (TDLDA) as developed at various levels of refinements since a few years

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“…(Monninger et al 2002;van Hemert & van Dishoeck 2008;Chang & Graham 1982). Because the dissociation limit is equal to 7.62 eV (162.7 nm) (Baulch et al 2005;Martin & Taylor 1995;Gingerich et al 1994) A.3.…”

Section: Resultsmentioning

confidence: 99%

Photochemistry of C₃H_phydrocarbons in Titan’s stratosphere revisited

Hébrard¹,

Dobrijévic²,

Loison³

et al. 2013

A&A

124

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The description of C 3 hydrocarbon chemistry in current photochemical models of Titan's atmosphere is found to be far from complete. We have carefully investigated the photochemistry involving C 3 H p compounds in the atmosphere of Titan (considering both photolysis and neutral reactions), which considerably impacts the abundances of many other hydrocarbon species (including C 2 compounds). Model results indicate that three species (C 3 , c−C 3 H 2 and C 3 H 3 ) could be abundant enough to be present in the Cassini/INMS data. Because the error bars on predicted C 3 -hydrocarbon abundances are considerably larger than those of the observational data, new experimental and theoretical studies targeting the measurement of low-temperature reaction rate constants and product branching ratios are required to reduce current model uncertainties. In particular, we highlight 30 "key reactions", the uncertainty factors of which should be lowered to improve the quality of photochemical models involving C 3 H p molecules.

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Vacuum UV spectrum of C3 trapped in argon at 8 K

Cited by 34 publications

References 28 publications

Optical response of small carbon clusters

Optical response of small carbon clusters

Dynamical Effects in the Optical Response of Carbon Chains

Photochemistry of C₃H_phydrocarbons in Titan’s stratosphere revisited

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Vacuum UV spectrum of C3 trapped in argon at 8 K

Cited by 34 publications

References 28 publications

Optical response of small carbon clusters

Optical response of small carbon clusters

Dynamical Effects in the Optical Response of Carbon Chains

Photochemistry of C3Hphydrocarbons in Titan’s stratosphere revisited

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Photochemistry of C₃H_phydrocarbons in Titan’s stratosphere revisited