Branching Processes in the Dissociative Recombination of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msubsup><mml:mrow><mml:mi mathvariant="normal">H</mml:mi></mml:mrow><mml:mrow><mml:mn>3</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msubsup></mml:mrow></mml:math>

Datz, S.; Sundström, Gerdt; Biedermann, C.; Broström, L.; Danared, H.; Mannervik, S.; Mowat, J. R.; Larsson, Mats

doi:10.1103/physrevlett.74.896

Cited by 143 publications

(76 citation statements)

References 24 publications

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“…[4] Furthermore, the group at TSR looked at the dynamics in, and competition between, the two-and threebody fragmentation dynamics of H ¥ 3 . Using a statistical model to describe the process, they reached good agreement with those experimental data previously obtained at CRYRING [5] as a function of reaction energy. [6] It is interesting to examine similar systems in detail to see if more insight can be obtained into the dynamical/statistical nature of the DR process.…”

Section: Introductionsupporting

confidence: 78%

Three-body Reaction Dynamics in Dissociative Recombination

Thomas¹,

Hellberg²,

Larsson

et al. 2003

AIP Conference Proceedings

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Abstract. Dissociative recombination of molecular ions with electrons is the most important neutralising process in plasmas cold enough to contain molecules. The basic features and principles describing recombination of diatomic molecular ions are now reasonably well characterised and understood. However, recombination of polyatomic ions is much less well understood. Over the last six years, experiments carried out at ion storage rings have shown that tri-atomic molecular ions tend to break up into three atoms upon recombination with free electrons. The question of how this break-up occurs has started to be investigated at ion storage rings using particle-imaging techniques. In this presentation, the imagine technique used in these experiments will be discussed together with results obtained from studies of H 2 O ¤ , NH ¤ 2 and CH ¤ 2 . Finally, the use of this technique to study the dissociative recombination of more complex polyatomic ions, for example D 5 O ¤ 2 , will also be discussed.

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Section: Introductionsupporting

confidence: 78%

Three-body Reaction Dynamics in Dissociative Recombination

Thomas¹,

Hellberg²,

Larsson

et al. 2003

AIP Conference Proceedings

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“…[1994]. The yield of the two channels in dissociative recombination of H3 + has also been measured recently by Datz et al [1995], and the reaction has been found to favor the production of three H atoms (channel (RC2)) by a factor of 3:1.…”

Section: Forty Ion Recombination Reactions Have Been Includedmentioning

confidence: 99%

Chemistry of the Jovian auroral ionosphere

Perry¹,

Kim²,

Fox³

et al. 1999

J. Geophys. Res.

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Abstract. We have investigated the chemistry of the Jovian auroral thermosphere-/ionosphere by modeling the precipitation of high-energy electrons into the auroral zones using a multistream electron-transport code and three model thermospheres' a standard model based on pressure and temperature data from Galileo, and two additional models that are characterized by enhanced eddy diffusion coefficients. We have predicted the effects of precipitation of monoenergetic electrons with energies between 20 and 100 keV with energy fluxes of about 11 ergs cm-2s -•. We have derived the column densities of H2, H, CH4, and C2H2 above the altitudes of peak energy deposition. For methane column densities similar to those determined from IUE and Hubble Space Telescope H2 spectral data, we find that for our standard model, the most likely electron energies are in the 45-55 keV range. For the enhanced eddy diffusion models the energies are lower. We present ion density profiles, H density profiles, and production profiles for the most important H2 and H emissions. The predicted H column densities are in the range (1 -6) x 10 •8 cm -2 for the standard model and are smaller for the enhanced eddy diffusion models. We find that the temperatures near the altitude of peak energy deposition vary from 160 to 200 K and are significantly lower than those derived from rotational analyses of auroral H2 emissions, which average 400-500 K. This indicates that the auroral thermosphere is considerably warmer than those at lower latitudes that were measured by the Voyager spacecraft or the Galileo probe.

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“…The branching fractions of the H 2 + H and H + H + H channels were also slightly affected by the rotational temperature. For rotationally hot ions, ∼75% of the DR reactions lead to H + H + H (Datz et al 1995), while for rotationally cold ions H + H + H was produced in 64% ± 5% of the DR reactions (McCall et al 2004). It must be stressed that H 3 + lacks a permanent dipole moment meaning that its rotational temperature does not change much during typical storage times.…”

Section: Branching Fractionsmentioning

confidence: 99%

Dissociative Recombination of Protonated Formic Acid: Implications for Molecular Cloud and Cometary Chemistry

Vigren

Hamberg

Zhaunerchyk

et al. 2010

ApJ

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At the heavy ion storage ring CRYRING in Stockholm, Sweden, we have investigated the dissociative recombination of DCOOD + 2 at low relative kinetic energies, from ∼1 meV to 1 eV. The thermal rate coefficient has been found to follow the expression k(T) = 8.43 × 10 −7 (T/300) −0.78 cm 3 s −1 for electron temperatures, T, ranging from ∼10 to ∼1000 K. The branching fractions of the reaction have been studied at ∼2 meV relative kinetic energy. It has been found that ∼87% of the reactions involve breaking a bond between heavy atoms. In only 13% of the reactions do the heavy atoms remain in the same product fragment. This puts limits on the gas-phase production of formic acid, observed in both molecular clouds and cometary comae. Using the experimental results in chemical models of the dark cloud, TMC-1, and using the latest release of the UMIST Database for Astrochemistry improves the agreement with observations for the abundance of formic acid. Our results also strengthen the assumption that formic acid is a component of cometary ices.

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Branching Processes in the Dissociative Recombination ofH3+

Cited by 143 publications

References 24 publications

Three-body Reaction Dynamics in Dissociative Recombination

Three-body Reaction Dynamics in Dissociative Recombination

Chemistry of the Jovian auroral ionosphere

Dissociative Recombination of Protonated Formic Acid: Implications for Molecular Cloud and Cometary Chemistry

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