Possible contribution of organometallic species in the solar system ices. Reactivity and spectroscopy

Klotz, A.; Marty, Philippe; Boissel, P.; de, Dominique; Serra, G.; Mascetti, Joëlle; Parseval, Patrick de; Derouault, J.; Daudey, J. P.; Chaudret, Bruno

doi:10.1016/0032-0633(96)00026-8

Cited by 40 publications

(46 citation statements)

References 23 publications

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“…Klotz et al (1995) noted that in the most common PAH complexes, each metal is bonded by six electrons on the same ring, implying that p z rings adjacent to a metal-bonded ring are not available to bond other metal atoms. They concluded that there can be at most one metal per two rings, or 12 C atoms.…”

Section: Saturation Of V Ery Small Grains With Metalsmentioning

confidence: 99%

Interstellar Depletion onto Very Small Dust Grains

Weingartner

Draine

1999

ApJ

110

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We consider the depletion of elements from the interstellar gas onto a population of very small dust grains. Adopting a grain model in which D4% of the cosmic C abundance is in grains with radii ¹10we Ðnd that the rate of accretion onto these grains is fast enough to account for the observed large A , depletions of elements like Ti, without invoking unreasonably high rates of mass transfer between interstellar phases or low grain destruction rates. If these grains are composed of arene rings, then only a limited number of metal atoms can be locked up in them. The depletion would be quenched when this limit is reached, unless there is a mechanism for transferring the metals to larger grains and refreshing the very small grain populationÈfor example, by grain coagulation and shattering in the di †use interstellar medium (ISM). If Fe depletes onto the very small grains, then for reasonable coagulation rates there is at least one metal atom per Ðve C atoms in the very small grain population. Furthermore, B60% of the cosmic Fe is associated with the carbonaceous grain population. It is unclear whether this scenario is compatible with observations. However, if there is another population of very small grains, with a large capacity for holding Fe atoms, it might be the sink for the most heavily depleted elements.

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Section: Saturation Of V Ery Small Grains With Metalsmentioning

confidence: 99%

Interstellar Depletion onto Very Small Dust Grains

Weingartner

Draine

1999

ApJ

110

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“…Several substituted PAHs have been studied theoretically and experimentally in order to seek to match the UIR bands. These include nitrogen substituted PAHs (Cook et al 1996;Bauschlicher 1998a;Mattioda et al 2003Mattioda et al , 2005Hudgins et al 2005;Alvaro Galué et al 2010), oxygen substituted PAHs (Cook et al 1996;Bauschlicher 1998b;Hudgins et al 2005), silicon substituted PAHs , methyl substituted PAHs , and PAHs with Fe and Mg (Serra et al 1992;Klotz et al 1995;Hudgins et al 2005;Simon et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Theoretical study of deuteronated PAHs as carriers for IR emission features in the ISM

Buragohain

Pathak

Sarre

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Indeed, most PAH ion spectra reported to date have been obtained using this method. We may also note that variants of this method are currently being applied to study the spectroscopy and (photo-)chemistry of PAHs and other species in interstellar ices (Bernstein et al 2007;Bouwman et al 2009;Klotz et al 1996). Matrix isolation spectra feature narrow bandwidths induced by the low temperature and the quenching of rotational motion in the rare gas matrix.…”

Section: Experimental Methods Comparedmentioning

confidence: 99%

“…Recent applications include the study of nitrogen containing PAHs (Mattioda et al 2003), which have been suggested to provide a better match for the interstellar 6.2 µm emission band (Hudgins et al 2005;Peeters et al 2002), and of complexes of PAHs and atomic Fe, which have been suggested to be stable in interstellar clouds (Klotz et al 1996;Wang et al 2007). The method has also been applied to record PAH spectra in the far-infrared range of the spectrum (Mattioda et al 2009), where very molecule-specific vibrational modes -the socalled "drumhead" modes -are located.…”

Section: Matrix Isolation Spectroscopymentioning

confidence: 99%

“…Clear differences are observed in the spectra of (even-electron) protonated species and (odd-electron) radical cation species. PAHs have long been suggested to efficiently bind to astrophysically abundant metal atoms or ions (Joalland et al 2009;Klotz et al 1996) and such species are now being investigated spectroscopically using IRMPD spectroscopy (Simon et al 2008;Szczepanski et al 2006).…”

Section: Ir Multiple Photon Dissociation Spectroscopymentioning

confidence: 99%

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