Detection of C
 8
 H
 -
 and Comparison with C
 8
 H toward IRC +10 216

Remijan, Anthony J.; Hollis, J. M.; Lovas, F. J.; Cordiner, Martin; Millar, T. J.; Markwick-Kemper, A. J.; Jewell, P. R.

doi:10.1086/520704

Cited by 171 publications

(122 citation statements)

References 15 publications

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“…Since then, it and other anions have been detected in a variety of sources (Brünken et al 2007;Remijan et al 2007;Sakai et al 2010b;Cordiner et al 2011). Rate12 includes 22 new anions, which are involved in 1280 reactions.…”

Section: Anion Reactionsmentioning

confidence: 99%

The UMIST database for astrochemistry 2012

McElroy

Walsh

Markwick

et al. 2013

A&A

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909

880

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We present the fifth release of the UMIST Database for Astrochemistry (UDfA). The new reaction network contains 6173 gas-phase reactions, involving 467 species, 47 of which are new to this release. We have updated rate coefficients across all reaction types. We have included 1171 new anion reactions and updated and reviewed all photorates. In addition to the usual reaction network, we also now include, for download, state-specific deuterated rate coefficients, deuterium exchange reactions and a list of surface binding energies for many neutral species. Where possible, we have referenced the original source of all new and existing data. We have tested the main reaction network using a dark cloud model and a carbon-rich circumstellar envelope model. We present and briefly discuss the results of these models.

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Section: Anion Reactionsmentioning

confidence: 99%

The UMIST database for astrochemistry 2012

McElroy

Walsh

Markwick

et al. 2013

A&A

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909

880

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“…This was later confirmed based on chemical models (Miller et al, 2007), which was then followed by detection of C 8H -and C4H -in the molecular cloud TMC-1 (BrOnken et al, 2007). C 8H -was detected within the circumstellar envelope IRC+10 216 by Remijan et al (2007). Sakai et al (2007) detected C6H-within a low-mass star-forming region of L1527 and then later Sakai et al (2008) reported the detection of C 4H-near the low-mass Class 0 protostar IRAS 04368+2557.…”

Section: Introductionmentioning

confidence: 98%

Heavy ion formation in Titan's ionosphere: Magnetospheric introduction of free oxygen and a source of Titan's aerosols?

Sittler

Ali

Cooper

et al. 2009

Planetary and Space Science

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“…The molecular anions detected so far in the interstellar and circumstellar gas are all fairly heavy linear carbon chains consisting of three or more carbon atoms, and with neutral counterparts with large electron affinities: C 4 H − , C 6 H − , C 8 H − , C 3 N − , and C 5 N − (McCarthy et al 2006;Cernicharo et al 2007;Brünken et al 2007a;Remijan et al 2007;Thaddeus et al 2008;Cernicharo et al 2008). The abundance of these anions relative to the neutral counterparts increases with both size and the electron affinity of the neutral molecule, as expected for formation by radiative electron attachment (Herbst & Osamura 2008).…”

Section: Introductionmentioning

confidence: 99%

Astronomical identification of CN^-, the smallest observed molecular anion

Agúndez¹,

Cernicharo

Guèlin³

et al. 2010

A&A

229

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We present the first astronomical detection of a diatomic negative ion, the cyanide anion CN − , and quantum mechanical calculations of the excitation of this anion by means of collisions with para-H 2 . The anion CN − is identified by observing the J = 2−1 and J = 3−2 rotational transitions in the C-star envelope IRC +10216 with the IRAM 30-m telescope. The U-shaped line profiles indicate that CN − , like the large anion C 6 H − , is formed in the outer regions of the envelope. Chemical and excitation model calculations suggest that this species forms from the reaction of large carbon anions with N atoms, rather than from the radiative attachment of an electron to CN, as is the case for large molecular anions. The unexpectedly high abundance derived for CN − , 0.25% relative to CN, indicates that its detection in other astronomical sources is likely. A parallel search for the small anion C 2 H − remains inconclusive, despite the previous tentative identification of the J = 1−0 rotational transition. The abundance of C 2 H − in IRC +10216 is found to be vanishingly small, <0.0014% relative to C 2 H.

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Detection of C ₈ H ^- and Comparison with C ₈ H toward IRC +10 216

Cited by 171 publications

References 15 publications

The UMIST database for astrochemistry 2012

The UMIST database for astrochemistry 2012

Heavy ion formation in Titan's ionosphere: Magnetospheric introduction of free oxygen and a source of Titan's aerosols?

Astronomical identification of CN^-, the smallest observed molecular anion

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Detection of C 8 H - and Comparison with C 8 H toward IRC +10 216

Cited by 171 publications

References 15 publications

The UMIST database for astrochemistry 2012

The UMIST database for astrochemistry 2012

Heavy ion formation in Titan's ionosphere: Magnetospheric introduction of free oxygen and a source of Titan's aerosols?

Astronomical identification of CN-, the smallest observed molecular anion

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Product

Resources

About

Detection of C ₈ H ^- and Comparison with C ₈ H toward IRC +10 216

Astronomical identification of CN^-, the smallest observed molecular anion