Temperature Dependence of Two Key Interstellar Reactions of H3+: O(3P) + H3+ and CO + H3+

Klippenstein, Stephen J.; Georgievskii, Yuri; McCall, Benjamin J.

doi:10.1021/jp908500h

Cited by 48 publications

(58 citation statements)

References 63 publications

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“…Bruhns et al (2010), Brunetti & Liuti (1975) Harada & Herbst (2008), Harrison et al (1986), Hasegawa & Herbst (1993), Hawley et al (1990), Hemsworth et al (1974), Herbst (1983), Herbst et al (1984), Herbst & Leung (1986), Herbst et al (1989a), Herbst & Leung (1989), Herbst et al (1989b), Herbst et al (1989c), Herbst & Leung (1990), Herbst et al (2000), Herbst & Osamura (2008), Herbst et al (2010), Herrero et al (2010), Hoobler & Leone (1997), Huo et al (2011), Iglesias (1977, Inomata & Washida (1999), Johnson et al (2000), , Kalhori et al (2002), Kamińska et al (2008), Kern et al (1988), Wakelam et al (2012), Klippenstein et al (2010), Kuan et al (1999) Millar et al (1985), Millar et al (1986), Millar et al (1987), Millar et al (1988), Millar & Herbst (1990), Millar (1991, Millar et al (1991), Millar et al (1997b), Millar et al (2000), Millar et al (2007), Mi...…”

Section: Appendix A: Rate12 Referencesmentioning

confidence: 99%

The UMIST database for astrochemistry 2012

McElroy

Walsh

Markwick

et al. 2013

A&A

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: Appendix A: Rate12 Referencesmentioning

confidence: 99%

The UMIST database for astrochemistry 2012

McElroy

Walsh

Markwick

et al. 2013

A&A

909

880

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“…H 2 O is destroyed by ultraviolet photons and by reactions with C þ , H þ 3 , and other ions such as HCO þ . All key reactions in this network have been measured or calculated at low temperatures (e.g., Klippenstein et al 2010). The steady-state H 2 O abundance resulting from pure gas-phase chemistry is typically a few times 10 À7 with respect to H 2 at low T and scales with the cosmic-ray ionization rate ζ (e.g., Woodall et al 2007).…”

Section: Chemistrymentioning

confidence: 99%

Water in Star-forming Regions with theHerschel Space Observatory(WISH). I. Overview of Key Program and First Results

Dishoeck¹,

Kristensen²,

Benz³

et al. 2011

Publications of the Astronomical Society of the Pacific

212

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ABSTRACT. Water In Star-forming regions with Herschel (WISH) is a key program on the Herschel Space Observatory designed to probe the physical and chemical structures of young stellar objects using water and related molecules and to follow the water abundance from collapsing clouds to planet-forming disks. About 80 sources are targeted, covering a wide range of luminosities-from low (<1 L ⊙ ) to high (>10 5 L ⊙ )-and a wide range of evolutionary stages-from cold prestellar cores to warm protostellar envelopes and outflows to disks around young stars. Both the HIFI and PACS instruments are used to observe a variety of lines of H 2 O, H 2 18 O and chemically related species at the source position and in small maps around the protostars and selected outflow positions. In addition, high-frequency lines of CO, 13 CO, and C 18 O are obtained with Herschel and are complemented by ground-based observations of dust continuum, HDO, CO and its isotopologs, and other molecules to ensure 16 PACIFIC, 123:138-170, 2011 February © 2011. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. a self-consistent data set for analysis. An overview of the scientific motivation and observational strategy of the program is given, together with the modeling approach and analysis tools that have been developed. Initial science results are presented. These include a lack of water in cold gas at abundances that are lower than most predictions, strong water emission from shocks in protostellar environments, the importance of UV radiation in heating the gas along outflow walls across the full range of luminosities, and surprisingly widespread detection of the chemically related hydrides OH þ and H 2 O þ in outflows and foreground gas. Quantitative estimates of the energy budget indicate that H 2 O is generally not the dominant coolant in the warm dense gas associated with protostars. Very deep limits on the cold gaseous water reservoir in the outer regions of protoplanetary disks are obtained that have profound implications for our understanding of grain growth and mixing in disks.

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“…and Klippenstein et al (2010) have reported total rate coefficients of 1:42 Â 10 À9 cm 3 s À1 and 2:2 Â 10 À9 cm 3 s À1 , respectively. The yields are given as 0.735 and $0.62, respectively, for channel (R49a), and 0.264 and $0.38, respectively, for channel (R49b).…”

mentioning

confidence: 99%

“…The yields are given as 0.735 and $0.62, respectively, for channel (R49a), and 0.264 and $0.38, respectively, for channel (R49b). Although we have adopted the calculated values ofKlippenstein et al (2010), the difference between the results of the two studies provides some insight into the magnitudes of the uncertainties in computed rate coefficients.The rate coefficients for the proton transfer reactions of ArH + with O:…”

mentioning

confidence: 99%