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Pathways to oxygen-bearing molecules in the interstellar medium and in planetary atmospheres: Cyclopropenone (c-C_3H_2O) and propynal (HCCCHO)

Zhou, Li and Kaiser, Ralf I. and Gao, Li Gyun and Chang, Agnes H. H. and Liang, Mao-Chang and Yung, Yuk L. (2008) Pathways to oxygen-bearing molecules in the interstellar medium and in planetary atmospheres: Cyclopropenone (c-C_3H_2O) and propynal (HCCCHO). Astrophysical Journal, 686 (2). pp. 1493-1502. ISSN 0004-637X. doi:10.1086/591072. https://resolver.caltech.edu/CaltechAUTHORS:ZHOapj08

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Abstract

We investigated the formation of two C_3H_2O isomers, i.e., cyclopropenone (c-C_3H_2O) and propynal (HCCCHO), in binary ice mixtures of carbon monoxide (CO) and acetylene (C_2H_2) at 10 K in an ultrahigh vacuum machine on high-energy electron irradiation. The chemical evolution of the ice samples was followed online and in situ via a Fourier transform infrared spectrometer and a quadrupole mass spectrometer. The temporal profiles of the cyclopropenone and propynal isomers suggest (pseudo-) first-order kinetics. The cyclic structure (c-C_3H_2O) is formed via an addition of triplet carbon monoxide to ground-state acetylene (or vice versa); propynal (HCCCHO) can be synthesized from a carbon monoxide-acetylene complex via a [HCO center dot center dot center dot CCH] radical pair inside the matrix cage. These laboratory studies showed for the first time that both C_3H_2O isomers can be formed in low-temperature ices via nonequilibrium chemistry initiated by energetic electrons as formed in the track of Galactic cosmic ray particles penetrating interstellar icy grains in cold molecular clouds. Our results can explain the hitherto unresolved gas phase abundances of cyclopropenone in star-forming regions via sublimation of c-C_3H_2O as formed on icy grains in the cold molecular cloud stage. Implications for the heterogeneous oxygen chemistry of Titan and icy terrestrial planets and satellites suggest that the production of oxygen-bearing molecules such as C_3H_2O may dominate on aerosol particles compared to pure gas phase chemistry.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/591072DOIUNSPECIFIED
http://www.iop.org/EJ/abstract/0004-637X/686/2/1493/PublisherUNSPECIFIED
ORCID:
AuthorORCID
Liang, Mao-Chang0000-0002-5294-9344
Yung, Yuk L.0000-0002-4263-2562
Contact Email Address:ralfk@hawaii.edu
Additional Information:© 2008 The American Astronomical Society. Received 2008 February 20; accepted 2008 June 10. The experimental work was supported by the Chemistry division of the US National Science Foundation (NSF-CRC CHE- 0627854). L. G. G. and A. H. H. C. wish to thank the National Center for High Performance Computer of Taiwan for the support of computer resources. M. C. L. was supported by an NSC grant to Academia Sinica and by grant NSC 97-2628-M-001- 001. Y. L. Y. was supported by NASA grant NNX07AI63G to the California Institute of Technology.
Funders:
Funding AgencyGrant Number
NSFNSF-CRC CHE-0627854
National Science CenterNSC 97-2628-M-001001
NASANNX07AI63G
Subject Keywords:astrobiology; astrochemistry; ISM: molecules; planets and satellites: individual (Titan)
Issue or Number:2
DOI:10.1086/591072
Record Number:CaltechAUTHORS:ZHOapj08
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:ZHOapj08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13381
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Jun 2009 14:53
Last Modified:08 Nov 2021 22:37

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