Origin of Gaseous CO2 in Low-Mass Star-Forming Regions

Details Origin of Gaseous CO2 in Low-Mass Star-Forming Regions Origin of Gaseous CO2 in Low-Mass Star-Forming Regions

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008atnf.prop.1425s&link_type=abstract

ATNF proposal C1832, Semester: April, 2008

Physics

Galactic, Atca

Scientific paper

Recently we have detected the rotational emission of HCO2+ toward a southern low-mass protostar, IRAS15398-3359 with Mopra. This is the second detection of HCO2+ after our detection in L1527, except for the Galactic Center clouds. The principal aim of this proposal is to understand the formation process of the gaseous CO2 through the high spatial resolution observation of the HCO2+ emission (3 mm) in IRAS15398-3359. According to our result in L1527, gaseous CO2 does not originate from direct evaporation of solid CO2, but would come from CH4 evaporated from grain mantles through various reactions in a lukewarm region around the protostar. Since the HCO2+ emission is stronger in IRAS15398-3359 than in L1527, the above scenario is best tested in IRAS15398-3359 with ATCA. With this observation, a new and concrete picture on CO2 production in the gas phase will be established, which would be very useful to study a link between molecular cloud chemistry and planetary chemistry.

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