Detection of HCO(+) J = 9 - 8 line emission toward Orion IRc2 - Molecular ions in hot dense gas

Details Detection of HCO(+) J = 9 - 8 line emission toward Orion IRc2 - Molecular ions in hot dense gas Detection of HCO(+) J = 9 - 8 line emission toward Orion IRc2 - Molecular ions in hot dense gas

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..240j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Jan. 20, 1992, p. 240-243. Research supported by David and Lucile Pack

Other

6

Emission Spectra, Formyl Ions, High Temperature Gases, Line Spectra, Molecular Ions, Orion Nebula, Chemical Equilibrium, Gas Density, Line Of Sight

Scientific paper

The HCO(+) J = 9 - 8 802.458 GHz transition toward IRc2 in Orion was detected. The line width implies that the emission originates in the low-velocity flow/doughnut most likely 10 arcsec or less from IRc2. If the line is optically thin, the density in the line-forming region is 10 exp 7/cu cm or higher. If the HCO(+) line arises in the same about 10 x 20 arcsec source as other lines with similar width, the total column density of HCO(+) is 3 x 10 exp 14/sq cm or higher, implying a line-of-sight averaged abundance 2 x 10 exp -9 or more. This abundance is significantly greater than would be expected in a high-density region. Equilibrium chemical models predict an abundance more than an order of magnitude lower than observed. Enhancement of HCO(+) by local UV and X-ray fields is probably also insufficient to explain the observations. Time-dependent enhancement of the HCO(+) abundance in shocks may offer an explanation.

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