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Title:
Tests of shock chemistry in IC 443G
Authors:
Turner, B. E.; Chan, Kin-Wing; Green, S.; Lubowich, D. A.
Affiliation:
AA(National Radio Astronomy Observatory, Charlottesville, VA), AB(Maryland Univ., College Park), AC(NASA, Goddard Inst. for Space Studies, New York), AD(Hofstra Univ., Hempstead; American Inst. of Physics, Woodbury, NY)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 1, p. 114-133. (ApJ Homepage)
Publication Date:
11/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
INTERSTELLAR CHEMISTRY, INTERSTELLAR MATTER, SHOCK WAVES, SUPERNOVA REMNANTS, ABUNDANCE, ASTRONOMICAL MODELS, CARBON MONOXIDE, FORMALDEHYDE, HYDROCYANIC ACID, SPECTRAL LINE WIDTH
DOI:
10.1086/171908
Bibliographic Code:
1992ApJ...399..114T

Abstract

Eight molecular species, in the hot dense clump IC 443G, believed to be impacted by the shock wave from the SNR IC 443, are investigated. The clump consists of two distinct regions, one relatively cool, and one hotter and denser. Region 1 contains CO, HCO(+), HCN, and CN, whose abundances may be explained either by ion-molecule chemistry, or by a D shock of 60-90 km/s, passing through a clump of about 100,000/cu cm. Region 2 gives rise to SiO, CS, SO, and H2CO, and requires an ND shock of 5-15 km/s passing through a region of about 1,000,000/cu cm. Observed fractional abundances fit ND shock models if L is about 6.6 x 10 exp 15 cm. In general, observed line widths vary inversely with derived excitation density, while centroid velocities of all species are essentially identical.

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